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Author name code: liu-wei
ADS astronomy entries on 2022-09-14
author:"Liu, Wei"

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Title: Research on the On-orbit Background of the Hard X-Ray Imager
    Onboard ASO-S
Authors: Liu, Wei; Chen, Deng-Yi; Jiang, Xian-Kai; Wu, Jian; Zhang,
   Zhe; Hu, Yi-Ming; Su, Yang; Chen, Wei; Ma, Tao
2022RAA....22i5011L    Altcode:
  The space environment background of various particle fluxes of
  the Hard X-ray Imager (HXI), one of the payloads of the Advanced
  Space-based Solar Observatory (ASO-S) spacecraft, is investigated
  and presented. Different approaches are used to obtain the input
  information on various space environment particles (protons, alpha
  particles, electrons, positrons, neutrons, and photons). Some special
  regions (SAA and radiation belt) are also taken into account. The
  findings indicate that electrons are the primary background source
  in the radiation belt. Due to the large background flux generated by
  electrons, HXI cannot effectively observe solar flares in the radiation
  belt. Outside the radiation belt, primary protons and albedo photons
  are the main sources of background at low and high magnetic latitudes
  respectively. The statistical analysis of the flare and background
  spectra shows that the errors of the flare energy spectrum observation
  are mainly concentrated in the high energy band, and the detector still
  has a certain spectrum observation capability for flares of C-class and
  below in the low energy band of the non-radiation belt. The imaging
  observation of flares of C-class and below is significantly affected
  by the accuracy of background subtraction. The energy band with the
  best signal-to-noise ratio is from 10 to 50 keV, which can be used to
  monitor the formation and class of flares.

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Title: Directly tracing cool filamentary accretion over >100 kpc
    into the interstellar medium of a quasar host at z=1
Authors: Johnson, Sean D.; Schaye, Joop; Walth, Gregory L.; Li,
   Jennifer I-Hsiu; Rudie, Gwen C.; Chen, Hsiao-Wen; Chen, Mandy C.;
   Epinat, Benoît; Gaspari, Massimo; Cantalupo, Sebastiano; Kollatschny,
   Wolfram; Zhuoqi; Liu; Muzahid, Sowgat
2022arXiv220904245J    Altcode:
  We report the discovery of giant (50-100 kpc) [O II] emitting nebulae
  with the Multi-Unit Spectroscopic Explorer (MUSE) in the field of TXS
  0206-048, a luminous quasar at z=1.13. An archival, down-the-barrel UV
  spectrum of the quasar shows absorption at velocities coincident with
  those of the extended nebulae, enabling new insights into inflows and
  outflows around the quasar host. One nebula exhibits a filamentary
  morphology extending over 120 kpc from the halo toward the quasar
  and intersecting with another nebula surrounding the quasar host
  with a radius of 50 kpc. The filamentary nebula has line-of-sight
  velocities >300 km/s from nearby galaxies but matches that of the
  nebula surrounding the quasar host where they intersect, consistent
  with filamentary accretion of cool inter- or circum-galactic medium
  or cooling hot halo gas. The kinematics of the nebulae surrounding
  the quasar host are unusual and complex, with one redshifted
  and one blue-shifted spiral-like structure. The nebular emission
  velocities at 5-10 kpc from the quasar match those of inflowing
  absorbing gas observed in a UV spectrum of the quasar. Together,
  the extended nebulae and associated redshifted absorption represent a
  compelling case of cool, filamentary gas accretion from halo scales
  into the extended interstellar medium and toward the nucleus of a
  massive quasar host galaxy at intermediate redshift. The inflow rate
  implied by the combination of emission and absorption constraints
  is orders-of-magnitude below levels required to sustain the quasar's
  radiative luminosity, indicating highly anisotropic or highly variable
  accretion.

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Title: Galactic cosmic ray propagation: sub-PeV diffuse gamma-ray
    and neutrino emission
Authors: Qiao, Bing-Qiang; Liu, Wei; Zhao, Meng-Jie; Bi, Xiao-Jun;
   Guo, Yi-Qing
2022FrPhy..1744501Q    Altcode: 2021arXiv210403729Q
  The Tibet ASγ experiment just reported their measurement of sub-PeV
  diffuse gamma-ray emission from the Galactic disk, with the highest
  energy up to 957 TeV. These diffuse gamma rays are most likely the
  hadronic origin by cosmic ray (CR) interaction with interstellar
  gas in the galaxy. This measurement provides direct evidence to the
  hypothesis that the Galactic Cosmic Rays (GCRs) can be accelerated
  beyond PeV energies. In this work, we try to explain the sub-PeV
  diffuse gamma-ray spectrum with different CR propagation models. We
  find that there is a tension between the sub-PeV diffuse gamma-ray
  and the local CR spectrum. To describe the sub-PeV diffuse gamma-ray
  flux, it generally requires larger local CR flux than measurement
  in the knee region. We further calculate the PeV neutrino flux from
  the CR propagation model. Even all of these sub-PeV diffuse gamma
  rays originate from the propagation, the Galactic Neutrinos (GNs)
  only account for less than ∼ 15% of observed flux, most of which
  are still from extragalactic sources.

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Title: Construction and Validation of a Geometry-based Mathematical
    Model for Hard X-ray Imager
Authors: Jiang, Xian-Kai; Wu, Jian; Chen, Deng-Yi; Hu, Yi-Ming; Wang,
   Hao-Xiang; Liu, Wei; Zhang, Zhe
2022arXiv220705390J    Altcode:
  Quantitative and analytical analysis of modulation process of the
  collimator is a great challenge, and is also of great value to the
  design and development of Fourier transform imaging telescopes. The
  Hard X-ray Imager (HXI), as one of the three payloads onboard
  the Advanced Space-based Solar Observatory(ASO-S) mission, adopts
  modulating Fourier-Transformation imaging technique and will be used
  to explore mechanism of energy release and transmission in solar flare
  activities. In this paper, a mathematical model is developed to analyze
  the modulation function under a simplified condition first. Then its
  behavior under six degrees of freedom is calculated after adding the
  rotation matrix and translation change to the model. In addition,
  unparalleled light and extended sources also are considered so that
  our model can be used to analyze the X-ray beam experiment. Next,
  applied to the practical HXI conditions, the model has been
  confirmed not only by Geant4 simulations but also by some verification
  experiments. Furthermore, how this model will help to improve the image
  reconstruction process after the launch of ASO-S is also presented.

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Title: Multiwavelength observations of Swift J0243.6+6124 from 2017
    to 2022
Authors: Liu, Wei; Yan, Jingzhi; Reig, Pablo; Wang, Xiaofeng; Xiao,
   Guangcheng; Lin, Han; Zhang, Xinhan; Sai, Hanna; Chen, Zhihao; Yan,
   Shengyu; Liu, Qingzhong
2022arXiv220800151L    Altcode:
  We have obtained optical spectroscopy and photometry data during
  four years after the event. The long-term photometric light-curve and
  the equivalent widths of the Halpha and He I 6678 lines were used to
  monitor the state of the Be star disk. The Halpha line profiles show
  evidence for V/R variability that was accounted for by fitting the
  Halpha spectral line profile with two Gaussian functions. We divided our
  data into three phases according to the intensity of the X-ray, optical,
  and infrared emission. Phase I covers the rise and decay of the giant
  X-ray outburst that took place in October to November 2017. We interpret
  phase II as the dissipation of the Be star equatorial disk and phase III
  as its recovery. The timescale of a complete formation and dissipation
  process is about 1250 days. The epoch when the dissipation process
  stopped and the reformation period began is estimated to be around MJD
  58530. We find a delay of about 100 to 200 days between the minimum
  of the optical or infrared intensity and the strength of the Halpha
  line after the X-ray outburst, which may indicate that the dissipation
  of the disk begins from the inner parts. The motion of the density
  perturbation inside the disk is prograde, with a V/R quasi-period of
  about four years. The source shows a positive correlation in the (B-V)
  color index versus V-band magnitude diagram, which implies that the
  system is seen at a small or moderate inclination angle.

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Title: Flux Variations of Cosmic Ray Air Showers Detected by
    LHAASO-KM2A During a Thunderstorm on 10 June 2021
Authors: LHAASO Collaboration; Aharonian, F.; An, Q.; Axikegu; Bai,
   L. X.; Bai, Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai,
   J. T.; Cao, Zhe; Cao, Zhen; Chang, J.; Chang, J. F.; Chen, E. S.; Chen,
   Liang; Chen, Liang; Chen, Long; Chen, M. J.; Chen, M. L.; Chen, S. H.;
   Chen, S. Z.; Chen, T. L.; Chen, X. J.; Chen, Y.; Cheng, H. L.; Cheng,
   N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Dai, B. Z.; Dai,
   H. L.; Dai, Z. G.; Danzengluobu; della Volpe, D.; Duan, K. K.; Fan,
   J. H.; Fan, Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng,
   L.; Feng, S. H.; Feng, X. T.; Feng, Y. L.; Gao, B.; Gao, C. D.; Gao,
   L. Q.; Gao, Q.; Gao, W.; Gao, W. K.; Ge, M. M.; Geng, L. S.; Gong,
   G. H.; Gou, Q. B.; Gu, M. H.; Gu, F. L.; Guo, J. G.; Guo, X. L.; Guo,
   Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, S. L.; He,
   X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.; Hu, H. B.;
   Hu, Q.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, W. H.;
   Huang, X. T.; Huang, X. Y.; Huang, Y.; Huang, Z. C.; Ji, X. L.; Jia,
   H. Y.; Jia, K.; Jiang, K.; Jiang, Z. J.; Jin, M.; Kang, M. M.; Ke,
   T.; Kuleshov, D.; Li, B. B.; Li, Cheng; Li, Cong; Li, F.; Li, H. B.;
   Li, H. C.; Li, H. Y.; Li, J.; Li, Jian; Li, Jie; Li, K.; Li, W. L.;
   Li, X. R.; Li, Xin; Li, Xin; Li, Y. Z.; Li, Zhe; Li, Zhuo; Liang,
   E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.; Liu, H.;
   Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.; Liu, M. Y.;
   Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.; Long, W. J.;
   Lu, R.; Luo, Q.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao,
   J. R.; Masood, A.; Min, Z.; Mitthumsiri, W.; Nan, Y. C.; Ou, Z. W.;
   Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Qi, Y. Q.;
   Qiao, B. Q.; Qin, J. J.; Ruffolo, D.; Sáiz, A.; Shao, C. Y.; Shao,
   L.; Shchegolev, O.; Sheng, X. D.; Shi, J. Y.; Song, H. C.; Stenkin,
   Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.; Sun, X. N.; Sun, Z. B.;
   Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang, B. D.; Wang, C.; Wang,
   H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang, L. P.; Wang, L. Y.;
   Wang, R.; Wang, R. N.; Wang, W.; Wang, X. G.; Wang, X. Y.; Wang, Y.;
   Wang, Y. D.; Wang, Y. J.; Wang, Y. P.; Wang, Z. H. Wang. Z. X.; Wang,
   Zhen; Wang, Zheng; Wei, D. M.; Wei, J. J.; Wei, Y. J.; Wen, T.; Wu,
   C. Y.; Wu, H. R.; Wu, S.; Wu, X. F.; W, Y. S.; Xi, S. Q.; Xia, J.;
   Xia, J. J.; Xiang, G. M.; Xiao, D. X.; Xiao, G.; Xin, G. G.; Xin,
   Y. L.; Xing, Y.; Xiong, Z.; Xu, D. L.; Xu, R. X.; Xue, L.; Yan, D. H.;
   Yan, J. Z.; Yang, C. W.; Yang, F. F.; Yang, H. W.; Yang, J. Y.; Yang,
   L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.;
   Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.;
   Yuan, Q.; Yue, H.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.;
   Zha, M.; Zhai, X. X.; Zhang, B. B.; Zhang, F.; Zhang, H. M.; Zhang,
   H. Y.; Zhang, J. L.; Zhang, L. X.; Zhang, Li; Zhang, Lu; Zhang, P. F.;
   Zhang, P. P.; Zhang, R.; Zhang, S. B.; Zhang, S. R.; Zhang, S. S.;
   Zhang, X.; Zhang, X. P.; Zhang, Y. F.; Zhang, Y. L.; Zhang, Yi; Zhang,
   Yong; Zhao, B.; Zhao, J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng,
   F.; Zheng, Y.; Zhou, B.; Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.;
   Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.
2022arXiv220712601L    Altcode:
  The Large High Altitude Air Shower Observatory (LHAASO) has three
  sub-arrays, KM2A, WCDA and WFCTA. The flux variations of cosmic ray air
  showers were studied by analyzing the KM2A data during the thunderstorm
  on 10 June 2021. The number of shower events that meet the trigger
  conditions increases significantly in atmospheric electric fields,
  with maximum fractional increase of 20%. The variations of trigger
  rates (increases or decreases) are found to be strongly dependent on
  the primary zenith angle. The flux of secondary particles increases
  significantly, following a similar trend with that of the shower
  events. To better understand the observed behavior, Monte Carlo
  simulations are performed with CORSIKA and G4KM2A (a code based on
  GEANT4). We find that the experimental data (in saturated negative
  fields) are in good agreement with simulations, assuming the presence
  of a uniform upward electric field of 700 V/cm with a thickness
  of 1500 m in the atmosphere above the observation level. Due to
  the acceleration/deceleration and deflection by the atmospheric
  electric field, the number of secondary particles with energy above
  the detector threshold is modified, resulting in the changes in shower
  detection rate.

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Title: Probing massive neutrinos with the Minkowski functionals of
    large-scale structure
Authors: Liu, Wei; Jiang, Aoxiang; Fang, Wenjuan
2022JCAP...07..045L    Altcode: 2022arXiv220402945L
  Massive neutrinos suppress the growth of structure under their
  free-streaming scales. The effect is most prominent on small scales
  where the widely-used two-point statistics can no longer capture
  the full information. In this work, we study the signatures massive
  neutrinos leave on large-scale structure (LSS) as revealed by its
  morphological properties, which are fully described by 4 Minkowski
  functionals (MFs), and quantify the constraints on the summed
  neutrino mass M<SUB>ν</SUB> from the MFs, by using publicly available
  N-body simulations. We find the MFs provide important complementary
  information, and give tighter constraints on M<SUB>ν</SUB> than the
  power spectrum. Specifically, depending on whether massive neutrinos are
  included in the density field (the 'm' field) or not (the 'cb' field),
  we find the constraint on M<SUB>ν</SUB> from the MFs with a smoothing
  scale of R<SUB>G</SUB> = 5h <SUP>-1</SUP>Mpc is 48 or 4 times better
  than that from the power spectrum. When the MFs are combined with the
  power spectrum, they can improve the constraint on M<SUB>ν</SUB>
  from the latter by a factor of 63 for the 'm' field and 5 for the
  'cb' field. Notably, when the 'm' field is used, the constraint on
  M<SUB>ν</SUB> from the MFs can reach 0.0177eV with a volume of 1(
  <SUP>-1</SUP>Gpc)<SUP>3</SUP>, while the combination of the MFs and
  power spectrum can tighten this constraint to be 0.0133eV, a 4.5σ
  significance on detecting the minimum sum of the neutrino masses. For
  the 'm' field, we also find the σ <SUB>8</SUB> and M<SUB>ν</SUB>
  degeneracy is broken with the MFs, leading to stronger constraints
  on all 6 cosmological parameters considered in this work than the
  power spectrum.

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Title: First Estimates of Hydrothermal Helium Fluxes in Continental
Collision Settings: Insights From the Southeast Tibetan Plateau Margin
Authors: Zhang, Maoliang; Liu, Wei; Guan, Lufeng; Takahata, Naoto;
   Sano, Yuji; Li, Ying; Zhou, Xiaocheng; Chen, Zhi; Cao, Chunhui; Zhang,
   Lihong; Lang, Yun-Chao; Liu, Cong-Qiang; Xu, Sheng
2022GeoRL..4998228Z    Altcode:
  Continental regions are essential for the outgassing of deeply-sourced
  helium in response to volcanic and tectonic processes. However,
  the helium fluxes remain largely unknown for continental collision
  settings such as the Tibetan Plateau. Here, we focus on hydrothermal
  helium degassing from the Simao block, Southeast Tibetan Plateau
  margin, and report flux estimates of (0.03 - 32) × 10<SUP>5</SUP>
  atoms m<SUP>−2</SUP> s<SUP>−1</SUP> for <SUP>3</SUP>He and (3.2
  - 32) × 10<SUP>10</SUP> atoms m<SUP>−2</SUP> s<SUP>−1</SUP>
  for <SUP>4</SUP>He, with mantle fractions of helium fluxes
  up to 2−3 orders of magnitude greater than those of stable
  continents. Geologically recent magma recharge beneath Quaternary
  volcanoes is proposed to account for the high mantle helium fluxes and
  <SUP>3</SUP>He/<SUP>4</SUP>He up to 7.24 Ra. Active tectonics driven
  by the India-Asia continental collision possibly maintained efficient
  release of crustal helium over geological timescales. These findings
  present the first flux estimates for hydrothermal helium degassing
  controlled by volcanic and tectonic processes in continental collision
  settings.

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Title: Evolution of Fractal Pore Structure in Sedimentary Rocks
Authors: Zhou, Nengwu; Wang, Min; Lu, Shuangfang; Dodd, Thomas J. H.;
   Liu, Wei; Guan, Ying
2022E&SS....902167Z    Altcode:
  Geological processes alter pore spaces over time, and their analysis
  can shed light on the dynamic fractal structure and fluid flow of rocks
  over time. This study presents experimental evidence to illustrate
  that the pore fractal structure evolves with sedimentation, carbonate
  cementation, clay growth, and dissolution. It examines, describes and
  characterizes a suite of core samples from the Gaotaizi oil layer of
  the second and third members of the Qingshankou Formation, Songliao
  Basin, China. The effects of mechanical compaction and other diagenesis
  effects on fractal pore structure on sedimentary rocks are discussed. A
  schematic diagram is proposed that describes the impacts of these
  diagenetic processes on fractal pore structure at the microscopic
  scale in sedimentary rocks. This work links the state of diagenetic
  alteration and fractal pore structure, which can guide practical
  applications such as predicting the permeability of sedimentary rocks.

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Title: Measurement of the Gamma-Ray Energy Spectrum beyond 100 TeV
    from the HESS J1843-033 Region
Authors: Amenomori, M.; Asano, S.; Bao, Y. W.; Bi, X. J.; Chen, D.;
   Chen, T. L.; Chen, W. Y.; Chen, Xu; Chen, Y.; Cirennima; Cui, S. W.;
   Danzengluobu; Ding, L. K.; Fang, J. H.; Fang, K.; Feng, C. F.; Feng,
   Zhaoyang; Feng, Z. Y.; Gao, Qi; Gomi, A.; Gou, Q. B.; Guo, Y. Q.; Guo,
   Y. Y.; He, H. H.; He, Z. T.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu,
   H. B.; Hu, K. Y.; Huang, J.; Jia, H. Y.; Jiang, L.; Jiang, P.; Jin,
   H. B.; Kasahara, K.; Katayose, Y.; Kato, C.; Kato, S.; Kawashima,
   T.; Kawata, K.; Kozai, M.; Kurashige, D.; Labaciren; Le, G. M.; Li,
   A. F.; Li, H. J.; Li, W. J.; Li, Y.; Lin, Y. H.; Liu, B.; Liu, C.;
   Liu, J. S.; Liu, L. Y.; Liu, M. Y.; Liu, W.; Liu, X. L.; Lou, Y. -Q.;
   Lu, H.; Meng, X. R.; Meng, Y.; Munakata, K.; Nagaya, K.; Nakamura,
   Y.; Nakazawa, Y.; Nanjo, H.; Ning, C. C.; Nishizawa, M.; Ohnishi, M.;
   Okukawa, S.; Ozawa, S.; Qian, L.; Qian, X.; Qian, X. L.; Qu, X. B.;
   Saito, T.; Sakakibara, Y.; Sakata, M.; Sako, T.; Sako, T. K.; Shao,
   J.; Shibata, M.; Shiomi, A.; Sugimoto, H.; Takano, W.; Takita, M.; Tan,
   Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo, S.; Wang, H.; Wang,
   Y. P.; Wangdui; Wu, H. R.; Wu, Q.; Xu, J. L.; Xue, L.; Yang, Z.; Yao,
   Y. Q.; Yin, J.; Yokoe, Y.; Yu, N. P.; Yuan, A. F.; Zhai, L. M.; Zhang,
   C. P.; Zhang, H. M.; Zhang, J. L.; Zhang, X.; Zhang, X. Y.; Zhang,
   Y.; Zhang, Yi; Zhang, Ying; Zhao, S. P.; Zhaxisangzhu; Zhou, X. X.
2022ApJ...932..120A    Altcode:
  HESS J1843-033 is a very high energy gamma-ray source whose origin
  remains unidentified. This work presents, for the first time, the
  energy spectrum of gamma rays beyond 100 TeV from the HESS J1843-033
  region using the data recorded by the Tibet air shower array and its
  underground muon detector array. A gamma-ray source with an extension
  of 0.°34 ± 0.°12 is successfully detected above 25 TeV at (α,
  δ) = (281.°09 ± 0.°10, -3.°76 ± 0.°09) near HESS J1843-033
  with a statistical significance of 6.2σ, and the source is named
  TASG J1844-038. The position of TASG J1844-038 is consistent with
  those of HESS J1843-033, eHWC J1842-035, and LHAASO J1843-0338. The
  measured gamma-ray energy spectrum in 25 TeV &lt; E &lt; 130 TeV
  is described with ${dN}/{dE}=(9.70\pm 1.89)\times {10}^{-16}$
  (E/40 TeV)<SUP>-3.26±0.30</SUP> TeV<SUP>-1</SUP> cm<SUP>-2</SUP>
  s<SUP>-1</SUP>, and the spectral fit to the combined spectra of HESS
  J1843-033, LHAASO J1843-0338, and TASG J1844-038 implies the existence
  of a cutoff at 49.5 ± 9.0 TeV. Associations of TASG J1844-038 with
  SNR G28.6-0.1 and PSR J1844-0346 are also discussed in detail for the
  first time.

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Title: Ultraviolet Photooxidation of Smectite-Bound Fe(II) and
    Implications for the Origin of Martian Nontronites
Authors: Rivera Banuchi, V. B.; Liu, W.; Yee, N.; Legett, C.; Glotch,
   T. D.; Chemtob, S. M.
2022JGRE..12707150R    Altcode:
  Clay minerals detected with orbital and in situ instruments in ancient
  Martian terrains constrain Mars' climate and aqueous alteration
  history. Early in its history, Mars experienced an atmospheric redox
  change and iron-bearing clay minerals may preserve the effects of
  that transition. Ferrous smectites, the thermodynamically predicted
  product of chemical weathering of basalts under anoxic conditions,
  may have undergone oxidation by exposure to chemical oxidants in the
  atmosphere or regolith, or by direct photooxidation at the surface. To
  assess these potential oxidation pathways, ferrous trioctahedral
  smectites of varying initial iron content were synthesized and
  subjected to oxidation by ultraviolet (UV) irradiation. Experimental
  UV irradiation under an anoxic atmosphere equivalent to approximately
  7 years of flux on the Martian surface caused partial oxidation
  of smectite-bound Fe (Fe<SUP>3+</SUP>/ΣFe = 16-18%) and octahedral
  sheet contraction. Metal-OH vibrational bands in visible/near infrared
  (VNIR) reflectance spectra of oxidized smectites changed in band depth
  and asymmetry with higher iron content. X-ray diffraction patterns
  of UV irradiated samples indicate the formation of a mixed di- and
  trioctahedral smectite or a secondary nontronite phase, possibly on
  the surfaces of higher iron content smectites. These experiments
  suggest that UV irradiation is able to oxidize structurally
  bound iron in smectites without the presence of other chemical
  oxidants. Photooxidation may have influenced the mineralogy, both
  syndepositionally and postdepositionally, of Martian alteration
  assemblages formed near the surface and this process needs not be
  limited to one part of their formation history.

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Title: Study on the variation of orbital period, quasi-periodic
    oscillations and negative superhumps in V729 Sgr
Authors: Sun, Qi-Bin; Qian, Sheng-Bang; Dong, Ai-Jun; Zhi, Qi-Jun;
   Han, Zhong-Tao; Liu, Wei; Chang, Xin; Liu, Chang; Xiang, Hong-Bin;
   Peng, Xue-Bing; Zhang, Bin; Zhang, Xu-Dong; Fernández Lajús, E.
2022NewA...9301751S    Altcode:
  Based on K2 and our observations of V729 Sgr, the study of the variation
  of orbital period, quasi-periodic oscillations (QPOs) and negative
  superhumps are presented. Using all available mid-eclipse times during
  quiescence, we find that V729 Sgr has a cyclic variation of the orbital
  period, with periods and amplitudes of ∼ 9 . 64 years and ∼ 442 . 37
  s, respectively. Based on the interpret of light travel-time effect,
  the mass of third body is derived as M<SUB>3</SUB> sini<SUP>'</SUP> = 0
  . 24(± 0 . 016) M<SUB>⊙</SUB> . When the third body is coplanar with
  the central body system, the third body may be a low-mass star. Using
  the Weighted Wavelet Z-transform (WWZ) method, we find for the first
  time that V729 Sgr has QPOs with the period of ∼1030-3370 s. Using
  WWZ method, we find that V729 Sgr also has negative superhumps in
  the first quiescence, indicating that the negative superhumps may be
  permanent in the quiescence of V729 Sgr.

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Title: Statistical Study of the Optimal Local Sources for Cosmic
    Ray Nuclei and Electrons
Authors: Luo, Qing; Qiao, Bing-qiang; Liu, Wei; Cui, Shu-wang;
   Guo, Yi-qing
2022ApJ...930...82L    Altcode: 2021arXiv211000501L
  Local sources, such as the Geminga supernova remnant (SNR), may
  have played an important role in the anomaly of protons, electrons,
  and anisotropy in past works. In fact, there exist 12 SNRs around
  the solar system within 1 kpc. One question is whether other SNRs
  also possibly contribute to the spectra of nuclei and electrons,
  and explain the special structure of the anisotropy. In this work,
  under spatial-dependent propagation, we systematically study the
  contribution of all local SNRs, within 1 kpc around the solar system,
  to the spectra of nuclei and electrons, as well as the energy dependence
  of the anisotropy. As a result, only the Geminga, the Monogem, and the
  Vela SNRs have quantitative contributions to the nuclei and electron
  spectra, and the anisotropy. Here, the Geminga SNR is the sole optimal
  candidate and the Monogem SNR is controversial due to the tension of the
  anisotropy between the model calculation and the observations. The Vela
  SNR contributes to a new spectral structure beyond TeV energy, hinted
  by the HESS, the VERITAS, the DAMPE, and the CALET measurements. More
  interestingly, the electron anisotropy satisfies the Fermi-LAT limit
  below TeV energy, but rises greatly and reaches 10% at several TeV. This
  novel structure will shed new light on verifying our model. We hope
  that the new structure of the electron spectrum and anisotropy can be
  observed by the spaceborne DAMPE and HERD, and the ground-based HAWC
  and LHAASO experiments in the near future.

---------------------------------------------------------
Title: Analogue cosmological particle creation in an ultracold
    quantum fluid of light
Authors: Steinhauer, Jeff; Abuzarli, Murad; Aladjidi, Tangui;
   Bienaimé, Tom; Piekarski, Clara; Liu, Wei; Giacobino, Elisabeth;
   Bramati, Alberto; Glorieux, Quentin
2022NatCo..13.2890S    Altcode: 2021arXiv210208279S
  The rapid expansion of the early universe resulted in the spontaneous
  production of cosmological particles from vacuum fluctuations, some
  of which are observable today in the cosmic microwave background
  anisotropy. The analogue of cosmological particle creation in a quantum
  fluid was proposed, but the quantum, spontaneous effect due to vacuum
  fluctuations has not yet been observed. Here we report the spontaneous
  creation of analogue cosmological particles in the laboratory, using a
  quenched 3-dimensional quantum fluid of light. We observe acoustic peaks
  in the density power spectrum, in close quantitative agreement with the
  quantum-field theoretical prediction. We find that the long-wavelength
  particles provide a window to early times. This work introduces the
  quantum fluid of light, as cold as an atomic Bose-Einstein condensate.

---------------------------------------------------------
Title: Effects of peculiar velocities on the morphological properties
    of large-scale structure
Authors: Jiang, Aoxiang; Liu, Wei; Fang, Wenjuan; Zhao, Wen
2022PhRvD.105j3028J    Altcode: 2021arXiv210803851J
  It is known that the large-scale structure mapped by a galaxy
  redshift survey is subject to distortions by galaxies' peculiar
  velocities. Besides the signatures generated in common N -point
  statistics, such as the anisotropy in the galaxy two-point correlation
  function, the peculiar velocities also induce distinct features in
  large-scale structures morphological properties, which are fully
  described by four Minkowski functionals (MFs), i.e., the volume,
  surface area, integrated mean curvature, and Euler characteristic (or
  genus). In this work, by using large suite of N -body simulations, we
  present and analyze these important features in the MFs of large-scale
  structure on both (quasi)linear and nonlinear scales, with a focus on
  the latter. We also find the MFs can give competitive constraints on
  cosmological parameters compared to the power spectrum, probably due
  to the nonlinear information contained. For a galaxy number density
  similar to the DESI BGS galaxies, the constraint on σ<SUB>8</SUB> from
  the MFs with one smoothing scale can be better by ∼50 % than from
  the power spectrum. These findings are important for the cosmological
  applications of MFs of large-scale structure, and probably open up a
  new avenue for studying the peculiar velocity field itself.

---------------------------------------------------------
Title: Deciphering the Migration of the Intertropical Convergence
    Zone During the Last Deglaciation
Authors: Li, Shouwei; Liu, Wei
2022GeoRL..4998806L    Altcode:
  Proxy evidences suggest abrupt southward displacements of the
  intertropical convergence zone (ITCZ) during Heinrich Stadial 1 (HS1)
  and Younger Dryas (YD) against a long-term trend of northward ITCZ
  migration from Last Glacial Maximum to modern climate. Climate model
  simulations reveal that the abrupt ITCZ changes in HS1 and YD are mainly
  driven by ice-sheet-induced meltwater while the long-term ITCZ trend
  primarily results from orbital variations, rising atmospheric greenhouse
  gases and ice-sheet retreats during the last deglaciation. Atmospheric
  energetics analysis elucidates two important processes driven by
  meltwater—less net radiation entering the top-of-atmosphere (TOA)
  in the Northern Hemisphere than the Southern Hemisphere and a reduced
  global cross-equatorial oceanic heat transport from the compensation
  between Atlantic and Indo-Pacific heat transports—induce the southward
  ITCZ shift during HS1. Ice sheet extent changes also create a large
  interhemispheric TOA radiation asymmetry during HS1, which, however,
  is not via the surface albedo feedback.

---------------------------------------------------------
Title: Experimental study of chromium (III) coprecipitation with
    calcium carbonate
Authors: Fang, Ziyao; Liu, Wei; Yao, Tao; Zhou, Gentao; Wei, Shiqiang;
   Qin, Liping
2022GeCoA.322...94F    Altcode:
  Chromium (Cr) isotope compositions of marine carbonates have widely
  been used to trace the evolution of oxygen levels in the atmosphere
  and ocean during geological history. Recent studies have indicated
  that Cr found in natural carbonates is dominated by trivalent Cr,
  also known as Cr(III). However, the incorporation behavior of Cr(III)
  into carbonates remains undefined. Here, we conducted coprecipitation
  experiments for Cr(III) with calcium carbonate to constrain the
  behavior of Cr(III) in carbonate deposition environments. Extended
  X-ray absorption fine structure (EXAFS) results suggest that Cr(III)
  is incompatible with the calcite crystal lattice. There are likely
  to be several Cr species in the coprecipitation samples. Most Cr is
  adsorbed on the crystal surface of calcite or exists as amorphous Cr
  hydroxide [Cr(OH)<SUB>3</SUB>]. A small fraction of Cr can reside in
  the calcite crystal, but Cr<SUP>3+</SUP> cannot directly substitute
  for Ca<SUP>2+</SUP>. It may exist in interstitial voids in crystals
  or occupy the position of Ca<SUP>2+</SUP> in the form of divalent
  Cr hydroxide cation [Cr(OH)<SUP>2+</SUP>], leading to a distorted
  structure. Moreover, we find that Cr(III) can stimulate polymorph
  selection of vaterite [a metastable polymorph of calcium carbonate
  (CaCO<SUB>3</SUB>)] during CaCO<SUB>3</SUB> precipitation, likely due
  to the formation of Cr hydroxide on the surface of vaterite crystals,
  hindering its transformation to calcite. Because Cr(III) is incompatible
  with the carbonate crystal lattice, we suggest that most Cr in natural
  carbonates is adsorbed on the crystal surface and may be acquired at
  water-sediment interfaces after carbonate precipitation. Therefore,
  Cr isotope compositions of carbonates may easily be affected by
  post-depositional diagenetic processes, and Cr isotope variations in
  sedimentary carbonates should not exclusively correspond to changes
  in oxygen levels in the atmosphere and ocean. Paleoenvironment
  reconstruction based on Cr isotope compositions of carbonates should
  take post-depositional processes into consideration.

---------------------------------------------------------
Title: The Forward Physics Facility at the High-Luminosity LHC
Authors: Feng, Jonathan L.; Kling, Felix; Hall Reno, Mary; Rojo, Juan;
   Soldin, Dennis; Anchordoqui, Luis A.; Boyd, Jamie; Ismail, Ahmed;
   Harland-Lang, Lucian; Kelly, Kevin J.; Pandey, Vishvas; Trojanowski,
   Sebastian; Tsai, Yu-Dai; Alameddine, Jean-Marco; Araki, Takeshi;
   Ariga, Akitaka; Ariga, Tomoko; Asai, Kento; Bacchetta, Alessandro;
   Balazs, Kincso; Barr, Alan J.; Battistin, Michele; Bian, Jianming;
   Bertone, Caterina; Bai, Weidong; Bakhti, Pouya; Baha Balantekin,
   A.; Barman, Basabendu; Batell, Brian; Bauer, Martin; Bauer, Brian;
   Becker, Mathias; Berlin, Asher; Bertuzzo, Enrico; Bhattacharya, Atri;
   Bonvini, Marco; Boogert, Stewart T.; Boyarsky, Alexey; Bramante,
   Joseph; Brdar, Vedran; Carmona, Adrian; Casper, David W.; Celiberto,
   Francesco Giovanni; Cerutti, Francesco; Chachamis, Grigorios; Chauhan,
   Garv; Citron, Matthew; Copello, Emanuele; Corso, Jean-Pierre; Darmé,
   Luc; Tito D'Agnolo, Raffaele; Darvishi, Neda; Das, Arindam; De Lellis,
   Giovanni; De Roeck, Albert; de Vries, Jordy; Dembinski, Hans P.;
   Demidov, Sergey; deNiverville, Patrick; Denton, Peter B.; Deppisch,
   Frank F.; Bhupal Dev, P. S.; Di Crescenzo, Antonia; Dienes, Keith
   R.; Diwan, Milind V.; Dreiner, Herbi K.; Du, Yong; Dutta, Bhaskar;
   Duwentäster, Pit; Elie, Lucie; Ellis, Sebastian A. R.; Enberg, Rikard;
   Farzan, Yasaman; Fieg, Max; Foguel, Ana Luisa; Foldenauer, Patrick;
   Foroughi-Abari, Saeid; Fortin, Jean-François; Friedland, Alexander;
   Fuchs, Elina; Fucilla, Michael; Gallmeister, Kai; Garcia, Alfonso;
   García Canal, Carlos A.; Vittoria Garzelli, Maria; Gauld, Rhorry;
   Ghosh, Sumit; Ghoshal, Anish; Gibson, Stephen; Giuli, Francesco;
   Gonçalves, Victor P.; Gorbunov, Dmitry; Goswami, Srubabati; Grau,
   Silvia; Günther, Julian Y.; Guzzi, Marco; Haas, Andrew; Hakulinen,
   Timo; Harris, Steven P.; Harz, Julia; Helo Herrera, Juan Carlos;
   Hill, Christopher S.; Hirsch, Martin; Hobbs, Timothy J.; Höche,
   Stefan; Hryczuk, Andrzej; Huang, Fei; Inada, Tomohiro; Infantino,
   Angelo; Ismail, Ameen; Jacobsson, Richard; Jana, Sudip; Jeong, Yu
   Seon; Ježo, Tomas; Jho, Yongsoo; Jodłowski, Krzysztof; Kalashnikov,
   Dmitry; Kärkkäinen, Timo J.; Keppel, Cynthia; Kim, Jongkuk; Klasen,
   Michael; Klein, Spencer R.; Ko, Pyungwon; Köhler, Dominik; Komatsu,
   Masahiro; Kovařík, Karol; Kulkarni, Suchita; Kumar, Jason; Kumar,
   Karan; Kuo, Jui-Lin; Krauss, Frank; Kusina, Aleksander; Laletin,
   Maxim; Le Roux, Chiara; Lee, Seung J.; Lee, Hye-Sung; Lefebvre,
   Helena; Li, Jinmian; Li, Shuailong; Li, Yichen; Liu, Wei; Liu, Zhen;
   Lonjon, Mickael; Lyu, Kun-Feng; Maciula, Rafal; Mammen Abraham,
   Roshan; Masouminia, Mohammad R.; McFayden, Josh; Mikulenko, Oleksii;
   Mohammed, Mohammed M. A.; Mohan, Kirtimaan A.; Morfín, Jorge G.;
   Mosel, Ulrich; Mosny, Martin; Muzakka, Khoirul F.; Nadolsky, Pavel;
   Nakano, Toshiyuki; Nangia, Saurabh; Navascues Cornago, Angel; Nevay,
   Laurence J.; Ninin, Pierre; Nocera, Emanuele R.; Nomura, Takaaki;
   Nunes, Rui; Okada, Nobuchika; Olness, Fred; Osborne, John; Otono,
   Hidetoshi; Ovchynnikov, Maksym; Papa, Alessandro; Pei, Junle; Peon,
   Guillermo; Perez, Gilad; Pickering, Luke; Plätzer, Simon; Plestid,
   Ryan; Poddar, Tanmay Kumar; Rai, Mudit; Rajaee, Meshkat; Raut, Digesh;
   Reimitz, Peter; Resnati, Filippo; Rhode, Wolfgang; Richardson, Peter;
   Ritz, Adam; Rokujo, Hiroki; Roszkowski, Leszek; Ruhe, Tim; Ruiz,
   Richard; Sabate-Gilarte, Marta; Sandrock, Alexander; Sarcevic, Ina;
   Sarkar, Subir; Sato, Osamu; Scherb, Christiane; Schienbein, Ingo;
   Schulz, Holger; Schwaller, Pedro; Sciutto, Sergio J.; Sengupta,
   Dipan; Shchutska, Lesya; Shimomura, Takashi; Silvetti, Federico;
   Sinha, Kuver; Sjöstrand, Torbjörn; Sobczyk, Jan T.; Song, Huayang;
   Soriano, Jorge F.; Soreq, Yotam; Stasto, Anna; Stuart, David; Su,
   Shufang; Su, Wei; Szczurek, Antoni; Tabrizi, Zahra; Takubo, Yosuke;
   Taoso, Marco; Thomas, Brooks; Thonet, Pierre; Tuckler, Douglas; Sabio
   Vera, Agustin; Vincke, Heinz; Vishnudath, K. N.; Wang, Zeren Simon;
   Winkler, Martin W.; Wu, Wenjie; Xie, Keping; Xu, Xun-Jie; You, Tevong;
   Yu, Ji-Young; Yu, Jiang-Hao; Zapp, Korinna; Zhang, Yongchao; Zhang,
   Yue; Zhou, Guanghui; Zukanovich Funchal, Renata
2022arXiv220305090F    Altcode:
  High energy collisions at the High-Luminosity Large Hadron Collider
  (LHC) produce a large number of particles along the beam collision axis,
  outside of the acceptance of existing LHC experiments. The proposed
  Forward Physics Facility (FPF), to be located several hundred meters
  from the ATLAS interaction point and shielded by concrete and rock,
  will host a suite of experiments to probe Standard Model (SM) processes
  and search for physics beyond the Standard Model (BSM). In this report,
  we review the status of the civil engineering plans and the experiments
  to explore the diverse physics signals that can be uniquely probed
  in the forward region. FPF experiments will be sensitive to a broad
  range of BSM physics through searches for new particle scattering or
  decay signatures and deviations from SM expectations in high statistics
  analyses with TeV neutrinos in this low-background environment. High
  statistics neutrino detection will also provide valuable data for
  fundamental topics in perturbative and non-perturbative QCD and in
  weak interactions. Experiments at the FPF will enable synergies between
  forward particle production at the LHC and astroparticle physics to be
  exploited. We report here on these physics topics, on infrastructure,
  detector, and simulation studies, and on future directions to realize
  the FPF's physics potential.

---------------------------------------------------------
Title: Surface Solvation of Martian Salt Analogues at Low Relative
    Humidities
Authors: Kong, X. R.; Zhu, S. Y.; Shavorskiy, A.; Li, J.; Liu, W. Y.;
   Corral Arroyo, P.; Signorell, R.; Wang, S.; Pettersson, J. B. C.
2022LPICo2678.1878K    Altcode:
  The synchrotron-based approach is used to characterize the surface
  of martian analogues, as well as their responses to varying relative
  humidity.

---------------------------------------------------------
Title: Search for very high energy gamma-ray emission from GRB
    190829A with LHASSO-WCDA triggerless data
Authors: Yao, Y.; Liu, W.; Qiao, B.; Guo, Y.; Hu, H.; Yang, C.; Yao,
   Z.; Lhaaso Collaboration
2022icrc.confE.853Y    Altcode: 2022PoS...395E.853Y
  No abstract at ADS

---------------------------------------------------------
Title: Adaboost-DSNN: an adaptive boosting algorithm based on deep
    self normalized neural network for pulsar identification
Authors: Tariq, Irfan; Meng, Qiao; Yao, Shunyu; Liu, Wei; Zhou,
   Chenye; Ahmed, Adnan; Spanakis-Misirlis, Apostolos
2022MNRAS.511..683T    Altcode: 2022MNRAS.tmp..188T
  A modern pulsar survey generates a large number of pulsar
  candidates. Filtering these pulsar candidates in a large astronomical
  data set is an important step towards discovering new pulsars. In
  this paper, a novel adaptive boosting algorithm based on deep self
  normalized neural network (Adaboost-DSNN) is proposed to accurately
  classify pulsar and non-pulsar signals. To train the proposed
  method on a highly imbalanced data set, the Synthetic Minority
  Oversampling TEchnique (SMOTE) was initially employed for balancing
  the data set. Then, a deep ensemble network combined with a deep
  self-normalized neural network and adaptive boosting was developed to
  train and learn the processed pulsar data. The design of the proposed
  Adaboost-DSNN method significantly reduced the computational time
  when dealing with large astronomical data sets, while also improving
  the classification performance. The scaled exponential liner units
  activation function was used to normalize the data. Considering their
  neighbour information and the special dropout technique (α-dropout),
  Adaboost-DSNN displayed good pulsar classification performance, while
  preserving the data properties across subsequent layers. The proposed
  Adaboost-DSNN method was tested on the High Time Resolution Universe
  Survey data sets (HTRU-1 and HTRU-2). According to experimental results,
  Adaboost-DSNN outperform other state-of-the-art methods with respect
  to training time and F1-score. The training time of the Adaboost-DSNN
  model is 10x times faster compared to other models of this kind.

---------------------------------------------------------
Title: The Spectral Features of Potential Life Markers on Mars by
    Multiple Spectral Detection
Authors: Liu, W.; Wu, Z. C.; Chen, W. X.; Jin, G. B.; Li, Z.
2022LPICo2678.1387L    Altcode:
  The spectral features of potential life markers on Mars by multiple
  spectral detection.

---------------------------------------------------------
Title: Geminga SNR: Possible Candidate of the Local Cosmic-Ray Factory
Authors: Zhao, Bing; Liu, Wei; Yuan, Qiang; Hu, Hong-Bo; Bi, Xiao-Jun;
   Wu, Han-Rong; Zhou, Xun-Xiu; Guo, Yi-Qing
2022ApJ...926...41Z    Altcode: 2021arXiv210407321Z
  The precise measurements of energy spectra and anisotropy could
  help us uncover the local cosmic-ray accelerators. Our recent works
  have shown that spectral hardening above 200 GeV in the energy
  spectra and transition of large-scale anisotropy at ~100 TeV are of
  local source origin. Less than 100 TeV, both spectral hardening and
  anisotropy explicitly indicate the dominant contribution from nearby
  sources. In this work, we further investigate the parameter space of
  sources allowed by the observational energy spectra and anisotropy
  amplitude. To obtain the best-fit source parameters, a numerical
  package to compute the parameter posterior distributions based on
  Bayesian inference, which is applied to perform an elaborate scan
  of parameter space. We find that by combining the energy spectra and
  anisotropy data, the permissible range of location and age of the local
  source is considerably reduced. When comparing with the current local
  supernova remnant (SNR) catalog, only Geminga SNR could be the proper
  candidate of the local cosmic-ray source.

---------------------------------------------------------
Title: Exploring Lorentz Invariance Violation from Ultrahigh-Energy
    γ Rays Observed by LHAASO
Authors: Cao, Zhen; Aharonian, F.; An, Q.; Axikegu, Bai, L. X.; Bai,
   Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai,
   J. T.; Cao, Zhe; Chang, J.; Chang, J. F.; Chen, B. M.; Chen, E. S.;
   Chen, J.; Chen, Liang; Chen, Liang; Chen, Long; Chen, M. J.; Chen,
   M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen,
   X. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui,
   Y. D.; Piazzoli, B. D'ettorre; Dai, B. Z.; Dai, H. L.; Dai, Z. G.;
   Danzengluobu, Della Volpe, D.; Dong, X. J.; Duan, K. K.; Fan, J. H.;
   Fan, Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.;
   Feng, S. H.; Feng, Y. L.; Gao, B.; Gao, C. D.; Gao, L. Q.; Gao, Q.;
   Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.;
   Guo, F. L.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han,
   Y. A.; He, H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.; He,
   Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.; Hu, H. B.; Hu, S.; Hu,
   S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.; Huang, W. H.; Huang,
   X. T.; Huang, X. Y.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.;
   Jiang, K.; Jiang, Z. J.; Jin, C.; Ke, T.; Kuleshov, D.; Levochkin,
   K.; Li, B. B.; Li, Cheng; Li, Cong; Li, F.; Li, H. B.; Li, H. C.;
   Li, H. Y.; Li, Jian; Li, Jie; Li, K.; Li, W. L.; Li, X. R.; Li, Xin;
   Li, Xin; Li, Y.; Li, Y. Z.; Li, Zhe; Li, Zhuo; Liang, E. W.; Liang,
   Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.; Liu, H.; Liu, H. D.;
   Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.;
   Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.; Liu, Z. X.; Long, W. J.; Lu,
   R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao, J. R.; Masood,
   A.; Min, Z.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.;
   Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Qi, Y. Q.; Qiao, B. Q.;
   Qin, J. J.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev,
   O.; Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov,
   V.; Su, Y.; Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang,
   Z. B.; Tian, W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.;
   Wang, J. C.; Wang, J. S.; Wang, L. P.; Wang, L. Y.; Wang, R. N.;
   Wang, W.; Wang, W.; Wang, X. G.; Wang, X. J.; Wang, X. Y.; Wang,
   Y.; Wang, Y. D.; Wang, Y. J.; Wang, Y. P.; Wang, Z. H.; Wang, Z. X.;
   Wang, Zhen; Wang, Zheng; Wei, D. M.; Wei, J. J.; Wei, Y. J.; Wen, T.;
   Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.; Wu, X. F.; Xi, S. Q.; Xia,
   J.; Xia, J. J.; Xiang, G. M.; Xiao, D. X.; Xiao, G.; Xiao, H. B.;
   Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.; Xu, R. X.; Xue, L.;
   Yan, D. H.; Yan, J. Z.; Yang, C. W.; Yang, F. F.; Yang, J. Y.; Yang,
   L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.;
   Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.;
   Yuan, Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.;
   Zhai, X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.;
   Zhang, J. W.; Zhang, L. X.; Zhang, Li; Zhang, Lu; Zhang, P. F.; Zhang,
   P. P.; Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.;
   Zhang, Y. F.; Zhang, Y. L.; Zhang, Yi; Zhang, Yong; Zhao, B.; Zhao,
   J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou,
   B.; Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu,
   C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; Lhaaso Collaboration
2022PhRvL.128e1102C    Altcode:
  Recently, the LHAASO Collaboration published the detection of 12
  ultrahigh-energy γ -ray sources above 100 TeV, with the highest
  energy photon reaching 1.4 PeV. The first detection of PeV γ rays
  from astrophysical sources may provide a very sensitive probe of the
  effect of the Lorentz invariance violation (LIV), which results in
  decay of high-energy γ rays in the superluminal scenario and hence
  a sharp cutoff of the energy spectrum. Two highest energy sources
  are studied in this work. No signature of the existence of the LIV
  is found in their energy spectra, and the lower limits on the LIV
  energy scale are derived. Our results show that the first-order LIV
  energy scale should be higher than about 10<SUP>5</SUP> times the
  Planck scale M<SUB>Pl</SUB> and that the second-order LIV scale is
  &gt;10<SUP>-3</SUP>M<SUB>Pl</SUB> . Both limits improve by at least
  one order of magnitude the previous results.

---------------------------------------------------------
Title: Identification of new M 31 star cluster candidates from PAndAS
    images using convolutional neural networks
Authors: Wang, Shoucheng; Chen, Bingqiu; Ma, Jun; Long, Qian; Yuan,
   Haibo; Liu, Dezi; Zhou, Zhimin; Liu, Wei; Chen, Jiamin; He, Zizhao
2022A&A...658A..51W    Altcode: 2021arXiv211107798W
  Context. Identification of new star cluster candidates in M 31 is
  fundamental for the study of the M 31 stellar cluster system. The
  machine-learning method convolutional neural network (CNN) is
  an efficient algorithm for searching for new M 31 star cluster
  candidates from tens of millions of images from wide-field photometric
  surveys. <BR /> Aims: We search for new M 31 cluster candidates from the
  high-quality g- and i-band images of 21 245 632 sources obtained from
  the Pan-Andromeda Archaeological Survey (PAndAS) through a CNN. <BR />
  Methods: We collected confirmed M 31 clusters and noncluster objects
  from the literature as our training sample. Accurate double-channel CNNs
  were constructed and trained using the training samples. We applied
  the CNN classification models to the PAndAS g- and i-band images of
  over 21 million sources to search new M 31 cluster candidates. The CNN
  predictions were finally checked by five experienced human inspectors
  to obtain high-confidence M 31 star cluster candidates. <BR />
  Results: After the inspection, we identified a catalogue of 117
  new M 31 cluster candidates. Most of the new candidates are young
  clusters that are located in the M 31 disk. Their morphology,
  colours, and magnitudes are similar to those of the confirmed young
  disk clusters. We also identified eight globular cluster candidates
  that are located in the M 31 halo and exhibit features similar to
  those of confirmed halo globular clusters. The projected distances
  to the M 31 centre for three of them are larger than 100 kpc. <P
  />Full Table 2 is only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr/">cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/658/A51">http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/658/A51</A>

---------------------------------------------------------
Title: VizieR Online Data Catalog: NH3 isotope ratios of Galactic
    disk sources (Chen+, 2021)
Authors: Chen, J. L.; Zhang, J. S.; Henkel, C.; Yan, Y. T.; Yu, H. Z.;
   Qiu, J. J.; Tang, X. D.; Wang, J.; Liu, W.; Wang, Y. X.; Zheng, Y. H.;
   Zhao, J. Y.; Zou, Y. P.
2022yCat..22570039C    Altcode:
  For our sample of 210 sources, we made observations of the
  (J,K)=(1,1), (2,2), and (3,3) lines of <SUP>14</SUP>NH<SUB>3</SUB>
  and <SUP>15</SUP>NH<SUB>3</SUB> (23694.5MHz, 23722.6MHz, 23870.1MHz,
  22624.9MHz, 22649.8MHz and 22789.4MHz, respectively), first with
  the Shanghai Tianma 65m radio telescope (TMRT) in 2019 April, May,
  November, and December, with a beam size of ~50". <P />We also used the
  Effelsberg 100m telescope to observe the (J,K)=(1,1), (2,2), and (3,3)
  lines of <SUP>14</SUP>NH<SUB>3</SUB> and <SUP>15</SUP>NH<SUB>3</SUB>
  toward 36 selected sources with strong <SUP>14</SUP>NH<SUB>3</SUB>
  signals from previous TMRT observations in 2019 December and 2020
  January. <P />(4 data files).

---------------------------------------------------------
Title: Winter mixing accelerates decomposition of sedimentary organic
    carbon in seasonally hypoxic coastal seas
Authors: Wei, Lin; Cai, Pinghe; Shi, Xiangming; Cai, Wei-Jun; Liu,
   Wei; Hong, Qingquan; Wu, Tong; Bai, Yan; Cheng, Peng; Sun, Zhenyu
2022GeCoA.317..457W    Altcode:
  Deltaic systems are characterized by the highest sedimentation
  rates in the globe. Meanwhile, sedimentary organic matter therein
  can be efficiently decomposed so that these depositional systems
  may deviate substantially from the oft-quoted correlation between
  net sediment accumulation and preservation of organic matter. The
  exact mechanisms that cause such a deviation in any given case,
  however, remain poorly understood. In this study, we utilize a novel
  <SUP>224</SUP>Ra/<SUP>228</SUP>Th disequilibrium method to examine
  sediment oxygen consumption and the release of diagenetic products of
  organic matter along the major mud wedge system in the inner shelf
  of the East China Sea. Our sampling campaign was carried out in two
  contrasting seasons: the summer when seasonal hypoxia was at its peak
  and physical conditions were relatively quiescent, and the winter
  when the water column was well oxygenated by intense winter mixing and
  underlying deposits were subjected to reworking. Unexpectedly, during
  summer 2017 when the seafloor received the annual maximum supply of
  organic matter, sediment oxygen consumption rates and benthic fluxes
  of NH<SUB>4</SUB><SUP>+</SUP> were relatively low, ranging from 6 to
  59 mmol O<SUB>2</SUB> m<SUP>-2</SUP> d<SUP>-1</SUP> and from 1.6 to
  13 mmol N m<SUP>-2</SUP> d<SUP>-1</SUP>, respectively. In contrast,
  during winter 2018 sediment oxygen consumption rates and benthic fluxes
  of NH<SUB>4</SUB><SUP>+</SUP> surged to 44-690 mmol O<SUB>2</SUB>
  m<SUP>-2</SUP> d<SUP>-1</SUP> and 22-58 mmol N m<SUP>-2</SUP>
  d<SUP>-1</SUP>, respectively. We have also identified an exponential
  relationship between amplification factor of sediment surface area
  and oxygen concentration in the bottom water. This relationship
  suggests that kinetic energy dissipation in the water column not only
  controlled air-sea exchange and seawater mixing, but also intensified
  sediment-water interaction. Importantly, sediment oxygen consumption
  rates (F<SUB>O<SUB>2</SUB></SUB>) in the mud wedge can be empirically
  described using a modified form of Michaelis-Menten kinetics, suggesting
  that F<SUB>O<SUB>2</SUB></SUB>and the associated benthic consumption
  and production of chemicals are controlled by both the transport and
  reaction processes. We have further demonstrated that a large portion
  of the organic matter deposited over the seafloor in summer is likely
  decomposed in winter. Overall, this study highlights intense winter
  mixing as an important mechanism that causes the highly efficient
  decomposition of sedimentary organic matter in coastal seas.

---------------------------------------------------------
Title: Development of 1.2-2.2 GHz Wideband Low Noise Amplifier
Authors: Liu, W. H.; Jiang, P.; Liu, H. F.; Lei, H. K.; Jiang, L.;
   Hu, H.
2022AcASn..63....3L    Altcode:
  In order to detect the weak radio signal, the telescope receiver
  requires good noise performance. As the key circuit of the receiver
  front end, the noise coefficient and gain of the low noise amplifier
  (LNA) determine the noise performance of the whole machine. A 1.2--2.2
  GHz low noise amplifier is designed. The circuit adopts a two-stage
  cascade structure. The second stage introduces negative feedback to
  improve the gain flatness and broaden the bandwidth while reducing
  the noise. After the post-stage input impedance optimization, only one
  capacitor is needed between the stages. Lossy output matching network is
  introduced to realize high gain, low noise, good return loss and flat
  broadband LNA design. The test results show that the gain is 30--33
  dB in the 1.2--2.2 GHz band, the average noise temperature is 47 K,
  and the output 1 dB compression point is greater than 11.3 dBm. Test
  results show that the device has good performance, which can be used
  in the receiver system in this frequency band.

---------------------------------------------------------
Title: The status and future of direct nuclear reaction measurements
    for stellar burning
Authors: Aliotta, M.; Buompane, R.; Couder, M.; Couture, A.; deBoer,
   R. J.; Formicola, A.; Gialanella, L.; Glorius, J.; Imbriani, G.;
   Junker, M.; Langer, C.; Lennarz, A.; Litvinov, Yu A.; Liu, W. -P.;
   Lugaro, M.; Matei, C.; Meisel, Z.; Piersanti, L.; Reifarth, R.;
   Robertson, D.; Simon, A.; Straniero, O.; Tumino, A.; Wiescher, M.;
   Xu, Y.
2022JPhG...49a0501A    Altcode: 2021arXiv210914418A
  The study of stellar burning began just over 100 years ago. Nonetheless,
  we do not yet have a detailed picture of the nucleosynthesis within
  stars and how nucleosynthesis impacts stellar structure and the remnants
  of stellar evolution. Achieving this understanding will require precise
  direct measurements of the nuclear reactions involved. This report
  summarizes the status of direct measurements for stellar burning,
  focusing on developments of the last couple of decades, and offering
  a prospectus of near-future developments.

---------------------------------------------------------
Title: A Real-time, Pipelined Incoherent Dedispersion Method and
    Implementation in FPGA
Authors: Liu, Wei; Meng, Qiao; Wang, Chen; Zhou, Chenye; Yao, Shunyu;
   Tariq, Irfan
2022PASP..134a5008L    Altcode:
  In pulsar observation, dispersion occurs due to the interstellar
  medium. The dispersion significantly affects the detection of pulsar
  signals. To overcome the dispersion effect, incoherent dedispersion
  methods are often applied. The tranditional inchoherent dedispersion
  methods are computationally expensive and troublesome. To deal with this
  problem, in this paper, we developed a Real-Time, Pipelined Incoherent
  Dedispersion Method (RT-PIDM). RT-PIMD only caches the summed-up time
  series, instead of all the frequency spectra, so the memory consumption
  is determined by the number of DM trails, whereas the traditional
  method's memory consumption is determined by the number of frequency
  channels. In most of the situations, the number of frequency channels
  is several times more than that of DM trails, which means the memory
  consumption of traditional methods is more than that of RT-PIDM. With
  RT-PIDM, we designed a 1.2 GHz bandwidth prototype digital backend,
  and we finished pulsar observation with the 40 m radio telescope at
  Yunnan Observatory. The results demonstrate that the RT-PIDM can be
  implemented inside a single FPGA chip with less Block RAM, and the
  proposed RT-PIDM dedisperses the pulsar signal in real time and achieves
  the same result as compared to traditional incoherent dedispersion.

---------------------------------------------------------
Title: Compact Scintillator Array Detector (ComSAD) for Sounding
    Rocket and CubeSat Missions
Authors: Wang, Pu Kai; Chen, Chih-Yun; Hsu, Hsiang-Chieh; Chang,
   Mu-Hsin; Liu, Wei Tai; Fang, Hui-Kuan; Wu, Ting-Chou; Chen, Wen-Hao;
   Tsai, Chin Cheng; Chen, Alfred Bing-Chih; Yang, Yi
2022JAI....1150007W    Altcode: 2021arXiv211012500W
  The development of CubeSats and more frequent launch chances of
  sounding rockets are a total game changer to the space program,
  and it allows us to build space instruments that are technologically
  feasible and affordable. Therefore, it gives us a good opportunity to
  build a small cosmic-ray detector which has capabilities to measure
  the flux, direction, and even energy of cosmic rays at an altitude
  above the limitation of balloon experiments, and it may open a new
  door for building a constellation of detectors to study cosmic-ray
  physics. Compact Scintillator Array Detector (ComSAD) is a funded
  sounding rocket mission of Taiwan’s National Space Organization. In
  this paper, we present the concept, design, and performance of ComSAD
  which is also suitable for future CubeSat missions.

---------------------------------------------------------
Title: Reconciling ultra-high-energy diffuse $\gamma$-rays and the
    knee of cosmic ray light nuclei
Authors: Zhang, Pei-pei; Guo, Yi-qing; Qiao, Bing-qiang; Liu, Wei
2021arXiv211204651Z    Altcode:
  The diffuse $\gamma$-ray was measured up to 957 TeV by the
  Tibet-AS$\gamma$ experiment. Presuming it is produced by the hadronic
  interaction between cosmic ray nuclei and the interstellar medium,
  it requires that the cosmic ray nuclei should be accelerated well
  beyond PeV energies. However, measurements of the spectrum of proton
  and Helium by a few experiments show break below PeV. To solve this
  apparent discrepancy, we propose in this work that a new structure of
  cosmic rays may exist beyond PeV, which can contribute to the highest
  energy diffuse $\gamma$ rays. This additional component may serve
  as another population of Galactic cosmic ray accelerators, and can
  contribute to the cosmic ray fluxes beyond the second knee. Future
  measurements of the energy spectra of different nuclei species may
  test the existence of this new component.

---------------------------------------------------------
Title: The Role of a Weakened Atlantic Meridional Overturning
    Circulation in Modulating Marine Heatwaves in a Warming Climate
Authors: Ren, Xianglin; Liu, Wei
2021GeoRL..4895941R    Altcode:
  We explore the effect of Atlantic meridional overturning circulation
  (AMOC) slowdown on global marine heatwaves (MHWs) under anthropogenic
  warming by maintaining AMOC strength in climate model simulations
  throughout the 21st century. The AMOC slowdown has an insignificant
  effect on global MHWs during the past four decades, except those
  over the North Atlantic warming hole (NAWH) where the weakened AMOC
  reduces the occurrence and duration of MHWs by about half by creating
  a cooler mean-state sea surface temperature. As the AMOC continues
  weakening in current century, its effect becomes significant on MHWs
  in the North Atlantic and Pacific Oceans. The weakened AMOC induces
  a bipolar-seesaw-like change in MHW frequencies, with more frequent
  MHWs in the Southern Hemisphere but less frequent MHWs in the North
  Hemisphere except over the NAWH. The reason for the exception is that
  the NAWH region would enter a near-permanent MHW state without an
  AMOC slowdown.

---------------------------------------------------------
Title: Prospects for the Detection of the Prompt Very-high-energy
    Emission from γ-ray Bursts with the High Altitude Detection of
    Astronomical Radiation Experiment
Authors: Xin, Guang-Guang; Yao, Yu-Hua; Qian, Xiang-Li; Liu, Cheng;
   Gao, Qi; Luo-Bu, Dan-Zeng; Feng, You-Liang; Gou, Quan-Bu; Hu, Hong-Bo;
   Li, Hai-Jin; Liu, Mao-Yuan; Liu, Wei; Qiao, Bing-Qiang; Wang, Zhen;
   Zhang, Yi; Cai, Hao; Chen, Tian-Lu; Guo, Yi-Qing
2021ApJ...923..112X    Altcode: 2021arXiv210304381X
  The observation of very-high-energy (VHE; &gt; 10 GeV) γ-ray emission
  from γ-ray bursts (GRBs), especially in the prompt phase, will provide
  critical information for understanding many aspects of their nature
  including the physical environment, the relativistic bulk motion, the
  mechanisms of particle acceleration of GRBs, and for studying Lorentz
  invariance violation, etc. For the afterglow phase, the highest-energy
  photons detected to date by the imaging atmospheric Cherenkov telescopes
  extend to the TeV regime. However, for the prompt phase, years of
  efforts in searching for the VHE emission has yielded no statistically
  significant detections. A wide field of view and large effective area
  above tens of GeV are essential for detecting the VHE emissions from
  GRBs in the prompt phase. The High Altitude Detection of Astronomical
  Radiation (HADAR) experiment has such merits. In this paper, we report
  the estimates of its expected annual GRB detection rate, which are
  obtained by combining the performance of the HADAR instrument with the
  theoretical calculations based on a phenomenological model to generate
  the pseudo-GRB population. The expected detectable gamma-ray signal
  from GRBs above the background is then obtained to give the detection
  rate. In the spectral model, an extra component is assigned to every GRB
  event in addition to the Band function. The results indicate that if the
  energy of the cutoff due to internal absorption is higher than 50 GeV,
  the detection rate for GRBs for the HADAR experiment is approximately
  two or three GRBs per year, which varies slightly depending upon the
  characteristics of the extra component.

---------------------------------------------------------
Title: Interstellar Nitrogen Isotope Ratios: New NH<SUB>3</SUB>
    Data from the Galactic Center out to the Perseus Arm
Authors: Chen, J. L.; Zhang, J. S.; Henkel, C.; Yan, Y. T.; Yu, H. Z.;
   Qiu, J. J.; Tang, X. D.; Wang, J.; Liu, W.; Wang, Y. X.; Zheng, Y. H.;
   Zhao, J. Y.; Zou, Y. P.
2021ApJS..257...39C    Altcode: 2022arXiv220803977C
  Our aim is to measure the interstellar <SUP>14</SUP>N/<SUP>15</SUP>N
  ratio across the Galaxy, to establish a standard data set on
  interstellar ammonia isotope ratios, and to provide new constraints on
  the Galactic chemical evolution. The (J, K) = (1, 1), (2, 2), and (3,
  3) lines of <SUP>14</SUP>NH<SUB>3</SUB> and <SUP>15</SUP>NH<SUB>3</SUB>
  were observed with the Shanghai Tianma 65 m radio telescope (TMRT)
  and the Effelsberg 100 m telescope toward a large sample of 210
  sources. One hundred fourty-one of these sources were detected by the
  TMRT in <SUP>14</SUP>NH<SUB>3</SUB>. Eight of them were also detected
  in <SUP>15</SUP>NH<SUB>3</SUB>. For 10 of the 36 sources with strong
  NH<SUB>3</SUB> emission, the Effelsberg 100 m telescope successfully
  detected their <SUP>15</SUP>NH<SUB>3</SUB>(1, 1) lines, including
  3 sources (G081.7522, W51D, and Orion-KL) with detections by the
  TMRT telescope. Thus, a total of 15 sources are detected in both the
  <SUP>14</SUP>NH<SUB>3</SUB> and <SUP>15</SUP>NH<SUB>3</SUB> lines. Line
  and physical parameters for these 15 sources are derived, including
  optical depths, rotation and kinetic temperatures, and total column
  densities. <SUP>14</SUP>N/<SUP>15</SUP>N isotope ratios were determined
  from the <SUP>14</SUP>NH<SUB>3</SUB>/<SUP>15</SUP>NH<SUB>3</SUB>
  abundance ratios. The isotope ratios obtained from both telescopes
  agree for a given source within the uncertainties, and no
  dependence on heliocentric distance and kinetic temperature
  is seen. <SUP>14</SUP>N/<SUP>15</SUP>N ratios tend to increase
  with galactocentric distance, confirming a radial nitrogen isotope
  gradient. This is consistent with results from recent Galactic chemical
  model calculations, including the impact of superasymptotic giant
  branch stars and novae.

---------------------------------------------------------
Title: Study on the Pointing Error Model of Terahertz Telescopes
    with Optically Assisted Pointing Measurements
Authors: Ying, X. K.; Luo, Z.; Liu, W.; Zuo, Y. X.
2021AcASn..62...69Y    Altcode:
  In view of the scarcity of terahertz astronomical point source targets,
  this paper studies the method of using a small optical telescope coaxial
  with terahertz antenna to assist the pointing measurement of terahertz
  telescope and establish the pointing error correction model. Based on
  the 1.2 m oblique axis terahertz antenna of Purple Mountain Observatory,
  the experiment of optical aided pointing measurement is carried out. A
  100 mm aperture refractive optical telescope mounted on the antenna
  back frame is used to obtain the pointing measurement accuracy better
  than 2”. In addition, by analyzing the structure of the slant axis
  antenna and the error sources of atmospheric refraction and local
  star time deviation, a slant axis optical pointing correction model
  with 23 error terms is established, and the fitting accuracy of about
  3” is achieved. Finally, with the help of high-precision digital
  photogrammetry, the photoelectric axis consistency is calibrated,
  and its influence on the pointing model accuracy is discussed. The
  research results of this paper will provide technical reference for the
  5 m Dome A Terahertz Explorer (DATE5) and other terahertz telescopes
  in pointing measurement and correction.

---------------------------------------------------------
Title: Panoramic SETI: overall mechanical system design
Authors: Brown, Aaron M.; Aronson, Michael L; Wright, Shelley A.;
   Maire, Jérôme; Cosens, Maren; Wiley, James H.; Antonio, Franklin;
   Horowitz, Paul; Raffanti, Rick; Werthimer, Dan; Liu, Wei
2021arXiv211112771B    Altcode:
  PANOSETI (Pulsed All-Sky Near-infrared Optical Search for
  Extra Terrestrial Intelligence) is a dedicated SETI (Search for
  Extraterrestrial Intelligence) observatory that is being designed to
  observe 4,441 sq. deg. to search for nano- to milli-second transient
  events. The experiment will have a dual observatory system that has
  a total of 90 identical optical 0.48 m telescopes that each have a 99
  square degree field of view. The two observatory sites will be separated
  by 1 km distance to help eliminate false positives and register a
  definitive signal. We discuss the overall mechanical design of the
  telescope modules which includes a Fresnel lens housing, a shutter,
  three baffles, an 32x32 array of Hamamatsu Multi-Photon Pixel Counting
  (MPPC) detectors that reside on a linear stage for focusing. Each
  telescope module will be housed in a triangle of a 3rd tessellation
  frequency geodesic dome that has the ability to have directional
  adjustment to correct for manufacturing tolerances and astrometric
  alignment to the second observatory site. Each observatory will have
  an enclosure to protect the experiment, and an observatory room for
  operations and electronics. We will review the overall design of the
  geodesic domes and mechanical telescope attachments, as well as the
  overall cabling and observatory infrastructure layout.

---------------------------------------------------------
Title: New experimental measurement of <SUP>nat</SUP>Er(n ,γ )
    cross sections between 1 and 100 eV
Authors: Li, X. X.; Liu, L. X.; Jiang, W.; Ren, J.; Wang, H. W.; Fan,
   G. T.; Cao, X. G.; Zhang, Y.; Hu, X. R.; Hao, Z. R.; Kuang, P.; Jiang,
   B.; Wang, X. H.; Hu, J. F.; Wang, J. C.; Wang, D. X.; Zhang, S. Y.;
   Liu, Y. D.; Ma, X.; Ma, C. W.; Wang, Y. T.; An, Z. D.; He, J. J.;
   Su, J.; Zhang, L. Y.; Yang, Y. X.; Liu, W. B.; Su, W. Q.
2021PhRvC.104e4302L    Altcode:
  <SUP>162</SUP>Er and <SUP>164</SUP>Er are two of the 35 p nuclei,
  and their (n ,γ ) cross sections are important input parameters in
  nuclear astrophysics network calculations. The neutron capture cross
  section in the resonance region of isotopes and even the natural erbium
  (<SUP>nat</SUP>Er) sample has not been measured experimentally according
  to the EXFOR database. The (n ,γ ) cross section of <SUP>nat</SUP>Er,
  using C<SUB>6</SUB>D<SUB>6</SUB> liquid scintillator and pulse height
  weighting techniques to measure prompt γ rays, has been measured in the
  energy range of 1-100 eV using a back streaming white neutron facility
  at China Spallation Neutron Source. The deduced neutron capture cross
  sections matches the evaluation databases ENDF/B-VIII.0, ENDF/B-VII.1,
  JENDL-4.0, and ROSFOND-2010, and resonance parameters extracted from
  the R -matrix code in the 1-100 eV region.

---------------------------------------------------------
Title: White-light Continuum Observation of the Off-limb Loops of
the SOL2017-09-10 X8.2 Flare: Temporal and Spatial Variations
Authors: Zhao, Junwei; Liu, Wei; Vial, Jean-Claude
2021ApJ...921L..26Z    Altcode: 2021arXiv211014130Z
  Observations of the Sun's off-limb white-light (WL) flares offer rare
  opportunities to study the energy release and transport mechanisms
  in flare loops. One of the best such events was SOL2017-09-10, an
  X8.2 flare that occurred near the Sun's west limb on 2017 September
  10 and produced a WL loop system lasting more than 60 minutes and
  reaching an altitude higher than 30 Mm. The event was well observed
  by a suite of ground- and space-based instruments, including the
  Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI)
  that captured its off-limb loops in WL continuum near Fe I 6173 Å,
  and the Atmospheric Imager Assembly (SDO/AIA) that observed its
  ultraviolet (UV) and extreme-ultraviolet (EUV) counterparts. We
  found quasi-periodic pulsations in the WL and UV emissions at the
  flare loop-top with a period around 8.0 minutes. Each pulsation
  appears to have an EUV counterpart that occurs earlier in time and
  higher in altitude. Despite many similarities in the WL and UV images
  and light curves, the WL flux at the loop-top continues to grow for
  about 16 minutes while the UV fluxes gradually decay. We discuss the
  implication of these unprecedented observations on the understanding
  of the enigmatic off-limb WL flare emission mechanisms.

---------------------------------------------------------
Title: A strange star scenario for the formation of eccentric
    millisecond pulsar PSR J1946+3417
Authors: Jiang, Long; Wang, Na; Chen, Wen-Cong; Liu, Wei-Min; Leng,
   Chun-Wei; Yuan, Jian-Ping; Qian, Xiang-Li
2021RAA....21..231J    Altcode: 2021arXiv210605717J
  PSR J1946+3417 is a millisecond pulsar (MSP) with a spin period P ≃
  3.17 ms. Harbored in a binary with an orbital period P<SUB>b</SUB> ≃
  27 days, the MSP is accompanied by a white dwarf (WD). The masses of
  the MSP and the WD were determined to be 1.83 M<SUB>⊙</SUB> and 0.266
  M<SUB>⊙</SUB>, respectively. Specially, its orbital eccentricity is e
  ≃ 0.134, which is challenging the recycling model of MSPs. Assuming
  that the neutron star in a binary may collapse to a strange star when
  its mass reaches a critical limit, we propose a phase transition (PT)
  scenario to account for the origin of the system. The sudden mass loss
  and the kick induced by asymmetric collapse during the PT may result in
  the orbital eccentricity. If the PT event takes place after the mass
  transfer ceases, the eccentric orbit cannot be re-circularized in the
  Hubble time. Aiming at the masses of both components, we simulate
  the evolution of the progenitor of PSR J1946+3417 via MESA. The
  simulations show that an NS / main sequence star binary with initial
  masses of 1.4+1.6 M<SUB>⊙</SUB> in an initial orbit of 2.59 days
  will evolve into a binary consisting of a 2.0 M<SUB>⊙</SUB> MSP and
  a 0.27 M<SUB>⊙</SUB> WD in an orbit of ~21.5 days. Assuming that
  the gravitational mass loss fraction during PT is 10%, we simulate
  the effect of PT via the kick program of BSE with a velocity of
  σ<SUB>PT</SUB> = 60 km s<SUP>-1</SUP>. The results show that the PT
  scenario can reproduce the observed orbital period and eccentricity
  with higher probability than other values.

---------------------------------------------------------
Title: Measurements of the center-of-mass energies of {{\boldsymbol
    e(+}{\boldsymbol) e(-}}) collisions at BESIII
Authors: Ablikim, M.; Achasov, M. N.; Adlarson, P.; Ahmed, S.;
   Albrecht, M.; Aliberti, R.; Amoroso, A.; An, M. R.; An, Q.; Bai,
   X. H.; Bai, Y.; Bakina, O.; Baldini Ferroli, R.; Balossino, I.; Ban,
   Y.; Begzsuren, K.; Berger, N.; Bertani, M.; Bettoni, D.; Bianchi,
   F.; Bloms, J.; Bortone, A.; Boyko, I.; Briere, R. A.; Cai, H.; Cai,
   X.; Calcaterra, A.; Cao, G. F.; Cao, N.; Cetin, S. A.; Chang, J. F.;
   Chang, W. L.; Chelkov, G.; Chen, D. Y.; Chen, G.; Chen, H. S.; Chen,
   M. L.; Chen, S. J.; Chen, X. R.; Chen, Y. B.; J. Chen, Z.; Cheng,
   W. S.; Cibinetto, G.; Cossio, F.; Cui, X. F.; Dai, H. L.; Dai, X. C.;
   Dbeyssi, A.; de Boer, R. E.; Dedovich, D.; Deng, Z. Y.; Denig, A.;
   Denysenko, I.; Destefanis, M.; de Mori, F.; Ding, Y.; Dong, C.; Dong,
   J.; Dong, L. Y.; Dong, M. Y.; Dong, X.; Du, S. X.; Fan, Y. L.; Fang,
   J.; Fang, S. S.; Fang, Y.; Farinelli, R.; Fava, L.; Feldbauer, F.;
   Felici, G.; Feng, C. Q.; Feng, J. H.; Fritsch, M.; Fu, C. D.; Gao,
   Y.; Gao, Y.; Gao, Y.; Gao, Y. G.; Garzia, I.; Ge, P. T.; Geng, C.;
   Gersabeck, E. M.; Gilman, A.; Goetzen, K.; Gong, L.; Gong, W. X.;
   Gradl, W.; Greco, M.; Gu, L. M.; Gu, M. H.; Gu, Y. T.; Y Guan, C.; Guo,
   A. Q.; Guo, L. B.; Guo, R. P.; Guo, Y. P.; Guskov, A.; Han, T. T.; Han,
   W. Y.; Hao, X. Q.; Harris, F. A.; He, K. L.; Heinsius, F. H.; Heinz,
   C. H.; Held, T.; Heng, Y. K.; Herold, C.; Himmelreich, M.; Holtmann,
   T.; Hou, G. Y.; Hou, Y. R.; Hou, Z. L.; Hu, H. M.; Hu, J. F.; Hu, T.;
   Hu, Y.; Huang, G. S.; Huang, L. Q.; Huang, X. T.; Huang, Y. P.; Huang,
   Z.; Hussain, T.; Husken, N.; Ikegami Andersson, W.; Imoehl, W.; Irshad,
   M.; Jaeger, S.; Janchiv, S.; Ji, Q.; Ji, Q. P.; Ji, X. B.; Ji, X. L.;
   Ji, Y. Y.; Jiang, H. B.; Jiang, X. S.; Jiao, J. B.; Jiao, Z.; Jin, S.;
   Jin, Y.; Jing, M. Q.; Johansson, T.; Kalantar-Nayestanaki, N.; Kang,
   X. S.; Kappert, R.; Kavatsyuk, M.; Ke, B. C.; Keshk, I. K.; Khoukaz,
   A.; Kiese, P.; Kiuchi, R.; Kliemt, R.; Koch, L.; Kolcu, O. B.; Kopf,
   B.; Kuemmel, M.; Kuessner, M.; Kupsc, A.; Kurth, M. G.; Kuhn, W.; Lane,
   J. J.; Lange, J. S.; Larin, P.; Lavania, A.; Lavezzi, L.; Lei, Z. H.;
   Leithoff, H.; Lellmann, M.; Lenz, T.; Li, C.; Li, C. H.; Li, Cheng;
   Li, D. M.; Li, F.; Li, G.; Li, H.; Li, H.; Li, H. B.; Li, H. J.; Li,
   J. L.; Li, J. Q.; Li, J. S.; Li, Ke; Li, L. K.; Li, Lei; Li, P. R.;
   Li, S. Y.; Li, W. D.; Li, W. G.; Li, X. H.; Li, X. L.; Li, Xiaoyu;
   Li, Z. Y.; Liang, H.; Liang, H.; Liang, H.; Liang, Y. F.; Liang,
   Y. T.; Liao, G. R.; Liao, L. Z.; Libby, J.; Lin, C. X.; Liu, B. J.;
   Liu, C. X.; Liu, D.; Liu, F. H.; Liu, Fang; Liu, Feng; Liu, H. B.;
   Liu, H. M.; Liu, Huanhuan; Liu, Huihui; Liu, J. B.; Liu, J. L.; Liu,
   J. Y.; Liu, K.; Liu, K. Y.; Liu, L.; Liu, M. H.; Liu, P. L.; Liu,
   Q.; Liu, Q.; Liu, S. B.; Liu, Shuai; Liu, T.; Liu, W. M.; Liu, X.;
   Liu, Y.; Liu, Y. B.; Liu, Z. A.; Liu, Z. Q.; Lou, X. C.; Lu, F. X.;
   Lu, H. J.; Lu, J. D.; Lu, J. G.; Lu, X. L.; Lu, Y.; Lu, Y. P.; Luo,
   C. L.; Luo, M. X.; Luo, P. W.; Luo, T.; Luo, X. L.; Lyu, X. R.; Ma,
   F. C.; Ma, H. L.; Ma, L. L.; Ma, M. M.; Ma, Q. M.; Ma, R. Q.; Ma,
   R. T.; Ma, X. X.; Ma, X. Y.; Maas, F. E.; Maggiora, M.; Maldaner,
   S.; Malde, S.; Malik, Q. A.; Mangoni, A.; Mao, Y. J.; Mao, Z. P.;
   Marcello, S.; Meng, Z. X.; Messchendorp, J. G.; Mezzadri, G.; Min,
   T. J.; Mitchell, R. E.; Mo, X. H.; Yu. Muchnoi, N.; Muramatsu, H.;
   Nakhoul, S.; Nefedov, Y.; Nerling, F.; Nikolaev, I. B.; Ning, Z.;
   Nisar, S.; Olsen, S. L.; Ouyang, Q.; Pacetti, S.; Pan, X.; Pan, Y.;
   Pathak, A.; Pathak, A.; Patteri, P.; Pelizaeus, M.; Peng, H. P.;
   Peters, K.; Pettersson, J.; Ping, J. L.; Ping, R. G.; Pogodin, S.;
   Poling, R.; Prasad, V.; Qi, H.; Qi, H. R.; Qi, K. H.; Qi, M.; Qi,
   T. Y.; Qian, S.; Qian, W. B.; Qian, Z.; Qiao, C. F.; Qin, L. Q.; Qin,
   X. P.; Qin, X. S.; Qin, Z. H.; Qiu, J. F.; Qu, S. Q.; Rashid, K. H.;
   Ravindran, K.; Redmer, C. F.; Rivetti, A.; Rodin, V.; Rolo, M.; Rong,
   G.; Rosner, Ch.; Rump, M.; Sang, H. S.; Sarantsev, A.; Schelhaas, Y.;
   Schnier, C.; Schoenning, K.; Scodeggio, M.; Shan, D. C.; Shan, W.;
   Shan, X. Y.; Shangguan, J. F.; Shao, M.; Shen, C. P.; Shen, H. F.;
   Shen, P. X.; Shen, X. Y.; Shi, H. C.; Shi, R. S.; Shi, X.; D Shi,
   X.; Song, J. J.; Song, W. M.; Song, Y. X.; Sosio, S.; Spataro, S.;
   Su, K. X.; Su, P. P.; Sui, F. F.; Sun, G. X.; Sun, H. K.; Sun, J. F.;
   Sun, L.; Sun, S. S.; Sun, T.; Sun, W. Y.; Sun, W. Y.; Sun, X.; Sun,
   Y. J.; Sun, Y. K.; Sun, Y. Z.; Sun, Z. T.; Tan, Y. H.; Tan, Y. X.;
   Tang, C. J.; Tang, G. Y.; Tang, J.; Teng, J. X.; Thoren, V.; Tian,
   W. H.; Tian, Y. T.; Uman, I.; Wang, B.; Wang, C. W.; Wang, D. Y.;
   Wang, H. J.; Wang, H. P.; Wang, K.; Wang, L. L.; Wang, M.; Wang,
   M. Z.; Wang, Meng; Wang, W.; Wang, W. H.; Wang, W. P.; Wang, X.; Wang,
   X. F.; Wang, X. L.; Wang, Y.; Wang, Y.; Wang, Y. D.; Wang, Y. F.;
   Wang, Y. Q.; Wang, Y. Y.; Wang, Z.; Wang, Z. Y.; Wang, Ziyi; Wang,
   Zongyuan; Wei, D. H.; Weidner, F.; Wen, S. P.; White, D. J.; Wiedner,
   U.; Wilkinson, G.; Wolke, M.; Wollenberg, L.; Wu, J. F.; Wu, L. H.;
   Wu, L. J.; Wu, X.; Wu, Z.; Xia, L.; Xiao, H.; Xiao, S. Y.; Xiao, Z. J.;
   Xie, X. H.; Xie, Y. G.; Xie, Y. H.; Xing, T. Y.; Xu, G. F.; Xu, Q. J.;
   Xu, W.; Xu, X. P.; Xu, Y. C.; Yan, F.; Yan, L.; Yan, W. B.; Yan, W. C.;
   Yan, Xu; Yang, H. J.; Yang, H. X.; Yang, L.; Yang, S. L.; Yang, Y. X.;
   Yang, Yifan; Yang, Zhi; Ye, M.; Ye, M. H.; Yin, J. H.; You, Z. Y.;
   Yu, B. X.; Yu, C. X.; Yu, G.; Yu, J. S.; Yu, T.; Yuan, C. Z.; Yuan,
   L.; Yuan, X. Q.; Yuan, Y.; Yuan, Z. Y.; Yue, C. X.; Zafar, A. A.;
   Zeng Zeng, X.; Zeng, Y.; Zhang, A. Q.; Zhang, B. X.; Zhang, Guangyi;
   Zhang, H.; Zhang, H. H.; Zhang, H. H.; Zhang, H. Y.; Zhang, J. J.;
   Zhang, J. L.; Zhang, J. Q.; Zhang, J. W.; Zhang, J. Y.; Zhang, J. Z.;
   Zhang, Jianyu; Zhang, Jiawei; Zhang, L. M.; Zhang, L. Q.; Zhang, Lei;
   Zhang, S.; Zhang, S. F.; Zhang, Shulei; Zhang, X. D.; Zhang, X. Y.;
   Zhang, Y.; Zhang, Y. T.; Zhang, Y. H.; Zhang, Yan; Zhang, Yao; Zhang,
   Z. Y.; Zhao, G.; Zhao, J.; Zhao, J. Y.; Zhao, J. Z.; Zhao, Lei; Zhao,
   Ling; Zhao, M. G.; Zhao, Q.; Zhao, S. J.; Zhao, Y. B.; Zhao, Y. X.;
   Zhao, Z. G.; Zhemchugov, A.; Zheng, B.; Zheng, J. P.; Zheng, Y. H.;
   Zhong, B.; Zhong, C.; Zhou, L. P.; Zhou, Q.; Zhou, X.; Zhou, X. K.;
   Zhou, X. R.; Zhou, X. Y.; Zhu, A. N.; Zhu, J.; Zhu, K.; Zhu, K. J.;
   Zhu, S. H.; Zhu, T. J.; Zhu, W. J.; Zhu, W. J.; Zhu, Y. C.; Zhu,
   Z. A.; Zou, B. S.; Zou, J. H.; Collaboration), (Besiii
2021ChPhC..45j3001A    Altcode:
  During the 2016-17 and 2018-19 running periods, the BESIII
  experiment collected 7.5 fb $ ^{-1} $ of $ e^+e^- $ collision data
  at center-of-mass energies ranging from 4.13 to 4.44 GeV. These data
  samples are primarily used for the study of excited charmonium and
  charmoniumlike states. By analyzing the di-muon process $e^+e^- \to $
  $ (\gamma_{\rm ISR/FSR}) \mu^+\mu^-$ , we measure the center-of-mass
  energies of the data samples with a precision of 0.6 MeV. Through a
  run-by-run study, we find that the center-of-mass energies were stable
  throughout most of the data-collection period. * Supported in part by
  National Key Research and Development Program of China (2020YFA0406300,
  2020YFA0406400); National Natural Science Foundation of China
  (NSFC) (11625523, 11635010, 11735014, 11822506, 11835012, 11935015,
  11935016, 11935018, 11961141012); the Chinese Academy of Sciences
  (CAS) Large-Scale Scientific Facility Program; Joint Large-Scale
  Scientific Facility Funds of the NSFC and CAS (U1732263, U1832207);
  CAS Key Research Program of Frontier Sciences (QYZDJ-SSW-SLH003,
  QYZDJ-SSW-SLH040); 100 Talents Program of CAS; INPAC and Shanghai
  Key Laboratory for Particle Physics and Cosmology; ERC (758462);
  European Union Horizon 2020 research and innovation programme
  (Marie Sklodowska-Curie grant agreement No 894790); German Research
  Foundation DFG (443159800), Collaborative Research Center CRC 1044,
  FOR 2359, FOR 2359, GRK 214; Istituto Nazionale di Fisica Nucleare,
  Italy; Ministry of Development of Turkey (DPT2006K-120470); National
  Science and Technology fund; Olle Engkvist Foundation (200-0605); STFC
  (United Kingdom); The Knut and Alice Wallenberg Foundation (Sweden)
  (2016.0157); The Royal Society, UK (DH140054, DH160214); The Swedish
  Research Council; U. S. Department of Energy (DE-FG02-05ER41374,
  DE-SC-0012069)

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Title: Constraining the cosmic ray propagation halo thickness using
    Fermi-LAT observations of high-latitude clouds
Authors: Yao, Yuhua; Qiao, Bing-Qiang; Liu, Wei; Yuan, Qiang; Hu,
   Hong-Bo; Bi, Xiao-Jun; Yang, Chao-Wen; Guo, Yi-Qing
2021ChPhC..45j5104Y    Altcode: 2021arXiv210300727Y
  The diffusive halo is a basic characteristic of cosmic ray (CR)
  propagation and can advance our understanding of many CR-related
  phenomena and indirect dark matter. The method used to derive the
  halo size often has degeneracy problems and is thus affected by large
  uncertainties. The diffuse $\rm\gamma$ rays from high-latitude clouds
  might shed light on the halo size independently. Because predictions
  using the spatially dependent propagation (SDP) model have better
  agreement with the observed CRs than those of the conventional
  propagation model, in this work, we investigated halo thickness based
  on the SDP model using Fermi-LAT $\rm\gamma$ -ray observations of high-
  and intermediate-velocity clouds. We found that to avoid exceeding the
  relative $\gamma$ -ray emissivity in high-latitude clouds, the halo
  thickness should be in the range of 3.3-9 kpc. Moreover, the spatial
  morphology of $\rm\gamma$ -rays estimated based on the SDP model for
  different values of the halo thickness are distinctive, which provides
  us with a tool to determine the halo size. This newly developed model
  can be tested and tuned using multi-wavelength observations in future
  studies. * Supported by the National Key R&amp;D Program of China
  (2018YFA0404202) and the National Natural Science Foundation of China
  (11635011, 11875264, 11722328, 11851305, U1738205, U2031110)

---------------------------------------------------------
Title: Laboratory Observation of C and O Emission Lines of the White
    Dwarf H1504+65-like Atmosphere Model
Authors: Ma, Bu-Bo; Ren, Jie-Ru; Wang, Shao-Yi; Hoffmann, Dieter H. H.;
   Deng, Zhi-Gang; Qi, Wei; Wang, Xing; Yin, Shuai; Feng, Jian-Hua; Fan,
   Quan-Ping; Liu, Wei; Xu, Zhong-Feng; Chen, Yong; Cui, Bo; He, Shu-Kai;
   Cao, Zhu-Rong; Zhao, Zong-Qing; Gu, Yu-Qiu; Zhu, Shao-Ping; Cheng,
   Rui; Zhou, Xian-Ming; Xiao, Guo-Qing; Zhao, Hong-Wei; Zhang, Yi-Hang;
   Zhang, Zhe; Li, Yu-Tong; Xu, Xing; Wei, Wen-Qing; Chen, Ben-Zheng;
   Zhang, Shi-Zheng; Hu, Zhong-Min; Liu, Li-Rong; Li, Fang-Fang; Xu,
   Hao; Zhou, Wei-Min; Cao, Lei-Feng; Zhao, Yong-Tao
2021ApJ...920..106M    Altcode:
  White dwarfs play important roles in stellar evolution and help us
  gauge the age of our galaxy. The white dwarf H1504+65, the hottest
  known post-asymptotic giant branch star, is peculiar due to its C- and
  O-rich but He- and H- deficient atmosphere whose composition cannot
  be well predicted by current stellar evolution models. The analysis
  of the elemental abundance and the benchmark of stellar atmospheric
  models depends heavily on spectral data under cosmic conditions, which
  are currently extremely scarce. We created a well-defined, uniform,
  relatively large-scale ~millimeter plasma sample in the laboratory
  with a temperature and a C/O ratio similar to those of H1504+65's
  atmosphere. The emission spectra with high precision in the range of
  10-80 nm were obtained and identified according to databases such as
  NIST and Kelly. A detailed comparison between our emission lines and the
  Chandra-observed white dwarf H1504+65 atmosphere's absorption lines was
  performed. The stongly isolated O VI lines in the range of 10-13 nm are
  observed in both cases. We observed a wealth of O V lines in the range
  of 13-14 nm that cannot be well identified or predicted by models due
  to the weak flux and also probably due to the blending effect of Fe
  group elements in the Chandra spectrum. Long-wavelength lines ranging
  from 14 to 80 nm, which are not observed in the Chandra spectrum
  because of the high interstellar neutral hydrogen column density,
  show abundant O IV-V, C IV lines, and strong O VI lines. Moreover,
  the intensities of the lines at 62.973 and 17.216 nm are analyzed to
  characterize the plasma temperature.

---------------------------------------------------------
Title: Property investigation of the wedge-shaped CsI(Tl) crystals
    for a charged-particle telescope
Authors: Li, G.; Lou, J. L.; Ye, Y. L.; Hua, H.; Wang, H.; Han, J. X.;
   Liu, W.; Bai, S. W.; Tan, Z. W.; Ma, K.; Chen, J. H.; Yang, L. S.;
   Wang, S. J.; Hu, Z. Y.; Yu, H. Z.; Zhu, H. Y.; Xia, B. L.; Jiang, Y.;
   Liu, Y.; Yang, X. F.; Li, Q. T.; Xu, J. Y.; Wang, J. S.; Yang, Y. Y.;
   Ma, J. B.; Chen, R. F.; Ma, P.; Bai, Z.; Duan, F. F.; Hu, L. Y.; Li,
   J. W.; Li, Y.,; Song, Y. S.; Zhang, Suyalatu; Huang, M. R.
2021NIMPA101365637L    Altcode:
  Two types of wedge-shaped CsI(Tl) crystals were designed to be placed
  behind an annular double-sided silicon detector to identify light
  charged-particles with the ΔE - E method. The properties of the CsI(Tl)
  detectors with different shapes and sizes were investigated using an α
  source and a radioactive beam of <SUP>15</SUP>C. The larger crystal
  was found to have better energy resolution, smaller light output
  non-uniformity, as well as better particle identification capability,
  and was finally adopted to form the ΔE - E telescope. The performance
  of the two types of CsI(Tl) crystals are interpreted based on Geant4
  simulation results.

---------------------------------------------------------
Title: Discovery of the Ultrahigh-energy Gamma-Ray Source LHAASO
    J2108+5157
Authors: Cao, Zhen; Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai,
   Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai,
   J. T.; Cao, Zhe; Chang, J.; Chang, J. F.; Chen, B. M.; Chen, E. S.;
   Chen, J.; Chen, Liang; Chen, Long; Chen, M. J.; Chen, M. L.; Chen,
   Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen, Y.;
   Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Piazzoli,
   B. D'Ettorre; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Dan-Zeng-Luo-Bu,
   Dan-Zeng; Volpe, D. della; Dong, X. J.; Duan, K. K.; Fan, J. H.; Fan,
   Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng,
   S. H.; Feng, Y. L.; Gao, B.; Gao, C. D.; Gao, L. Q.; Gao, Q.; Gao,
   W.; Ge, M. M.; Geng, L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo,
   F. L.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He,
   H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.; He, Y.; Heller, M.;
   Hor, Y. K.; Hou, C.; Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang,
   D. H.; Huang, Q. L.; Huang, W. H.; Huang, X. T.; Huang, X. Y.; Huang,
   Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin,
   C.; Ke, T.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li, Cheng; Li,
   Cong; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.; Li,
   W. L.; Li, X. R.; Li, Xin; Li, Xin; Li, Y.; Li, Y. Z.; Li, Zhe; Li,
   Zhuo; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu,
   D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.;
   Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.;
   Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma,
   X. H.; Mao, J. R.; Masood, A.; Min, Z.; Mitthumsiri, W.; Montaruli,
   T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi,
   M. Y.; Qi, Y. Q.; Qiao, B. Q.; Qin, J. J.; Ruffolo, D.; Rulev, V.;
   Sáiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. Y.; Song,
   H. C.; Stenkin, Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.; Sun, X. N.;
   Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang, B. D.;
   Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang,
   L. P.; Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang, X. G.;
   Wang, X. J.; Wang, X. Y.; Wang, Y.; Wang, Y. D.; Wang, Y. J.; Wang,
   Y. P.; Wang, Z. H.; Wang, Z. X.; Wang, Zhen; Wang, Zheng; Wei, D. M.;
   Wei, J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu,
   W. X.; Wu, X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao,
   D. X.; Xiao, G.; Xiao, H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu,
   D. L.; Xu, R. X.; Xue, L.; Yan, D. H.; Yan, J. Z.; Yang, C. W.; Yang,
   F. F.; Yang, J. Y.; Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.;
   Yao, Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.;
   You, Z. Y.; Yu, Y. H.; Yuan, Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.;
   Zeng, Z. K.; Zha, M.; Zhai, X. X.; Zhang, B. B.; Zhang, H. M.; Zhang,
   H. Y.; Zhang, J. L.; Zhang, J. W.; Zhang, L. X.; Zhang, Li; Zhang,
   Lu; Zhang, P. F.; Zhang, P. P.; Zhang, R.; Zhang, S. R.; Zhang, S. S.;
   Zhang, X.; Zhang, X. P.; Zhang, Y. F.; Zhang, Y. L.; Zhang, Yi; Zhang,
   Yong; Zhao, B.; Zhao, J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng,
   F.; Zheng, Y.; Zhou, B.; Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.;
   Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.
2021ApJ...919L..22C    Altcode: 2021arXiv210609865T
  We report the discovery of an ultrahigh-energy (UHE) gamma-ray source,
  LHAASO J2108+5157, by analyzing the LHAASO-KM2A data of 308.33 live
  days. A significant excess of gamma ray-induced showers is observed
  in both energy bands of 25-100 and &gt;100 TeV with 9.5σ and 8.5σ,
  respectively. This source is not significantly favored as an extended
  source with an angular extension smaller than the point-spread function
  of KM2A. The measured energy spectrum from 20 to 200 TeV can be
  approximately described by a power-law function with an index of -2.83
  ± 0.18<SUB>stat</SUB>. A harder spectrum is demanded at lower energies
  considering the flux upper limit set by Fermi-LAT observations. The
  position of the gamma-ray emission is correlated with a giant molecular
  cloud, which favors a hadronic origin. No obvious counterparts have
  been found, and deeper multiwavelength observations will help to cast
  new light on this intriguing UHE source.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Sulfur isotopes in SFR with 12m
    ARO and 30m IRAM (Yu+, 2020)
Authors: Yu, H. Z.; Zhang, J. S.; Henkel, C.; Yan, Y. T.; Liu, W.;
   Tang, X. D.; Langer, N.; Luan, T. C.; Chen, J. L.; Wang, Y. X.; Deng,
   G. G.; Zou, Y. P.
2021yCat..18990145Y    Altcode:
  The observations were performed in 2018 November and December using
  the Arizona Radio Observatory (ARO) 12m telescope toward 95 massive
  star-forming regions. A 3mm sideband separating (SBS) receiver was
  employed covering Atacama Large Millimeter/submillimeter Array (ALMA)
  band 3 (84-116GHz). The center frequencies were set at 97.980986,
  96.412982, 92.494299, and 97.172086GHz for the CS, C34S, 13CS, and
  C33S lines, respectively; the beam size was ~63". <P />Six sources
  among our sample were also observed by the Institut de radioastronomie
  millimetrique (IRAM) 30m with the Eight MIxer Receive (EMIR) heterodyne
  receiver during June 2016. We applied the {lmabda}~3mm E090 band to
  observe the J=2-1 lines of the CS, C34S, 13CS, and C33S isotopologs. A
  fast Fourier transform spectrometer (FTS) backend in the wideband mode
  was employed in our observations, with a spectral resolution of 400kHz
  (~0.6km/s at 96GHz). <P />(3 data files).

---------------------------------------------------------
Title: Direct Measurement of the Astrophysical F 19 (p ,α γ )O 16
    Reaction in the Deepest Operational Underground Laboratory
Authors: Zhang, L. Y.; Su, J.; He, J. J.; Wiescher, M.; deBoer, R. J.;
   Kahl, D.; Chen, Y. J.; Li, X. Y.; Wang, J. G.; Zhang, L.; Cao, F. Q.;
   Zhang, H.; Zhang, Z. C.; Jiao, T. Y.; Sheng, Y. D.; Wang, L. H.;
   Song, L. Y.; Jiang, X. Z.; Li, Z. M.; Li, E. T.; Wang, S.; Lian, G.;
   Li, Z. H.; Tang, X. D.; Zhao, H. W.; Sun, L. T.; Wu, Q.; Li, J. Q.;
   Cui, B. Q.; Chen, L. H.; Ma, R. G.; Guo, B.; Xu, S. W.; Li, J. Y.;
   Qi, N. C.; Sun, W. L.; Guo, X. Y.; Zhang, P.; Chen, Y. H.; Zhou, Y.;
   Zhou, J. F.; He, J. R.; Shang, C. S.; Li, M. C.; Zhou, X. H.; Zhang,
   Y. H.; Zhang, F. S.; Hu, Z. G.; Xu, H. S.; Chen, J. P.; Liu, W. P.
2021PhRvL.127o2702Z    Altcode:
  Fluorine is one of the most interesting elements in nuclear
  astrophysics, where the F 19 (p ,α )O 16 reaction is of crucial
  importance for Galactic F 19 abundances and CNO cycle loss in first
  generation Population III stars. As a day-one campaign at the Jinping
  Underground Nuclear Astrophysics experimental facility, we report
  direct measurements of the essential F 19 (p ,α γ )O 16 reaction
  channel. The γ -ray yields were measured over E<SUB>c .m .</SUB>=72.4
  - 344 keV , covering the Gamow window; our energy of 72.4 keV is
  unprecedentedly low, reported here for the first time. The experiment
  was performed under the extremely low cosmic-ray-induced background
  environment of the China JinPing Underground Laboratory, one of the
  deepest underground laboratories in the world. The present low-energy
  S factors deviate significantly from previous theoretical predictions,
  and the uncertainties are significantly reduced. The thermonuclear F
  19 (p ,α γ )O 16 reaction rate has been determined directly at the
  relevant astrophysical energies.

---------------------------------------------------------
Title: The <SUP>59</SUP>Fe (n,γ) <SUP>60</SUP>Fe Cross Section from
    the Surrogate Ratio Method and Its Effect on the <SUP>60</SUP>Fe
    Nucleosynthesis
Authors: Yan, S. Q.; Li, X. Y.; Nishio, K.; Lugaro, M.; Li, Z. H.;
   Makii, H.; Pignatari, M.; Wang, Y. B.; Orlandi, R.; Hirose, K.;
   Tsukada, K.; Mohr, P.; Li, G. S.; Wang, J. G.; Gao, B. S.; Han, Y. L.;
   Guo, B.; Li, Y. J.; Shen, Y. P.; Sato, T. K.; Ito, Y.; Suzaki, F.; Su,
   J.; Yang, Y. Y.; Wang, J. S.; Ma, J. B.; Ma, P.; Bai, Z.; Xu, S. W.;
   Ren, J.; Fan, Q. W.; Zeng, S.; Han, Z. Y.; Nan, W.; Nan, W. K.; Chen,
   C.; Lian, G.; Hu, Q.; Duan, F. F.; Jin, S. Y.; Tang, X. D.; Liu, W. P.
2021ApJ...919...84Y    Altcode: 2021arXiv210912654Y
  The long-lived <SUP>60</SUP>Fe (with a half-life of 2.62 Myr) is a
  crucial diagnostic of active nucleosynthesis in the Milky Way galaxy
  and in supernovae near the solar system. The neutron-capture reaction
  <SUP>59</SUP>Fe(n,γ)<SUP>60</SUP>Fe on <SUP>59</SUP>Fe (half-life =
  44.5 days) is the key reaction for the production of <SUP>60</SUP>Fe
  in massive stars. This reaction cross section has been previously
  constrained by the Coulomb dissociation experiment, which offered
  partial constraint on the E1 γ-ray strength function but a negligible
  constraint on the M1 and E2 components. In this work, for the first
  time, we use the surrogate ratio method to experimentally determine
  the <SUP>59</SUP>Fe(n,γ)<SUP>60</SUP>Fe cross sections in which all
  the components are included. We derived a Maxwellian-averaged cross
  section of 27.5 ± 3.5 mb at kT = 30 keV and 13.4 ± 1.7 mb at kT =
  90 keV, roughly 10%-20% higher than previous estimates. We analyzed the
  impact of our new reaction rates in nucleosynthesis models of massive
  stars and found that uncertainties in the production of <SUP>60</SUP>Fe
  from the <SUP>59</SUP>Fe(n,γ)<SUP>60</SUP>Fe rate are at most 25%. We
  conclude that stellar physics uncertainties now play a major role in
  the accurate evaluation of the stellar production of <SUP>60</SUP>Fe.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Quiet-Sun MgII h &amp; k line
    profiles from IRIS (Gunar+, 2021)
Authors: Gunar, S.; Koza, J.; Schwartz, P.; Heinzel, P.; Liu, W.
2021yCat..22550016G    Altcode:
  Since its launch, the Interface Region Imaging Spectrograph (IRIS)
  commenced a quasi-regular acquisition of maps of the entire solar
  disk in both NUV and FUV spectral ranges. At the time of writing,
  the archive of the IRIS full-Sun mosaics contained 91 observations
  spanning the period from 2013 September 30 to 2020 October 19 which
  cover two spectral windows of +/-1.75Å centered at 2803.53Å (MgII h)
  and 2796.35Å (MgII k). <P />(4 data files).

---------------------------------------------------------
Title: Calibration of the air shower energy scale of the water and
    air Cherenkov techniques in the LHAASO experiment
Authors: Aharonian, F.; An, Q.; Axikegu, Bai, L. X.; Bai, Y. X.; Bao,
   Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao,
   Zhen; Cao, Zhe; Chang, J.; Chang, J. F.; Chen, B. M.; Chen, E. S.;
   Chen, J.; Chen, Liang; Chen, Liang; Chen, Long; Chen, M. J.; Chen,
   M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.;
   Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.;
   Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu, Della Volpe, D.;
   Piazzoli, B. D'ettorre; Dong, X. J.; Duan, K. K.; Fan, J. H.; Fan,
   Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng,
   S. H.; Feng, Y. L.; Gao, B.; Gao, C. D.; Gao, L. Q.; Gao, Q.; Gao,
   W.; Ge, M. M.; Geng, L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo,
   F. L.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He,
   H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.; He, Y.; Heller, M.;
   Hor, Y. K.; Hou, C.; Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang,
   D. H.; Huang, Q. L.; Huang, W. H.; Huang, X. T.; Huang, X. Y.; Huang,
   Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin,
   C.; Ke, T.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li, Cong; Li,
   Cheng; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.; Li,
   W. L.; Li, Xin; Li, Xin; Li, X. R.; Li, Y.; Li, Y. Z.; Li, Zhe; Li,
   Zhuo; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu,
   D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.;
   Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.;
   Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma,
   X. H.; Mao, J. R.; Masood, A.; Min, Z.; Mitthumsiri, W.; Montaruli, T.;
   Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.;
   Qi, Y. Q.; Qiao, B. Q.; Qin, J. J.; Ruffolo, D.; Rulev, V.; Sáiz,
   A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. Y.; Song, H. C.;
   Stenkin, Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.; Sun, X. N.; Sun,
   Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang, B. D.; Wang,
   C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang, L. P.;
   Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang, X. G.; Wang,
   X. J.; Wang, X. Y.; Wang, Y.; Wang, Y. D.; Wang, Y. J.; Wang, Y. P.;
   Wang, Z. H.; Wang, Z. X.; Wang, Zhen; Wang, Zheng; Wei, D. M.; Wei,
   J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.;
   Wu, X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, D. X.;
   Xiao, G.; Xiao, H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.;
   Xu, R. X.; Xue, L.; Yan, D. H.; Yan, J. Z.; Yang, C. W.; Yang, F. F.;
   Yang, J. Y.; Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao,
   Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You,
   Z. Y.; Yu, Y. H.; Yuan, Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng,
   Z. K.; Zha, M.; Zhai, X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.;
   Zhang, J. L.; Zhang, J. W.; Zhang, Lu; Zhang, Li; Zhang, L. X.; Zhang,
   P. F.; Zhang, P. P.; Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang,
   X.; Zhang, X. P.; Zhang, Y. F.; Zhang, Y. L.; Zhang, Yong; Zhang,
   Yi; Zhao, B.; Zhao, J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng,
   F.; Zheng, Y.; Zhou, B.; Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.;
   Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.;
   Lhaaso Collaboration
2021PhRvD.104f2007A    Altcode: 2021arXiv210404965A
  The Wide Field-of-View Cherenkov Telescope Array (WFCTA) and the Water
  Cherenkov Detector Array (WCDA) of LHAASO are designed to work in
  combination for measuring the energy spectra of the cosmic ray species
  over a very wide energy range from a few TeV to 10 PeV. The energy
  calibration can be achieved with a proven technique of measuring
  the westward shift of the Moon shadow cast by galactic cosmic rays
  due to the geomagnetic field. This deflection angle Δ is inversely
  proportional to the cosmic ray rigidity. The precise measurement of the
  shifts by WCDA allows us to calibrate its energy scale for energies as
  high as 35 TeV. Through a set of commonly triggered events, the energy
  scales can be propagated to WFCTA. The energies of the events can be
  derived both by WCDA-1 and WFCTA with the median energies 23.4 ±0.1
  ±1.3 TeV and (21.9 ±0.1 TeV ), respectively, which are consistent
  within uncertainties. In addition, the propagation of the energy scale
  is also validated by the Moon shadow based on the same data selection
  criteria of the commonly triggered events. This paper reports, for
  the first time, an observational measurement of the absolute energy
  scale of the primary cosmic rays generating showers observed by air
  Cherenkov telescopes.

---------------------------------------------------------
Title: Energy Flux Densities at Dipolarization Fronts
Authors: Liu, C. M.; Fu, H. S.; Yu, Y. Q.; Lu, H. Y.; Liu, W. L.;
   Xu, Y.; Giles, B. L.; Burch, J. L.
2021GeoRL..4894932L    Altcode:
  Dipolarization fronts (DFs) have been suggested as crucial energy
  conversion sites contributing significantly to global energy transfer
  in the magnetosphere. However, energy partitioning of DF-driven energy
  transfer remains hitherto elusive. Using high-cadence data from
  MMS spacecraft, we present a detailed investigation of energy flux
  densities at two DFs with/without surface ripples. We find that during
  both DF intervals, electron enthalpy flux increases dramatically,
  carries the greatest energy, and well correlates with local energy
  conversion. Poynting flux also increases but contributes to a relatively
  smaller portion. Ion enthalpy flux which in magnitude is slightly
  smaller than electron enthalpy flux barely changes. Particle kinetic
  energy and heat fluxes are negligible. Strong difference in energy
  fluxes observed by different spacecraft is found at the rippled DF,
  indicating three-dimensional energy transport. These results indicate
  that energy budgets at the DFs are dominated by electron physics,
  rather than ion dynamics suggested by previous studies.

---------------------------------------------------------
Title: An efficient channelization architecture and its implementation
    for radio astronomy
Authors: Liu, W.; Meng, Q.; Wang, C.; Zhou, C.; Yao, S.; Tariq, I.
2021JInst..16P8047L    Altcode:
  Channelization is one of the most important parts in a Digital
  Back-End(DBE) for radio astronomy. A DBE with wider bandwidth and
  higher resolution consumes larger amount of computing and memory
  resources, which results in much higher hardware cost. This paper
  presents an efficient channelization architecture, which consists
  of Bit-Inverted, Parallel Complex Fast Fourier Transform(BIPC-FFT)
  and In-place Forward-Backward Decomposition(IPFBD). The efficient
  architecture can assist with saving a lot of resources, so a wide-band
  and high-resolution DBE can be implemented on an resource restricted
  platform. Based on the efficient channelization architecture,
  we designed a Dual-Input, 64K-Channelized prototype DBE with 1.2
  GHz bandwidth on a Xilinx Virtex-6 LX240T Field Programmable Gate
  Array(FPGA) chip. The test results in the lab and observation results at
  Yunnan Observatory demonstrate the DBE can be used for radio astronomy.

---------------------------------------------------------
Title: Direct measurement of the resonance strengths and branching
    ratios of low-energy (p, γ) reactions on Mg isotopes
Authors: Zhang, Hao; Li, Zhi-Hong; Su, Jun; Li, Yun-Ju; Chen, Chen;
   Zhang, Long; Cao, Fu-Qiang; Shen, Yang-Ping; Nan, Wei; Nan, Wei-Ke;
   Li, Xin-Yue; Chen, Li-Hua; Lian, Gang; Cui, Bao-Qun; Guo, Bing;
   Liu, Wei-Ping
2021ChPhC..45h4108Z    Altcode:
  Proton capture reactions on Mg isotopes are significant in the Mg-Al
  cycle in stellar H-burning. In particular, the resonance strengths
  and branching ratios of low-energy resonances in <SUP>25</SUP>Mg(
  $ p,\gamma$ )<SUP>26</SUP>Al reactions determine the production
  of <SUP>26</SUP>Al, which is one of the most important long-lived
  radioactive nuclei in nuclear astrophysics. In this article, we report
  our first experiment using the intense proton beam of approximately 2 mA
  provided by the JUNA accelerator ground laboratory and a new technique
  that can minimize the composition change of targets under intense beam
  irradiation. The resonance strengths and branching ratios of E = 214,
  304, and 326 keV resonances in the reactions of <SUP>24</SUP>Mg(
  $ p,\gamma$ )<SUP>25</SUP>Al, <SUP>25</SUP>Mg( $ p,\gamma$
  )<SUP>26</SUP>Al, and <SUP>26</SUP>Mg( $ p,\gamma$ )<SUP>27</SUP>Al,
  respectively, were measured with high accuracy. The success of this
  experiment provides a good calibration for the nuclear astrophysical
  experiment at the Jinping underground laboratory. * Supported by the
  National Natural Science Foundation of China (11490563, 11961141003)
  and the Continuous Basic Scientific Research Project (WDJC-2019-13)

---------------------------------------------------------
Title: Discovery of a New Gamma-Ray Source, LHAASO J0341+5258,
    with Emission up to 200 TeV
Authors: Cao, Zhen; Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai,
   Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai,
   J. T.; Cao, Zhe; Chang, J.; Chang, J. F.; Chen, B. M.; Chen, E. S.;
   Chen, J.; Chen, Liang; Chen, Liang; Chen, Long; Chen, M. J.; Chen,
   M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen,
   X. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui,
   Y. D.; D'Ettorre Piazzoli, B.; Dai, B. Z.; Dai, H. L.; Dai, Z. G.;
   Danzengluobu; Volpe, D. della; Dong, X. J.; Duan, K. K.; Fan, J. H.;
   Fan, Y. Z.; Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.;
   Feng, S. H.; Feng, Y. L.; Gao, B.; Gao, C. D.; Gao, L. Q.; Gao, Q.;
   Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.;
   Guo, F. L.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.;
   He, H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.; He, Y.; Heller,
   M.; Hor, Y. K.; Hou, C.; Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.;
   Huang, D. H.; Huang, Q. L.; Huang, W. H.; Huang, X. T.; Huang, X. Y.;
   Huang, Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.;
   Jin, C.; Ke, T.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li, Cheng;
   Li, Cong; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.;
   Li, W. L.; Li, X. R.; Li, Xin; Li, Xin; Li, Y.; Li, Y. Z.; Li, Zhe;
   Li, Zhuo; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.;
   Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu,
   J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu,
   Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma,
   L. L.; Ma, X. H.; Mao, J. R.; Masood, A.; Min, Z.; Mitthumsiri, W.;
   Montaruli, T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei,
   Z. Y.; Qi, M. Y.; Qi, Y. Q.; Qiao, B. Q.; Qin, J. J.; Ruffolo, D.;
   Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi,
   J. Y.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.;
   Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang,
   B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.;
   Wang, L. P.; Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang,
   X. G.; Wang, X. J.; Wang, X. Y.; Wang, Y.; Wang, Y. D.; Wang, Y. J.;
   Wang, Y. P.; Wang, Z. H.; Wang, Z. X.; Wang, Zhen; Wang, Zheng; Wei,
   D. M.; Wei, J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.;
   Wu, W. X.; Wu, X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.;
   Xiao, D. X.; Xiao, G.; Xiao, H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.;
   Xu, D. L.; Xu, R. X.; Xue, L.; Yan, D. H.; Yan, J. Z.; Yang, C. W.;
   Yang, F. F.; Yang, J. Y.; Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang,
   S. B.; Yao, Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You,
   X. H.; You, Z. Y.; Yu, Y. H.; Yuan, Q.; Zeng, H. D.; Zeng, T. X.;
   Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai, X. X.; Zhang, B. B.; Zhang,
   H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang, J. W.; Zhang, L. X.; Zhang,
   Li; Zhang, Lu; Zhang, P. F.; Zhang, P. P.; Zhang, R.; Zhang, S. R.;
   Zhang, S. S.; Zhang, X.; Zhang, X. P.; Zhang, Y. F.; Zhang, Y. L.;
   Zhang, Yi; Zhang, Yong; Zhao, B.; Zhao, J.; Zhao, L.; Zhao, L. Z.;
   Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, B.; Zhou, H.; Zhou, J. N.;
   Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.;
   Zhu, K. J.; Zuo, X.
2021ApJ...917L...4C    Altcode: 2021arXiv210702020L
  We report the discovery of a new unidentified extended γ-ray source in
  the Galactic plane named LHAASO J0341+5258 with a pretrial significance
  of 8.2 standard deviations above 25 TeV. The best-fit position is R.A. =
  55°34 ± 0°11 and decl. = 52°97 ± 0°07. The angular size of LHAASO
  J0341+5258 is 0°29 ± 0°06<SUB>stat</SUB> ± 0°02<SUB>sys</SUB>. The
  flux above 25 TeV is about 20% of the flux of the Crab Nebula. Although
  a power-law fit of the spectrum from 10 to 200 TeV with the photon
  index α = 2.98 ± 0.19<SUB>stat</SUB> ± 0.02<SUB>sys</SUB> is not
  excluded, the LHAASO data together with the flux upper limit at 10 GeV
  set by the Fermi-LAT observation, indicate a noticeable steepening of
  an initially hard power-law spectrum with a cutoff at ≍50 TeV. We
  briefly discuss the origin of ultra-high-energy gamma rays. The lack
  of an energetic pulsar and a young supernova remnant inside or in the
  vicinity of LHAASO J0341+5258 challenge, but do not exclude, both the
  leptonic and hadronic scenarios of gamma-ray production.

---------------------------------------------------------
Title: Performance of LHAASO-WCDA and observation of the Crab Nebula
    as a standard candle
Authors: Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai, Y. X.; Bao,
   Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao,
   Z.; Cao, Z.; Chang, J.; Chang, J. F.; Chang, X. C.; Chen, B. M.; Chen,
   J.; Chen, L.; Chen, L.; Chen, L.; Chen, M. J.; Chen, M. L.; Chen,
   Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen,
   Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.;
   Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; Della Volpe, D.;
   Piazzoli, B. D'ettorre; Dong, X. J.; Fan, J. H.; Fan, Y. Z.; Fan,
   Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng,
   Y. L.; Gao, B.; Gao, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.;
   Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.; Guo,
   Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He,
   S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.;
   Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.;
   Huang, W. H.; Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia,
   H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.;
   Li, B. B.; Li, C.; Li, C.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li,
   J.; Li, K.; Li, W. L.; Li, X.; Li, X.; Li, X. R.; Li, Y.; Li, Y. Z.;
   Li, Z.; Li, Z.; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu,
   C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.;
   Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y. N.;
   Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.;
   Ma, X. H.; Mao, J. R.; Masood, A.; Mitthumsiri, W.; Montaruli, T.;
   Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.;
   Qiao, B. Q.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev,
   O.; Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov,
   V.; Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.;
   Tian, W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.;
   Wang, J. S.; Wang, L. P.; Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.;
   Wang, X. G.; Wang, X. J.; Wang, X. Y.; Wang, Y. D.; Wang, Y. J.; Wang,
   Y. P.; Wang, Z.; Wang, Z.; Wang, Z. H.; Wang, Z. X.; Wei, D. M.; Wei,
   J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.;
   Wu, X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, G.;
   Xiao, H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.; Xu, R. X.;
   Xue, L.; Yan, D. H.; Yang, C. W.; Yang, F. F.; Yang, J. Y.; Yang,
   L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.;
   Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.;
   Yuan, Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.;
   Zhai, X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.;
   Zhang, J. W.; Zhang, L.; Zhang, L.; Zhang, L. X.; Zhang, P. F.; Zhang,
   P. P.; Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.;
   Zhang, Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. L.; Zhao, B.; Zhao, J.;
   Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, B.;
   Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.;
   Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; Collaboration), (The Lhaaso
2021ChPhC..45h5002A    Altcode:
  The first Water Cherenkov detector of the LHAASO experiment (WCDA-1)
  has been operating since April 2019. The data for the first year have
  been analyzed to test its performance by observing the Crab Nebula
  as a standard candle. The WCDA-1 achieves a sensitivity of 65 mCU per
  year, with a statistical threshold of 5 $\sigma$ . To accomplish this,
  a 97.7% cosmic-ray background rejection rate around 1 TeV and 99.8%
  around 6 TeV with an approximate photon acceptance of 50% is achieved
  after applying an algorithm to separate gamma-induced showers. The
  angular resolution is measured using the Crab Nebula as a point source
  to be approximately 0.45° at 1 TeV and better than 0.2° above 6 TeV,
  with a pointing accuracy better than 0.05°. These values all match
  the design specifications. The energy resolution is found to be 33% for
  gamma rays around 6 TeV. The spectral energy distribution of the Crab
  Nebula in the range from 500 GeV to 15.8 TeV is measured and found to be
  in agreement with the results from other TeV gamma ray observatories. *
  Supported by the following grants: the National Key R&amp;D program of
  China (2018YFA0404201, 2018YFA0404202, 2018YFA0404203), the National
  Natural Science Foundation of China (12022502, 11905227, U1931112,
  11635011, 11761141001, Y811A35, 11675187, U1831208, U1931111) and in
  Thailand by RTA6280002 from Thailand Science Research and Innovation

---------------------------------------------------------
Title: Progress in Nuclear Astrophysics of East and Southeast Asia
Authors: Aziz, Azni Abdul; Sofiah Ahmad, Nor; Ahn, S.; Aoki, Wako;
   Bhuyan, Muruthujaya; Chen, Ke-Jung; Guo, Gang; Hahn, K. I.; Kajino,
   Toshitaka; Abu Kassim, Hasan; Kim, D.; Kubono, Shigeru; Kusakabe,
   Motohiko; Li, A.; Li, Haining; Li, Z. H.; Liu, W. P.; Liu, Z. W.;
   Motobayashi, Tohru; Pan, Kuo-Chuan; Park, T. -S.; Shi, Jian-Rong;
   Tang, Xiaodong; Wang, W.; Wen, Liangjian; Wu, Meng-Ru; Yan, Hong-Liang;
   Yusof, Norhasliza
2021AAPPS..31...18A    Altcode: 2021arXiv210803814A
  Nuclear astrophysics is an interdisciplinary research field of
  nuclear physics and astrophysics, seeking for the answer to a
  question, how to understand the evolution of the Universe with
  the nuclear processes which we learn. We review the research
  activities of nuclear astrophysics in east and southeast Asia which
  includes astronomy, experimental and theoretical nuclear physics and
  astrophysics. Several hot topics such as the Li problems, critical
  nuclear reactions and properties in stars, properties of dense matter,
  r-process nucleosynthesis and ν-process nucleosynthesis are chosen and
  discussed in further details. Some future Asian facilities, together
  with physics perspectives, are introduced.

---------------------------------------------------------
Title: Atmospheric Humic-Like Substances (HULIS) Act as Ice Active
    Entities
Authors: Chen, J.; Wu, Z. J.; Zhao, X.; Wang, Y. J.; Chen, J. C.;
   Qiu, Y. T.; Zong, T. M.; Chen, H. X.; Wang, B. B.; Lin, P.; Liu, W.;
   Guo, S.; Yao, M. S.; Zeng, L. M.; Wex, H.; Liu, X.; Hu, M.; Li, S. M.
2021GeoRL..4892443C    Altcode:
  We investigated the ice nucleation activities of humic-like substances
  (HULIS), an important component of organic aerosol (OA), derived
  from atmospheric and biomass burning aerosols, and produced from
  aqueous-phase chemical reactions. Respective HULIS can effectively
  trigger heterogeneous IN under mixed-phase cloud conditions. HULIS
  ice active entities (IAE) were aggregates in size between 0.02 and
  0.10 μm. At −20°C, the IAE numbers per unit HULIS mass varied
  from 213 to 8.7 × 10<SUP>4</SUP> mg<SUP>−1</SUP>. Such results
  were different than those detected in aquatic humic substances (HS)
  from previous studies, implying using HS as surrogates may not robustly
  estimate the IAE concentrations in the real atmosphere. Combining the
  abundance of atmospheric HULIS with the present results suggests that
  HULIS could be an important IAE contributor in the atmosphere where
  other ice nucleating particle species, such as dust and biological
  particles, are either low in concentration or absent.

---------------------------------------------------------
Title: High-efficient and high-accurate integrated division-of-time
    polarimeter
Authors: Liu, Wei; Liao, Jiawen; Yu, Yu; Zhang, Xinliang
2021APLP....6g1302L    Altcode:
  The characterization of the state of polarization is of great importance
  in broad applications, such as microscopy, communications, astronomy,
  and remote sensing. In this Letter, we propose and demonstrate a novel
  integrated division-of-time polarimeter (DOTP) based on a Mach-Zehnder
  interferometer and two photodetectors (PDs). The proposed DOTP achieves
  improved measuring efficiency and accuracy by measuring a pair of
  orthogonal polarization states simultaneously. The analysis matrix,
  which is used to recover the Stokes vector, is elaborately optimized to
  reduce the influence of the PD noise. Compared to the conventionally
  designed DOTP, the measuring efficiency is improved by 33% and the
  equally weighted variance, a figure of merit used to characterize
  the total variance of the Stokes vector, is also reduced by 33%. The
  performance of the proposed device is experimentally characterized by
  comparing with a commercial product. Furthermore, a method based on
  the least-squares method and singular value decomposition is adopted
  to quantize the deviation between the ideal optimal analysis matrix
  and the practical one.

---------------------------------------------------------
Title: Coeval Evolution of the Eastern Philippine Sea Plate and the
South China Sea in the Early Miocene: Paleomagnetic and Provenance
    Constraints From ODP Site 1177
Authors: Liu, Wei; Gai, Congcong; Feng, Wanyi; Cao, Wei; Guo, Laiyin;
   Zhong, Yi; Liu, Jiabo; Zhou, Yang; Chou, Yu-min; Lin, Jian; Liu,
   Qingsong
2021GeoRL..4893916L    Altcode:
  The Philippine Sea Plate (PSP) and the South China Sea (SCS), located
  at the intersection of the Eurasian, Pacific, and Indo-Australian
  plates, are key areas for global plate reconstruction. However, the
  relationships between the PSP and the SCS are still elusive. Here we
  report a new paleolatitude determination (16.0° ± 4.5°N at ∼20 Ma)
  from the Ocean Drilling Program Site 1177 in the Shikoku Basin (SB)
  within the eastern PSP. The new results indicate that the SB had a
  geographical affinity with the SCS in the early Miocene. Furthermore,
  the similarity in the U-Pb zircon age spectra of early Miocene
  turbidites from SB Site 1177 and SCS Site X28 implies that the two
  sites might receive similar materials in the early Miocene. Based
  on the new paleolatitude, provenance results, and other constraints,
  we suggest that the eastern PSP might be coupled dynamically to the
  SCS in the early Miocene.

---------------------------------------------------------
Title: Gamma-Ray Observation of the Cygnus Region in the 100-TeV
    Energy Region
Authors: Amenomori, M.; Bao, Y. W.; Bi, X. J.; Chen, D.; Chen, T. L.;
   Chen, W. Y.; Chen, Xu; Chen, Y.; Cirennima, Cui, S. W.; Danzengluobu,
   Ding, L. K.; Fang, J. H.; Fang, K.; Feng, C. F.; Feng, Zhaoyang;
   Feng, Z. Y.; Gao, Qi; Gomi, A.; Gou, Q. B.; Guo, Y. Q.; Guo, Y. Y.;
   He, H. H.; He, Z. T.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, H. B.;
   Huang, J.; Jia, H. Y.; Jiang, L.; Jiang, P.; Jin, H. B.; Kasahara, K.;
   Katayose, Y.; Kato, C.; Kato, S.; Kawata, K.; Kozai, M.; Kurashige,
   D.; Labaciren, Le, G. M.; Li, A. F.; Li, H. J.; Li, W. J.; Li, Y.; Lin,
   Y. H.; Liu, B.; Liu, C.; Liu, J. S.; Liu, L. Y.; Liu, M. Y.; Liu, W.;
   Liu, X. L.; Lou, Y. -Q.; Lu, H.; Meng, X. R.; Munakata, K.; Nakada,
   H.; Nakamura, Y.; Nakazawa, Y.; Nanjo, H.; Ning, C. C.; Nishizawa,
   M.; Ohnishi, M.; Ohura, T.; Okukawa, S.; Ozawa, S.; Qian, L.; Qian,
   X.; Qian, X. L.; Qu, X. B.; Saito, T.; Sakata, M.; Sako, T.; Sako,
   T. K.; Shao, J.; Shibata, M.; Shiomi, A.; Sugimoto, H.; Takano, W.;
   Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo,
   S.; Wang, H.; Wang, Y. P.; Wangdui, Wu, H. R.; Wu, Q.; Xu, J. L.; Xue,
   L.; Yamamoto, Y.; Yang, Z.; Yao, Y. Q.; Yin, J.; Yokoe, Y.; Yu, N. P.;
   Yuan, A. F.; Zhai, L. M.; Zhang, C. P.; Zhang, H. M.; Zhang, J. L.;
   Zhang, X.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhang, Ying; Zhao,
   S. P.; Zhaxisangzhu, Zhou, X. X.; Tibet AS<SUB>γ</SUB> Collaboration
2021PhRvL.127c1102A    Altcode: 2021arXiv210701064A
  We report observations of gamma-ray emissions with energies in the
  100-TeV energy region from the Cygnus region in our Galaxy. Two
  sources are significantly detected in the directions of the Cygnus
  OB1 and OB2 associations. Based on their positional coincidences,
  we associate one with a pulsar PSR J 2032 +4127 and the other mainly
  with a pulsar wind nebula PWN G 75.2 +0.1 , with the pulsar moving
  away from its original birthplace situated around the centroid of the
  observed gamma-ray emission. This work would stimulate further studies
  of particle acceleration mechanisms at these gamma-ray sources.

---------------------------------------------------------
Title: Quasi-periodic oscillations and long-term orbital period
    variation of the eclipsing dwarf nova EM Cyg
Authors: Liu, Wei; Qian, Sheng-Bang; Zhi, Qi-Jun; Han, Zhong-Tao;
   Wang, Qi-Shan; Dong, Ai-Jun
2021MNRAS.505..677L    Altcode: 2021MNRAS.tmp.1304L
  EM Cyg is an eclipsing dwarf nova with an orbital period above the
  period gap of cataclysmic variables. Based on the whole outburst of EM
  Cyg observed by the Transiting Exoplanet Survey Satellite (TESS) from
  2019 July 18-August 14, the evolution of quasi-periodic oscillations
  (QPOs) in EM Cyg was investigated. A QPO with a period of about 1000
  s was found during both outburst and quiescence. In addition, we found
  another QPO with a period of about 500 s, which was present during the
  outburst but disappeared as the outburst ended. QPOs should be caused
  by the activity of the accretion disc. Using the data obtained during
  the outburst, we analysed the characteristics of the light curves and
  found that the eclipsing depth increased and the light-minimum moment
  earlier during the outburst. In addition, with the new eclipse times
  obtained by TESS and from our observations, an O - C diagram for this
  system was produced. According to the O - C analysis, the orbital period
  is increasing at a rate of $\dot{P} = 1.66(\pm 0.36) \times 10^{-8}\,
  \mathrm{d\,yr^{-1}}$. There is a cyclic variation in the O - C curve
  that might be caused by the light-traveltime effect. A third body may
  exist in the EM Cyg system with the mass $m_3\sin {i{^{\prime }}} =
  0.097(\pm 0.000\,35) \, \mathrm{M}_{\odot }$.

---------------------------------------------------------
Title: Alpha-cluster transfer reactions: A tool for understanding
    stellar helium burning
Authors: Shen, Y. P.; Guo, B.; Liu, W. P.
2021PrPNP.11903857S    Altcode:
  Nuclear processes not only generate the energy and drive the
  evolution of stars, but also are responsible for the synthesis of
  the elements in the Universe. Helium (<SUP>4</SUP>He, or α) is the
  second most abundant element after hydrogen, thus α-particle induced
  reactions such as (α , γ) , (α , n) and (α , p) play a crucial
  role in nuclear astrophysics, especially for understanding stellar
  helium burning. Direct measurement of the cross sections for these
  α-capture reactions at stellar energies is greatly hindered because
  of the strong Coulomb repulsion. Alpha-cluster transfer reaction is
  a powerful tool for investigation of astrophysical (α , γ) , (α ,
  n) and (α , p) reactions since it can preferentially populate the
  natural-parity states with an α-cluster structure which dominantly
  contribute to these astrophysical α-capture reactions during stellar
  helium burning. In this review we summarize the theoretical scheme,
  the experimental technique, astrophysical applications and the future
  perspectives of such approach based on α-cluster transfer reactions.

---------------------------------------------------------
Title: Construction and on-site performance of the LHAASO WFCTA camera
Authors: Aharonian, F.; An, Q.; Axikegu, Bai, L. X.; Bai, Y. X.; Bao,
   Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao,
   Z.; Cao, Z.; Chang, J.; Chang, J. F.; Chang, X. C.; Chen, B. M.;
   Chen, J.; Chen, L.; Chen, L.; Chen, L.; Chen, M. J.; Chen, M. L.;
   Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen,
   Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Dai,
   B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu, Volpe, D. Della; Piazzoli,
   B. D'ettorre; Dong, X. J.; Fan, J. H.; Fan, Y. Z.; Fan, Z. X.; Fang,
   J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng, Y. L.; Gao,
   B.; Gao, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.;
   Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.;
   Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.;
   He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.; Hu, H. B.; Hu,
   S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.; Huang, W. H.;
   Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.;
   Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li,
   C.; Li, C.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.;
   Li, W. L.; Li, X.; Li, X.; Li, X. R.; Li, Y.; Li, Y. Z.; Li, Z.; Li,
   Z.; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.;
   Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.; Liu,
   M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y. N.; Liu, Z. X.; Long,
   W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao, J. R.;
   Masood, A.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.;
   Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Ruffolo, D.; Rulev, V.;
   Sáiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. R.; Song,
   H. C.; Stenkin, Yu. V.; Stepanov, V.; Sun, Q. N.; Sun, X. N.; Sun,
   Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang, B. D.; Wang,
   C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang, L. P.;
   Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang, X. G.; Wang,
   X. J.; Wang, X. Y.; Wang, Y. D.; Wang, Y. J.; Wang, Y. P.; Wang,
   Z.; Wang, Z.; Wang, Z. H.; Wang, Z. X.; Wei, D. M.; Wei, J. J.;
   Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.; Wu,
   X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, G.; Xiao,
   H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.; Xu, R. X.; Xue,
   L.; Yan, D. H.; Yang, C. W.; Yang, F. F.; Yang, J. Y.; Yang, L. L.;
   Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye,
   Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan,
   Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai,
   X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang,
   J. W.; Zhang, L.; Zhang, L.; Zhang, L. X.; Zhang, P. F.; Zhang, P. P.;
   Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.; Zhang,
   Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. L.; Zhao, B.; Zhao, J.; Zhao,
   L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, B.; Zhou,
   H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu,
   F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; Lhaaso Collaboration
2021EPJC...81..657A    Altcode: 2020arXiv201214622A
  The focal plane camera is the core component of the Wide
  Field-of-view Cherenkov/fluorescence Telescope Array (WFCTA) of
  the Large High-Altitude Air Shower Observatory (LHAASO). Because
  of the capability of working under moonlight without aging, silicon
  photomultipliers (SiPM) have been proven to be not only an alternative
  but also an improvement to conventional photomultiplier tubes (PMT) in
  this application. Eighteen SiPM-based cameras with square light funnels
  have been built for WFCTA. The telescopes have collected more than 100
  million cosmic ray events and preliminary results indicate that these
  cameras are capable of working under moonlight. The characteristics
  of the light funnels and SiPMs pose challenges (e.g. dynamic range,
  dark count rate, assembly techniques). In this paper, we present the
  design features, manufacturing techniques and performances of these
  cameras. Finally, the test facilities, the test methods and results
  of SiPMs in the cameras are reported here.

---------------------------------------------------------
Title: A scenario for the anisotropy of galactic cosmic rays related
    to nearby source and local interstellar magnetic field
Authors: Li, Ai-feng; Yuan, Qiang; Liu, Wei; Guo, Yi-qing
2021arXiv210700313L    Altcode:
  In our recent work, we build a propagation scenario to simultaneously
  explain the spectra and anisotropy of cosmic rays (CRs) by considering
  spatially dependent propagation (SDP) model and nearby Geminga
  supernova remnant (SNR) source. But the phase of anisotropy is still
  inconsistent with the experimental data. Recent observations of CR
  anisotropy show that the phase is consistent with local regular
  magnetic field (LRMF) observed by Interstellar Boundary Explorer
  (IBEX) below 100 TeV, which indicates that diffusion along LRMF is
  important. In this work, we further introduce the LRMF and take into
  account the effect of corresponding anisotropic diffusion to explain
  the anisotropy of CRs. We find that when the diffusion coefficient
  perpendicular to the LRMF is much smaller than the parallel one, the
  phase of anisotropy points to $\sim R.A.= 3^h$, which accords with
  experimental observation below 100 TeV. We also analyze the influence
  of the ratio of perpendicular and parallel diffusion coefficient on
  the anisotropy and the energy dependence of the ratio. The results
  illustrate that with the decrease of perpendicular diffusion, the
  anisotropic phase changes from the direction of nearby source to the
  LRMF below 100 TeV, meanwhile it changes from the galactic center (GC)
  to opposite direction of LRMF above 100 TeV. When the perpendicular
  diffusion coefficient grows faster than the parallel one with energy,
  the diffusion approaches to the isotropic at high energy, the phase
  of anisotropy shifts from the LRMF to the GC above 100 TeV. This could
  be helpful to ascertain the energy dependence of diffusion coefficients.

---------------------------------------------------------
Title: Peta-electron volt gamma-ray emission from the Crab Nebula
Authors: Lhaaso Collaboration; Cao, Zhen; Aharonian, F.; An, Q.;
   Axikegu; Bai, L. X.; Bai, Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.;
   Bi, Y. J.; Cai, H.; Cai, J. T.; Cao, Zhe; Chang, J.; Chang, J. F.;
   Chen, B. M.; Chen, E. S.; Chen, J.; Chen, Liang; Chen, Liang; Chen,
   Long; Chen, M. J.; Chen, M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.;
   Chen, T. L.; Chen, X. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui,
   S. W.; Cui, X. H.; Cui, Y. D.; D'Ettorre Piazzoli, B.; Dai, B. Z.;
   Dai, H. L.; Dai, Z. G.; Danzengluobu; Della Volpe, D.; Dong, X. J.;
   Duan, K. K.; Fan, J. H.; Fan, Y. Z.; Fan, Z. X.; Fang, J.; Fang,
   K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng, Y. L.; Gao, B.; Gao,
   C. D.; Gao, L. Q.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.; Gong,
   G. H.; Gou, Q. B.; Gu, M. H.; Guo, F. L.; Guo, J. G.; Guo, X. L.;
   Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.;
   He, S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou,
   X.; Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang,
   Q. L.; Huang, W. H.; Huang, X. T.; Huang, X. Y.; Huang, Z. C.; Ji,
   F.; Ji, X. L.; Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Ke, T.;
   Kuleshov, D.; Levochkin, K.; Li, B. B.; Li, Cheng; Li, Cong; Li, F.;
   Li, H. B.; Li, H. C.; Li, H. Y.; Li, Jian; Li, Jie; Li, K.; Li, W. L.;
   Li, X. R.; Li, Xin; Li, Xin; Li, Y.; Li, Y. Z.; Li, Zhe; Li, Zhuo;
   Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.;
   Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.;
   Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y.; Liu, Y. N.;
   Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma,
   X. H.; Mao, J. R.; Masood, A.; Min, Z.; Mitthumsiri, W.; Montaruli,
   T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi,
   M. Y.; Qi, Y. Q.; Qiao, B. Q.; Qin, J. J.; Ruffolo, D.; Rulev, V.;
   Saiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. Y.; Song,
   H. C.; Stenkin, Yu. V.; Stepanov, V.; Su, Y.; Sun, Q. N.; Sun, X. N.;
   Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang, B. D.;
   Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang,
   L. P.; Wang, L. Y.; Wang, R. N.; Wang, Wei; Wang, Wei; Wang, X. G.;
   Wang, X. J.; Wang, X. Y.; Wang, Y.; Wang, Y. D.; Wang, Y. J.; Wang,
   Y. P.; Wang, Z. H.; Wang, Z. X.; Wang, Zhen; Wang, Zheng; Wei, D. M.;
   Wei, J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu,
   W. X.; Wu, X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao,
   D. X.; Xiao, G.; Xiao, H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu,
   D. L.; Xu, R. X.; Xue, L.; Yan, D. H.; Yan, J. Z.; Yang, C. W.; Yang,
   F. F.; Yang, J. Y.; Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.;
   Yao, Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.;
   You, Z. Y.; Yu, Y. H.; Yuan, Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.;
   Zeng, Z. K.; Zha, M.; Zhai, X. X.; Zhang, B. B.; Zhang, H. M.; Zhang,
   H. Y.; Zhang, J. L.; Zhang, J. W.; Zhang, L. X.; Zhang, Li; Zhang,
   Lu; Zhang, P. F.; Zhang, P. P.; Zhang, R.; Zhang, S. R.; Zhang, S. S.;
   Zhang, X.; Zhang, X. P.; Zhang, Y. F.; Zhang, Y. L.; Zhang, Yi; Zhang,
   Yong; Zhao, B.; Zhao, J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng,
   F.; Zheng, Y.; Zhou, B.; Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.;
   Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.
2021Sci...373..425L    Altcode: 2021arXiv211106545T
  The Crab Nebula is a bright source of gamma rays powered by the Crab
  Pulsar's rotational energy through the formation and termination of
  a relativistic electron-positron wind. We report the detection of
  gamma rays from this source with energies from 5 × 10^{-4} to 1.1
  peta-electron volts with a spectrum showing gradual steepening over
  three energy decades. The ultrahigh-energy photons imply the presence
  of a peta-electron volt electron accelerator (a pevatron) in the
  nebula, with an acceleration rate exceeding 15% of the theoretical
  limit. We constrain the pevatron' size between 0.025 and 0.1 parsecs
  and the magnetic field to ≍110 microgauss. The production rate
  of peta-electron volt electrons, 2.5 × 10^{36} ergs per second,
  constitutes 0.5% of the pulsar spin-down luminosity, although we cannot
  exclude a contribution of peta-electron volt protons to the production
  of the highest-energy gamma rays.

---------------------------------------------------------
Title: Extended Very-High-Energy Gamma-Ray Emission Surrounding PSR
    J 0622 +3749 Observed by LHAASO-KM2A
Authors: Aharonian, F.; An, Q.; Axikegu, Bai, L. X.; Bai, Y. X.; Bao,
   Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao,
   Z.; Cao, Z.; Chang, J.; Chang, J. F.; Chang, X. C.; Chen, B. M.; Chen,
   J.; Chen, L.; Chen, L.; Chen, L.; Chen, M. J.; Chen, M. L.; Chen,
   Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen,
   Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.;
   Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; Della Volpe, D.;
   D'Ettorre Piazzoli, B.; Dong, X. J.; Fan, J. H.; Fan, Y. Z.; Fan,
   Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng,
   Y. L.; Gao, B.; Gao, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.;
   Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.; Guo,
   Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He,
   S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.;
   Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.;
   Huang, W. H.; Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia,
   H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.;
   Li, B. B.; Li, C.; Li, C.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.;
   Li, J.; Li, K.; Li, W. L.; Li, X.; Li, X.; Li, X. R.; Li, Y.; Li,
   Y. Z.; Li, Z.; Li, Z.; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu,
   B.; Liu, C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu,
   J. S.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu,
   Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma,
   L. L.; Ma, X. H.; Mao, J. R.; Masood, A.; Mitthumsiri, W.; Montaruli,
   T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi,
   M. Y.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.;
   Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.;
   Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian,
   W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang,
   J. S.; Wang, L. P.; Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang,
   X. G.; Wang, X. J.; Wang, X. Y.; Wang, Y. D.; Wang, Y. J.; Wang, Y. P.;
   Wang, Z.; Wang, Z.; Wang, Z. H.; Wang, Z. X.; Wei, D. M.; Wei, J. J.;
   Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.; Wu,
   X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, G.; Xiao,
   H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.; Xu, R. X.; Xue,
   L.; Yan, D. H.; Yang, C. W.; Yang, F. F.; Yang, J. Y.; Yang, L. L.;
   Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye,
   Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan,
   Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai,
   X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang,
   J. W.; Zhang, L.; Zhang, L.; Zhang, L. X.; Zhang, P. F.; Zhang, P. P.;
   Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.; Zhang,
   Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. L.; Zhao, B.; Zhao, J.; Zhao,
   L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, B.; Zhou,
   H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu,
   F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; LHAASO Collaboration; Huang, X. Y.
2021PhRvL.126x1103A    Altcode: 2021arXiv210609396L
  We report the discovery of an extended very-high-energy (VHE) gamma-ray
  source around the location of the middle-aged (207.8 kyr) pulsar
  PSR J 0622 +3749 with the Large High-Altitude Air Shower Observatory
  (LHAASO). The source is detected with a significance of 8.2 σ for
  E &gt;25 TeV assuming a Gaussian template. The best-fit location
  is (right ascension, declination) =(95.47 ° ±0.11 ° ,37.92 °
  ±0.09 ° ) , and the extension is 0.40 ° ±0.07 ° . The energy
  spectrum can be described by a power-law spectrum with an index of
  -2.92 ±0.17<SUB>stat</SUB>±0.02<SUB>sys</SUB> . No clear extended
  multiwavelength counterpart of the LHAASO source has been found from
  the radio to sub-TeV bands. The LHAASO observations are consistent
  with the scenario that VHE electrons escaped from the pulsar,
  diffused in the interstellar medium, and scattered the interstellar
  radiation field. If interpreted as the pulsar halo scenario, the
  diffusion coefficient, inferred for electrons with median energies
  of ∼160 TeV , is consistent with those obtained from the extended
  halos around Geminga and Monogem and much smaller than that derived
  from cosmic ray secondaries. The LHAASO discovery of this source thus
  likely enriches the class of so-called pulsar halos and confirms that
  high-energy particles generally diffuse very slowly in the disturbed
  medium around pulsars.

---------------------------------------------------------
Title: Large-scale EUV Waves and Their Implications for Global
    Coronal Seismology
Authors: Liu, W.; Jin, M.; Wang, T.; Ofman, L.; Sun, X.
2021AAS...23832817L    Altcode:
  Large-scale extreme ultraviolet (EUV) waves associated with coronal mass
  ejections (CMEs) and solar flares can provide novel diagnostics of the
  solar corona on global scales, an area yet to be fully exploited. We
  perform detailed analysis of various behaviors, such as reflection,
  refraction, and diffraction of several well-observed EUV waves,
  including those associated with the SOL2017-09-10 X8.2 flare and
  the SOL2011-02-15 X2 flare. We also performed data-constrained MHD
  simulations of these events using the University of Michigan Alfven Wave
  Solar Model (AWSoM). By comparing the observations and simulations,
  we benchmark diagnostics of the magnetic field strengths and thermal
  properties of the solar corona. This opens the door to the full
  applications to global coronal seismology using large-scale EUV waves.

---------------------------------------------------------
Title: Solar Prominence Bubbles and Associated Plasma Instabilities:
    IRIS and SDO/AIA Observations
Authors: Liu, W.; Berger, T.
2021AAS...23811311L    Altcode:
  Solar prominences are cool and dense plasma in the hot corona. The
  so-called prominence bubbles are mysterious, dome-shaped, apparently
  void structures residing in the lower portions of prominences. Such
  bubbles are associated with various plasma instabilities, such as the
  Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The
  former is manifested in plumes that are often produced at the top
  boundary of a bubble and intrude upward into the dense prominence
  material. The latter is found to be triggered by shear flows at
  the bubble boundaries. We present recent observations of prominence
  bubbles by IRIS and SDO/AIA, focusing on the diagnostic potential of
  RT and KH instabilities on the physical conditions of the prominence
  and its supporting magnetic field. We search for evidence of magnetic
  flux emergence as the origin of prominence bubbles. We discuss their
  role in mass ad magnetic flux transport in the solar atmosphere.

---------------------------------------------------------
Title: Applications of AOTF Spectrometers in In Situ Lunar
    Measurements
Authors: Li, Jinning; Gui, Yuhua; Xu, Rui; Zhang, Zehong; Liu, Wei;
   Lv, Gang; Wang, Meizhu; Li, Chunlai; He, Zhiping
2021Mate...14.3454L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Radio frequency interference detection based on the AC-UNet
    model
Authors: Yan, Rui-Qing; Dai, Cong; Liu, Wei; Li, Ji-Xia; Chen, Si-Ying;
   Yu, Xian-Chuan; Zuo, Shi-Fan; Chen, Xue-Lei
2021RAA....21..119Y    Altcode:
  Radio frequency interference (RFI) is a serious issue in radio
  astronomy. This paper proposes a U-Net network model with atrous
  convolution to detect RFI. Using the ability of convolutional
  neural networks to extract image features of RFI, and learning RFI
  distribution patterns, the detection model of the RFI is established. We
  use observational data containing real RFIs obtained by the Tianlai
  telescope to train the model so that the model can detect RFI. Calculate
  the probability of a data point being RFI pixel by pixel, and set
  a threshold. At the same time the dropout layer was added to avoid
  overfitting problems. If the predicted probability of a data point
  exceeds the threshold, it is considered that there is RFI, and if the
  predicted probability of a data point does not exceed the threshold,
  then it is considered that there is no RFI, so that the part of the
  image with RFI is flagged. Experimental results show that this approach
  can achieve satisfactory accuracy in the detection of radio observation
  images with a small amount of RFI.

---------------------------------------------------------
Title: Ultrahigh-energy photons up to 1.4 petaelectronvolts from 12
    γ-ray Galactic sources
Authors: Cao, Zhen; Aharonian, F. A.; An, Q.; Axikegu, Bai, L. X.;
   Bai, Y. X.; Bao, Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.;
   Cai, J. T.; Cao, Zhe; Chang, J.; Chang, J. F.; Chang, X. C.; Chen,
   B. M.; Chen, J.; Chen, L.; Chen, Liang; Chen, Long; Chen, M. J.;
   Chen, M. L.; Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen,
   X. L.; Chen, Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui,
   Y. D.; Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; della Volpe,
   D.; D'Ettorre Piazzoli, B.; Dong, X. J.; Fan, J. H.; Fan, Y. Z.;
   Fan, Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.;
   Feng, Y. L.; Gao, B.; Gao, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng,
   L. S.; Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.;
   Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.;
   He, S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou,
   X.; Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang,
   Q. L.; Huang, W. H.; Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.;
   Jia, H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin,
   K.; Li, B. B.; Li, Cong; Li, Cheng; Li, F.; Li, H. B.; Li, H. C.; Li,
   H. Y.; Li, J.; Li, K.; Li, W. L.; Li, X.; Li, Xin; Li, X. R.; Li, Y.;
   Li, Y. Z.; Li, Zhe; Li, Zhuo; Liang, E. W.; Liang, Y. F.; Lin, S. J.;
   Liu, B.; Liu, C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.;
   Liu, J. S.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.;
   Liu, Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma,
   L. L.; Ma, X. H.; Mao, J. R.; Masood, A.; Mitthumsiri, W.; Montaruli,
   T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi,
   M. Y.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.;
   Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.;
   Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian,
   W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.;
   Wang, J. S.; Wang, L. P.; Wang, L. Y.; Wang, R. N.; Wang, W.; Wang,
   W.; Wang, X. G.; Wang, X. J.; Wang, X. Y.; Wang, Y. D.; Wang, Y. J.;
   Wang, Y. P.; Wang, Zheng; Wang, Zhen; Wang, Z. H.; Wang, Z. X.; Wei,
   D. M.; Wei, J. J.; Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.;
   Wu, W. X.; Wu, X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.;
   Xiao, G.; Xiao, H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.;
   Xu, R. X.; Xue, L.; Yan, D. H.; Yang, C. W.; Yang, F. F.; Yang, J. Y.;
   Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao,
   Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu,
   Y. H.; Yuan, Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.;
   Zha, M.; Zhai, X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang,
   J. L.; Zhang, J. W.; Zhang, L.; Zhang, Li; Zhang, L. X.; Zhang, P. F.;
   Zhang, P. P.; Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang,
   X. P.; Zhang, Yong; Zhang, Yi; Zhang, Y. F.; Zhang, Y. L.; Zhao, B.;
   Zhao, J.; Zhao, L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.;
   Zhou, B.; Zhou, H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.;
   Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.
2021Natur.594...33C    Altcode:
  The extension of the cosmic-ray spectrum beyond 1 petaelectronvolt
  (PeV; 10<SUP>15</SUP> electronvolts) indicates the existence of the
  so-called PeVatrons—cosmic-ray factories that accelerate particles
  to PeV energies. We need to locate and identify such objects to
  find the origin of Galactic cosmic rays<SUP>1</SUP>. The principal
  signature of both electron and proton PeVatrons is ultrahigh-energy
  (exceeding 100 TeV) γ radiation. Evidence of the presence of a
  proton PeVatron has been found in the Galactic Centre, according
  to the detection of a hard-spectrum radiation extending to 0.04 PeV
  (ref. <SUP>2</SUP>). Although γ-rays with energies slightly higher
  than 0.1 PeV have been reported from a few objects in the Galactic
  plane<SUP>3-6</SUP>, unbiased identification and in-depth exploration
  of PeVatrons requires detection of γ-rays with energies well above 0.1
  PeV. Here we report the detection of more than 530 photons at energies
  above 100 teraelectronvolts and up to 1.4 PeV from 12 ultrahigh-energy
  γ-ray sources with a statistical significance greater than seven
  standard deviations. Despite having several potential counterparts in
  their proximity, including pulsar wind nebulae, supernova remnants and
  star-forming regions, the PeVatrons responsible for the ultrahigh-energy
  γ-rays have not yet been firmly localized and identified (except for
  the Crab Nebula), leaving open the origin of these extreme accelerators.

---------------------------------------------------------
Title: Possible bump structure of cosmic ray electrons unveiled by
    AMS-02 data and its common origin along with the nuclei and positron
Authors: Zhang, Pei-pei; Qiao, Bing-qiang; Liu, Wei; Cui, Shu-wang;
   Yuan, Qiang; Guo, Yi-qing
2021JCAP...05..012Z    Altcode: 2021arXiv210100189Z
  The local pulsar and its progenitor, SNR, can together accelerate the
  positron, electron and nuclei to very high energy. The famous excesses
  of positron(nuclei) above 20(200) GeV possibly come from such kind of
  local source. This hints that the primary electron should also hold
  "excess" above 200 GeV, synchronously accelerated along with the
  nuclei. The recent precise measurement of sharp dropoff at 284 GeV
  of positron by AMS-02 experiment takes chance to study this expected
  electron excess. In this work, the spatially-dependent propagation
  with a local source is used to reproduce the spectrum of positron,
  electron and proton. When considering the dropoff at 284 GeV of
  positron, a sharp bump structure for primary electron above 284 GeV is
  required to fit the total spectrum of positron and electron. Then we
  systematically study the common origin of the excesses of positron,
  electron and nuclei from Geminga pulsar and SNR. Those excesses can
  be reproduced under this unified single-source model. Lastly, we hope
  that the fine bump structure can be observed to support our model by
  AMS-02 experiment in future.

---------------------------------------------------------
Title: Oceanic Pathways of an Active Pacific Meridional Overturning
    Circulation (PMOC)
Authors: Thomas, M. D.; Fedorov, A. V.; Burls, N. J.; Liu, W.
2021GeoRL..4891935T    Altcode:
  In contrast to the modern day climate, North Pacific deep water
  formation and a Pacific meridional overturning circulation (PMOC)
  may have been active during past climate conditions, in particular
  during the Pliocene epoch (some 3-5 million years ago). Here, we use
  a climate model simulation with a robust PMOC cell to investigate
  the pathways of the North Pacific deep water from subduction to
  upwelling, as revealed by Lagrangian particle trajectories. We find
  that similar to the present day Atlantic Meridional Overturning
  Circulation (AMOC), most subducted North Pacific deep water upwells
  in the Southern Ocean. However, roughly 15% upwells in the tropical
  Indo Pacific Oceans instead—a key feature distinguishing the PMOC
  from the AMOC. The connection to the Indian Ocean is relatively fast,
  at about 250 years. The connection to the tropical Pacific is slower
  (∼800 years) as water first travels to the subtropical South Pacific
  then gradually upwells through the thermocline.

---------------------------------------------------------
Title: A New View of the Solar Interface Region from the Interface
    Region Imaging Spectrograph (IRIS)
Authors: De Pontieu, Bart; Polito, Vanessa; Hansteen, Viggo; Testa,
   Paola; Reeves, Katharine K.; Antolin, Patrick; Nóbrega-Siverio,
   Daniel Elias; Kowalski, Adam F.; Martinez-Sykora, Juan; Carlsson,
   Mats; McIntosh, Scott W.; Liu, Wei; Daw, Adrian; Kankelborg, Charles C.
2021SoPh..296...84D    Altcode: 2021arXiv210316109D
  The Interface Region Imaging Spectrograph (IRIS) has been obtaining
  near- and far-ultraviolet images and spectra of the solar atmosphere
  since July 2013. IRIS is the highest resolution observatory to provide
  seamless coverage of spectra and images from the photosphere into the
  low corona. The unique combination of near- and far-ultraviolet spectra
  and images at sub-arcsecond resolution and high cadence allows the
  tracing of mass and energy through the critical interface between the
  surface and the corona or solar wind. IRIS has enabled research into the
  fundamental physical processes thought to play a role in the low solar
  atmosphere such as ion-neutral interactions, magnetic reconnection, the
  generation, propagation, and dissipation of waves, the acceleration of
  non-thermal particles, and various small-scale instabilities. IRIS has
  provided insights into a wide range of phenomena including the discovery
  of non-thermal particles in coronal nano-flares, the formation and
  impact of spicules and other jets, resonant absorption and dissipation
  of Alfvénic waves, energy release and jet-like dynamics associated
  with braiding of magnetic-field lines, the role of turbulence and the
  tearing-mode instability in reconnection, the contribution of waves,
  turbulence, and non-thermal particles in the energy deposition during
  flares and smaller-scale events such as UV bursts, and the role of flux
  ropes and various other mechanisms in triggering and driving CMEs. IRIS
  observations have also been used to elucidate the physical mechanisms
  driving the solar irradiance that impacts Earth's upper atmosphere,
  and the connections between solar and stellar physics. Advances in
  numerical modeling, inversion codes, and machine-learning techniques
  have played a key role. With the advent of exciting new instrumentation
  both on the ground, e.g. the Daniel K. Inouye Solar Telescope (DKIST)
  and the Atacama Large Millimeter/submillimeter Array (ALMA), and
  space-based, e.g. the Parker Solar Probe and the Solar Orbiter, we aim
  to review new insights based on IRIS observations or related modeling,
  and highlight some of the outstanding challenges.

---------------------------------------------------------
Title: Measurement of the Cosmic Ray Helium Energy Spectrum from 70
    GeV to 80 TeV with the DAMPE Space Mission
Authors: Alemanno, F.; An, Q.; Azzarello, P.; Barbato, F. C. T.;
   Bernardini, P.; Bi, X. J.; Cai, M. S.; Catanzani, E.; Chang, J.;
   Chen, D. Y.; Chen, J. L.; Chen, Z. F.; Cui, M. Y.; Cui, T. S.; Cui,
   Y. X.; Dai, H. T.; D'Amone, A.; de Benedittis, A.; de Mitri, I.;
   de Palma, F.; Deliyergiyev, M.; di Santo, M.; Dong, T. K.; Dong,
   Z. X.; Donvito, G.; Droz, D.; Duan, J. L.; Duan, K. K.; D'Urso, D.;
   Fan, R. R.; Fan, Y. Z.; Fang, K.; Fang, F.; Feng, C. Q.; Feng, L.;
   Fusco, P.; Gao, M.; Gargano, F.; Gong, K.; Gong, Y. Z.; Guo, D. Y.;
   Guo, J. H.; Guo, X. L.; Han, S. X.; Hu, Y. M.; Huang, G. S.; Huang,
   X. Y.; Huang, Y. Y.; Ionica, M.; Jiang, W.; Kong, J.; Kotenko, A.;
   Kyratzis, D.; Lei, S. J.; Li, S.; Li, W. L.; Li, X.; Li, X. Q.;
   Liang, Y. M.; Liu, C. M.; Liu, H.; Liu, J.; Liu, S. B.; Liu, W. Q.;
   Liu, Y.; Loparco, F.; Luo, C. N.; Ma, M.; Ma, P. X.; Ma, T.; Ma,
   X. Y.; Marsella, G.; Mazziotta, M. N.; Mo, D.; Niu, X. Y.; Pan, X.;
   Parenti, A.; Peng, W. X.; Peng, X. Y.; Perrina, C.; Qiao, R.; Rao,
   J. N.; Ruina, A.; Salinas, M. M.; Shang, G. Z.; Shen, W. H.; Shen,
   Z. Q.; Shen, Z. T.; Silveri, L.; Song, J. X.; Stolpovskiy, M.; Su,
   H.; Su, M.; Sun, Z. Y.; Surdo, A.; Teng, X. J.; Tykhonov, A.; Wang,
   H.; Wang, J. Z.; Wang, L. G.; Wang, S.; Wang, X. L.; Wang, Y.; Wang,
   Y. F.; Wang, Y. Z.; Wang, Z. M.; Wei, D. M.; Wei, J. J.; Wei, Y. F.;
   Wen, S. C.; Wu, D.; Wu, J.; Wu, L. B.; Wu, S. S.; Wu, X.; Xia, Z. Q.;
   Xu, H. T.; Xu, Z. H.; Xu, Z. L.; Xu, Z. Z.; Xue, G. F.; Yang, H. B.;
   Yang, P.; Yang, Y. Q.; Yao, H. J.; Yu, Y. H.; Yuan, G. W.; Yuan, Q.;
   Yue, C.; Zang, J. J.; Zhang, F.; Zhang, S. X.; Zhang, W. Z.; Zhang,
   Y.; Zhang, Y. J.; Zhang, Y. L.; Zhang, Y. P.; Zhang, Y. Q.; Zhang,
   Z.; Zhang, Z. Y.; Zhao, C.; Zhao, H. Y.; Zhao, X. F.; Zhou, C. Y.;
   Zhu, Y.; Dampe Collaboration
2021PhRvL.126t1102A    Altcode: 2021arXiv210509073A
  The measurement of the energy spectrum of cosmic ray helium nuclei
  from 70 GeV to 80 TeV using 4.5 years of data recorded by the Dark
  Matter Particle Explorer (DAMPE) is reported in this work. A hardening
  of the spectrum is observed at an energy of about 1.3 TeV, similar
  to previous observations. In addition, a spectral softening at about
  34 TeV is revealed for the first time with large statistics and well
  controlled systematic uncertainties, with an overall significance of
  4.3 σ . The DAMPE spectral measurements of both cosmic protons and
  helium nuclei suggest a particle charge dependent softening energy,
  although with current uncertainties a dependence on the number of
  nucleons cannot be ruled out.

---------------------------------------------------------
Title: Novel fluorescent probe based on dicoumarin for rapid on-site
    detection of Hg<SUP>2+</SUP> in loess
Authors: Jiang, Youhong; Li, Huiwen; Chen, Ruofei; Liu, Wei; Chen,
   Chunyang; Li, Zhongguo; Liu, Weisheng
2021AcSpA.25119438J    Altcode:
  It is momentous to exploit rapid, specific and on-site detection
  methods for mercury ion (Hg<SUP>2+</SUP>) in loess, as the severe
  toxicity of Hg<SUP>2+</SUP> and the fragile ecological environment
  of Loess Plateau. In this paper, a novel fluorescent probe DC-Hg
  (Dicoumarin-Hg) was synthesized by 3-hydroxybiscoumarin and phenyl
  thiochloroformate at room temperature. DC-Hg could exclusively
  combine with Hg<SUP>2+</SUP> to 'turn-on' yellow fluorescence at
  530 nm among various other metal ions. The relationship between the
  remarkable increase in intensity and concentration of Hg<SUP>2+</SUP>
  was associated with photoinduced electron transfer (PET), which was
  founded by Job's plot and <SUP>1</SUP>H NMR. The limit detection of
  DC-Hg showed to 85.25 nM in aqueous medium, which could be applied to
  varying situations. For the loess samples, they were only extracted by
  hand-shake and filtration for quickly complete the treatment operation
  on site, and the results proved that DC-Hg could satisfactorily detect
  the Hg<SUP>2+</SUP> in mercury pollution areas.

---------------------------------------------------------
Title: Geometrical reconstruction of fluorescence events observed
    by the LHAASO experiment
Authors: Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai, Y. X.; Bao,
   Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao,
   Z.; Cao, Z.; Chang, J.; Chang, J. F.; Chang, X. C.; Chen, B. M.; Chen,
   J.; Chen, L.; Chen, L.; Chen, L.; Chen, M. J.; Chen, M. L.; Chen,
   Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen,
   Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.;
   Dai, B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; Della Volpe, D.;
   D'Ettorre Piazzoli, B.; Dong, X. J.; Fan, J. H.; Fan, Y. Z.; Fan,
   Z. X.; Fang, J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng,
   Y. L.; Gao, B.; Gao, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.;
   Gong, G. H.; Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.; Guo,
   Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He,
   S. L.; He, X. B.; He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.;
   Hu, H. B.; Hu, S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.;
   Huang, W. H.; Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia,
   H. Y.; Jiang, K.; Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.;
   Li, B. B.; Li, C.; Li, C.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li,
   J.; Li, K.; Li, W. L.; Li, X.; Li, X.; Li, X. R.; Li, Y.; Li, Y. Z.;
   Li, Z.; Li, Z.; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu,
   C.; Liu, D.; Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. L.;
   Liu, J. S.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.;
   Liu, Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma,
   L. L.; Ma, X. H.; Mao, J. R.; Masood, A.; Mitthumsiri, W.; Montaruli,
   T.; Nan, Y. C.; Pang, B. Y.; Pattarakijwanich, P.; Pei, Z. Y.; Qi,
   M. Y.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.;
   Sheng, X. D.; Shi, J. R.; Song, H. C.; Stenkin, Yu. V.; Stepanov, V.;
   Sun, Q. N.; Sun, X. N.; Sun, Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian,
   W. W.; Wang, B. D.; Wang, C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang,
   J. S.; Wang, L. P.; Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang,
   X. G.; Wang, X. J.; Wang, X. Y.; Wang, Y. D.; Wang, Y. J.; Wang, Y. P.;
   Wang, Z.; Wang, Z.; Wang, Z. H.; Wang, Z. X.; Wei, D. M.; Wei, J. J.;
   Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.; Wu,
   X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, G.; Xiao,
   H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.; Xu, R. X.; Xue,
   L.; Yan, D. H.; Yang, C. W.; Yang, F. F.; Yang, J. Y.; Yang, L. L.;
   Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye,
   Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan,
   Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai,
   X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang,
   J. W.; Zhang, L.; Zhang, L.; Zhang, L. X.; Zhang, P. F.; Zhang, P. P.;
   Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.; Zhang,
   Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. L.; Zhao, B.; Zhao, J.; Zhao,
   L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, B.; Zhou,
   H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu,
   F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; LHAASO Collaboration
2021ChPhC..45d5101A    Altcode:
  The LHAASO-WFCTA experiment, which aims to observe cosmic rays in the
  sub-EeV range using the fluorescence technique, uses a new generation
  of high-performance telescopes. To ensure that the experiment has
  excellent detection capability associated with the measurement of
  the energy spectrum, the primary composition of cosmic rays, and
  so on, an accurate geometrical reconstruction of air-shower events
  is fundamental. This paper describes the development and testing
  of geometrical reconstruction for stereo viewed events using the
  WFCTA (Wide Field of view Cherenkov/Fluorescence Telescope Array)
  detectors. Two approaches, which take full advantage of the WFCTA
  detectors, are investigated. One is the stereo-angular method,
  which uses the pointing of triggered SiPMs in the shower trajectory,
  and the other is the stereo-timing method, which uses the triggering
  time of the fired SiPMs. The results show that both methods have good
  geometrical resolution; the resolution of the stereo-timing method is
  slightly better than the stereo-angular method because the resolution
  of the latter is slightly limited by the shower track length. *
  Supported by National Natural Science Foundation of China (11903005,
  11563004, 11475190)

---------------------------------------------------------
Title: IRIS observations of chromospheric heating by acoustic waves
    in solar quiet and active regions
Authors: Abbasvand, V.; Sobotka, M.; Švanda, M.; Heinzel, P.; Liu,
   W.; Mravcová, L.
2021A&A...648A..28A    Altcode: 2021arXiv210208678A
  <BR /> Aims: To study the heating of solar chromospheric magnetic and
  nonmagnetic regions by acoustic and magnetoacoustic waves, the deposited
  acoustic-energy flux derived from observations of strong chromospheric
  lines is compared with the total integrated radiative losses. <BR />
  Methods: A set of 23 quiet-Sun and weak-plage regions were observed in
  the Mg II k and h lines with the Interface Region Imaging Spectrograph
  (IRIS). The deposited acoustic-energy flux was derived from Doppler
  velocities observed at two different geometrical heights corresponding
  to the middle and upper chromosphere. A set of scaled nonlocal
  thermodynamic equilibrium 1D hydrostatic semi-empirical models -
  obtained by fitting synthetic to observed line profiles - was applied
  to compute the radiative losses. The characteristics of observed waves
  were studied by means of a wavelet analysis. <BR /> Results: Observed
  waves propagate upward at supersonic speed. In the quiet chromosphere,
  the deposited acoustic flux is sufficient to balance the radiative
  losses and maintain the semi-empirical temperatures in the layers under
  study. In the active-region chromosphere, the comparison shows that
  the contribution of acoustic-energy flux to the radiative losses is
  only 10−30%. <BR /> Conclusions: Acoustic and magnetoacoustic waves
  play an important role in the chromospheric heating, depositing a main
  part of their energy in the chromosphere. Acoustic waves compensate
  for a substantial fraction of the chromospheric radiative losses in
  quiet regions. In active regions, their contribution is too small to
  balance the radiative losses and the chromosphere has to be heated by
  other mechanisms.

---------------------------------------------------------
Title: Pedogenic processes in loess-paleosol sediments: Clues from
    Li isotopes of leachate in Luochuan loess
Authors: He, Mao-Yong; Dong, Ji-Bao; Jin, Zhangdong; Liu, Chun-Yao;
   Xiao, Jun; Zhang, Fei; Sun, He; Zhao, Zhi-Qi; Gou, Long-Fei; Liu,
   Wei-Guo; Luo, Chong-Guang; Song, You-Gui; Ma, Long; Deng, Li
2021GeCoA.299..151H    Altcode:
  Tracing pedogenic processes is fundamental for reconstructing
  climatic and environmental changes using loess deposits. Lithium
  isotopes can serve as a sensitive tracer to unravel these processes,
  owing to its active behaviors without effect by redox and biological
  reactions. This study investigated the Li contents and δ<SUP>7</SUP>Li
  values of leachate and residue ([Li]<SUB>leachate</SUB>,
  [Li]<SUB>residue</SUB>, δ<SUP>7</SUP>Li<SUB>leachate</SUB> and
  δ<SUP>7</SUP>Li<SUB>residue</SUB>) of the upper 12.5 m Luochuan
  loess-paleosol sediment (since the last interglacial) on the Chinese
  Loess Plateau, in order to better understand pedogenic processes in
  loess. The [Li]<SUB>leachate</SUB>, varying from 0.39 to 1.97 μg/g, is
  mainly derived from the adsorption phase, with a significant variation
  in δ<SUP>7</SUP>Li<SUB>leachate</SUB>, from -6.55‰ to +12.88‰. Both
  [Li]<SUB>leachate</SUB> and δ<SUP>7</SUP>Li<SUB>leachate</SUB>
  variations reflect weathering and adsorption processes during different
  periods. The [Li]<SUB>residue</SUB> vary from 34.4 to 46.3 μg/g
  (averaging 38.4 μg/g) and their δ<SUP>7</SUP>Li<SUB>residue</SUB>
  vary from -3.66‰ to +2.44‰ (averaging -0.22 ± 1.68‰), both
  in agreement with the upper continental crust values. At initial
  stage after loess deposited (stage I), high [Li]<SUB>leachate</SUB>
  but low δ<SUP>7</SUP>Li<SUB>leachate</SUB> are results of
  preferential adsorption of <SUP>6</SUP>Li by clays and migration
  of <SUP>7</SUP>Li with soil solution during weathering and
  eluviation processes. When overlying loess was deposited and
  experienced pedogenesis as the stage I, <SUP>7</SUP>Li migrated
  downward and was adsorbed by clays (stage II), resulting in high
  [Li]<SUB>leachate</SUB> and δ<SUP>7</SUP>Li<SUB>leachate</SUB> in
  underlying loess. When loess has superimposed pedogenic and adsorption
  processes as the stages I and II, loess became as paleosol with highest
  δ<SUP>7</SUP>Li<SUB>leachate</SUB> in underlying carbonate accumulation
  layer. A persistent increase in δ<SUP>7</SUP>Li<SUB>leachate</SUB>
  indicates dominant control of post-depositional adsorptions on
  Li fractionation along solution migrations during weathering
  and eluviation of overlying deposits, and vice versa. These
  results highlight that variations in [Li]<SUB>leachate</SUB> and
  δ<SUP>7</SUP>Li<SUB>leachate</SUB> can be used to trace soil water
  migration processes and the magnitude of pedogenic processes in
  loess-paleosol sediment at different periods.

---------------------------------------------------------
Title: Critical Science Plan for the Daniel K. Inouye Solar Telescope
    (DKIST)
Authors: Rast, Mark P.; Bello González, Nazaret; Bellot Rubio,
   Luis; Cao, Wenda; Cauzzi, Gianna; Deluca, Edward; de Pontieu, Bart;
   Fletcher, Lyndsay; Gibson, Sarah E.; Judge, Philip G.; Katsukawa,
   Yukio; Kazachenko, Maria D.; Khomenko, Elena; Landi, Enrico; Martínez
   Pillet, Valentín; Petrie, Gordon J. D.; Qiu, Jiong; Rachmeler,
   Laurel A.; Rempel, Matthias; Schmidt, Wolfgang; Scullion, Eamon; Sun,
   Xudong; Welsch, Brian T.; Andretta, Vincenzo; Antolin, Patrick; Ayres,
   Thomas R.; Balasubramaniam, K. S.; Ballai, Istvan; Berger, Thomas E.;
   Bradshaw, Stephen J.; Campbell, Ryan J.; Carlsson, Mats; Casini,
   Roberto; Centeno, Rebecca; Cranmer, Steven R.; Criscuoli, Serena;
   Deforest, Craig; Deng, Yuanyong; Erdélyi, Robertus; Fedun, Viktor;
   Fischer, Catherine E.; González Manrique, Sergio J.; Hahn, Michael;
   Harra, Louise; Henriques, Vasco M. J.; Hurlburt, Neal E.; Jaeggli,
   Sarah; Jafarzadeh, Shahin; Jain, Rekha; Jefferies, Stuart M.; Keys,
   Peter H.; Kowalski, Adam F.; Kuckein, Christoph; Kuhn, Jeffrey R.;
   Kuridze, David; Liu, Jiajia; Liu, Wei; Longcope, Dana; Mathioudakis,
   Mihalis; McAteer, R. T. James; McIntosh, Scott W.; McKenzie, David
   E.; Miralles, Mari Paz; Morton, Richard J.; Muglach, Karin; Nelson,
   Chris J.; Panesar, Navdeep K.; Parenti, Susanna; Parnell, Clare E.;
   Poduval, Bala; Reardon, Kevin P.; Reep, Jeffrey W.; Schad, Thomas A.;
   Schmit, Donald; Sharma, Rahul; Socas-Navarro, Hector; Srivastava,
   Abhishek K.; Sterling, Alphonse C.; Suematsu, Yoshinori; Tarr, Lucas
   A.; Tiwari, Sanjiv; Tritschler, Alexandra; Verth, Gary; Vourlidas,
   Angelos; Wang, Haimin; Wang, Yi-Ming; NSO and DKIST Project; DKIST
   Instrument Scientists; DKIST Science Working Group; DKIST Critical
   Science Plan Community
2021SoPh..296...70R    Altcode: 2020arXiv200808203R
  The National Science Foundation's Daniel K. Inouye Solar Telescope
  (DKIST) will revolutionize our ability to measure, understand,
  and model the basic physical processes that control the structure
  and dynamics of the Sun and its atmosphere. The first-light DKIST
  images, released publicly on 29 January 2020, only hint at the
  extraordinary capabilities that will accompany full commissioning of
  the five facility instruments. With this Critical Science Plan (CSP)
  we attempt to anticipate some of what those capabilities will enable,
  providing a snapshot of some of the scientific pursuits that the DKIST
  hopes to engage as start-of-operations nears. The work builds on the
  combined contributions of the DKIST Science Working Group (SWG) and
  CSP Community members, who generously shared their experiences, plans,
  knowledge, and dreams. Discussion is primarily focused on those issues
  to which DKIST will uniquely contribute.

---------------------------------------------------------
Title: First Detection of sub-PeV Diffuse Gamma Rays from the Galactic
Disk: Evidence for Ubiquitous Galactic Cosmic Rays beyond PeV Energies
Authors: Amenomori, M.; Bao, Y. W.; Bi, X. J.; Chen, D.; Chen,
   T. L.; Chen, W. Y.; Chen, Xu; Chen, Y.; Cirennima, Cui, S. W.;
   Danzengluobu, Ding, L. K.; Fang, J. H.; Fang, K.; Feng, C. F.;
   Feng, Zhaoyang; Feng, Z. Y.; Gao, Qi; Gou, Q. B.; Guo, Y. Q.; Guo,
   Y. Y.; He, H. H.; He, Z. T.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu,
   H. B.; Huang, J.; Jia, H. Y.; Jiang, L.; Jin, H. B.; Kasahara, K.;
   Katayose, Y.; Kato, C.; Kato, S.; Kawata, K.; Kihara, W.; Ko, Y.;
   Kozai, M.; Labaciren, Le, G. M.; Li, A. F.; Li, H. J.; Li, W. J.;
   Lin, Y. H.; Liu, B.; Liu, C.; Liu, J. S.; Liu, M. Y.; Liu, W.; Lou,
   Y. -Q.; Lu, H.; Meng, X. R.; Munakata, K.; Nakada, H.; Nakamura, Y.;
   Nanjo, H.; Nishizawa, M.; Ohnishi, M.; Ohura, T.; Ozawa, S.; Qian,
   X. L.; Qu, X. B.; Saito, T.; Sakata, M.; Sako, T. K.; Shao, J.;
   Shibata, M.; Shiomi, A.; Sugimoto, H.; Takano, W.; Takita, M.; Tan,
   Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo, S.; Wang, H.; Wu,
   H. R.; Xue, L.; Yamamoto, Y.; Yang, Z.; Yokoe, Y.; Yuan, A. F.; Zhai,
   L. M.; Zhang, H. M.; Zhang, J. L.; Zhang, X.; Zhang, X. Y.; Zhang,
   Y.; Zhang, Yi; Zhang, Ying; Zhao, S. P.; Zhaxisangzhu, Zhou, X. X.;
   Tibet AS<SUB>γ</SUB> Collaboration
2021PhRvL.126n1101A    Altcode: 2021arXiv210405181A
  We report, for the first time, the long-awaited detection of diffuse
  gamma rays with energies between 100 TeV and 1 PeV in the Galactic
  disk. Particularly, all gamma rays above 398 TeV are observed apart
  from known TeV gamma-ray sources and compatible with expectations from
  the hadronic emission scenario in which gamma rays originate from the
  decay of π<SUP>0</SUP>'s produced through the interaction of protons
  with the interstellar medium in the Galaxy. This is strong evidence
  that cosmic rays are accelerated beyond PeV energies in our Galaxy
  and spread over the Galactic disk.

---------------------------------------------------------
Title: On the Progenitors of AM CVn Stars as LISA Sources: The
    Evolved Donor Star Channel
Authors: Liu, Wei-Min; Jiang, Long; Chen, Wen-Cong
2021ApJ...910...22L    Altcode: 2021arXiv210109850L
  The space gravitational wave (GW) detector Laser Interferometer Space
  Antenna (LISA) that is planned to be launched in the early 2030s will
  detect the low-frequency GW signals in the Galaxy. AM CVn stars were
  generally thought to be important low-frequency GW sources. Employing
  the MESA code, in this work we calculate the evolution of a great number
  of binary systems consisting of a white dwarf (WD) and a main sequence
  (MS) star, and diagnose whether their descendant-AM CVn stars will be
  visible with LISA. The simulated results show that the progenitors of
  these LISA sources, within a distance of 1 kpc, are WD-MS binaries
  with a donor star of 1.0-1.4 M<SUB>⊙</SUB> (for initial WD mass
  of 0.5 M<SUB>⊙</SUB>) or 1.0-2.0 M<SUB>⊙</SUB> (for initial WD
  mass of 0.7 M<SUB>⊙</SUB>), and an initial orbital period slightly
  smaller than the bifurcation period. Our simulations also indicate
  that 10 verification AM CVn sources can be reproduced by the standard
  magnetic braking model, and are potential LISA sources. Based on the
  birth rate of AM CVn stars simulated by the population synthesis, the
  birth rate of AM CVn-LISA sources evolving from the evolved donor star
  channel within a distance of 1 kpc can be estimated to be (0.6-1.4) ×
  10<SUP>-6</SUP> yr<SUP>-1</SUP>, and the predicted number of AM CVn-LISA
  sources is about 340-810. Therefore, the evolved donor star channel
  plays an important role in forming AM CVn-LISA sources in the Galaxy.

---------------------------------------------------------
Title: The readout system design of 320x256 InGaAs astronomical camera
Authors: Liu, Wei; Men, Jinrui; Lou, Zheng
2021SPIE11763E..0ML    Altcode:
  InGaAs detector can be used as the image sensor in SWIR (Shortwave
  Infrared) band as. Cameras with InGaAs detector have been widely used
  in the astronomical observation field. Based on the optical band CCD
  camera readout technologies that we have mastered, this paper introduced
  one China domestic InGaAs detector, and proposed this camera readout
  system with it, which includes the whole circuits structure, pixel
  transferring timing and image acquisition method. We summarized these
  technologies, presented the appropriate solutions and the simulation
  results as well. These works provide technical support to develop
  infrared scientific camera

---------------------------------------------------------
Title: AA Tau polarimetric observation using Kanata HONIR instrument
Authors: Liu, Wei; Kawabata, Koji S.; Akitaya, Hiroshi
2021SPIE11763E..0KL    Altcode:
  Astronomical polarimetric observation is one of the important methods in
  modern astrophysics research field. In the infrared bands, polarimetric
  observation is one effective tool to study the evolution and formation
  of star, and reveal multiband radiation characteristics of high-energy
  celestial bodies and other aspects. This paper will introduce the system
  composition, operating principle, calibration and data analysis method
  of polarimetric observation using HONIR camera on Kanata telescope. We
  also present part of the analysis results of AA Tau with polarimetric
  observation, which is one young classical T Tauri star.

---------------------------------------------------------
Title: Chemical Characterization of Surface Salts in Qaidam Basin:
    Implications for Climates of Planet Earth and Mars
Authors: Kong, X.; Liu, W.; Li, J.; Santos, L.; Boman, J.; Zhang,
   X.; Wang, S.
2021LPI....52.1191K    Altcode:
  The Qaidam Basin has been considered as a good terrestrial analogue
  for Mars, so here we study the physical and chemical properties of salt
  samples from the Qaidam Basin to shed light on the climate systems on
  planet Earth and Mars.

---------------------------------------------------------
Title: Evidence of a thick halo for the spatial-dependent propagation
    model with Cosmic Ray anisotropy
Authors: Qiao, Bing-Qiang; Yao, Yu-Hua; Liu, Wei; Yuan, Qiang; Bi,
   Xiao-Jun; Hu, Hong-Bo; Guo, Yi-Qing
2021arXiv210213498Q    Altcode:
  The spatial-dependent propagation (SDP) model with a nearby source
  works well to reproduce the co-evolving features of both cosmic ray
  (CR) nuclei spectra and anisotropy. However, it is well known that the
  Sun is offset from the Galactic plane. This will lead to a dominating
  anisotropy in perpendicular direction, which is discrepant with
  observations. Thus it is necessary to reboot further investigation into
  the effect of the solar offset. In this work, for the first time the
  combined studies of the solar offset, nuclei spectra and anisotropy are
  performed based on the SDP model. As a result, to reproduce CR spectra
  and anisotropy, the thickness of the halo $\rm (\xi z_h)$ increases
  linearly with the displacement of the Sun. When the offset is $\rm
  \sim8~pc$ as estimated from the matter-borne methods, $\rm \xi z_h$
  is about 0.9 kpc, which is a much thicker halo than usually. Moreover,
  the PeV anisotropy could estimate the value of diffusion coefficient,
  thus breaking the degeneracy of diffusion coefficient and halo
  thickness. Therefore it is a good messenger to constrain the halo
  thickness. On the other hand, the anisotropy in PeV energy region,
  as a new probe, might also shed new light to constrain the solar
  offset. We hope that the anisotropy at the energies of $\rm \sim TeV$
  to $\rm PeV$ can be finely measured by LHAASO experiment, leading to
  a better understanding about the thick halo.

---------------------------------------------------------
Title: Earth Wind as a Possible Exogenous Source of Lunar Surface
    Hydration
Authors: Wang, H. Z.; Zhang, J.; Shi, Q. Q.; Saito, Y.; Degeling,
   A. W.; Rae, I. J.; Zong, Q. G.; Wei, Y.; Liu, J.; Guo, R. L.; Yao,
   Z. H.; Tian, A. M.; Fu, X. H.; Liu, J. Z.; Ling, Z. C.; Fu, S. Y.;
   Sun, W. J.; Bai, S. C.; Chen, J.; Yao, S. T.; Zhang, H.; Liu, W. L.;
   Xia, L. D.; Feng, Y. Y.; Pu, Z. Y.
2021ApJ...907L..32W    Altcode:
  Understanding the sources of lunar water is crucial for studying
  the history of lunar evolution, as well as the interaction of solar
  wind with the Moon and other airless bodies. Recent orbital spectral
  observations revealed that the solar wind is a significant exogenous
  driver of lunar surficial hydration. However, the solar wind is shielded
  over a period of 3-5 days per month as the Moon passes through the
  Earth's magnetosphere, during which a significant loss of hydration
  is expected. Here we report the temporal and spatial distribution
  of polar surficial OH/H<SUB>2</SUB>O abundance, using Chandrayaan-1
  Moon Mineralogy Mapper (M<SUP>3</SUP>) data, which covers the regions
  inside/outside the Earth's magnetosphere. The data shows that polar
  surficial OH/H<SUB>2</SUB>O abundance increases with latitude, and that
  the probability of polar surficial OH/H<SUB>2</SUB>O abundance remains
  at the same level when in the solar wind and in the magnetosphere
  by controlling latitude, composition, and lunar local time. This
  indicates that the OH/H<SUB>2</SUB>O abundance in the polar regions
  may be saturated, or supplemented from other possible sources, such
  as Earth wind (particles from the magnetosphere, distinct from the
  solar wind), which may compensate for thermal diffusion losses while
  the Moon lies within the Earth's magnetosphere. This work provides
  some clues for studies of planet-moon systems, whereby the planetary
  wind serves as a bridge connecting the planet with its moons.

---------------------------------------------------------
Title: Study of BESIII trigger efficiencies with the 2018 J/ψ data
Authors: Ablikim, M.; Achasov, M. N.; Adlarson, P.; Ahmed, S.;
   Albrecht, M.; Aliberti, R.; Amoroso, A.; An, M. R.; An, Q.; Bai,
   X. H.; Bai, Y.; Bakina, O.; Ferroli, R. Baldini; Balossino, I.; Ban,
   Y.; Begzsuren, K.; Berger, N.; Bertani, M.; Bettoni, D.; Bianchi,
   F.; Bloms, J.; Bortone, A.; Boyko, I.; Briere, R. A.; Cai, H.; Cai,
   X.; Calcaterra, A.; Cao, G. F.; Cao, N.; Cetin, S. A.; Chang, J. F.;
   Chang, W. L.; Chelkov, G.; Chen, D. Y.; Chen, G.; Chen, H. S.; Chen,
   M. L.; Chen, S. J.; Chen, X. R.; Chen, Y. B.; Chen, Z. J.; Cheng,
   W. S.; Cibinetto, G.; Cossio, F.; Cui, X. F.; Dai, H. L.; Dai, X. C.;
   Dbeyssi, A.; Boer, R. E. De; Dedovich, D.; Deng, Z. Y.; Denig, A.;
   Denysenko, I.; Destefanis, M.; de Mori, F.; Ding, Y.; Dong, C.; Dong,
   J.; Dong, L. Y.; Dong, M. Y.; Dong, X.; Du, S. X.; Fan, Y. L.; Fang,
   J.; Fang, S. S.; Fang, Y.; Farinelli, R.; Fava, L.; Feldbauer, F.;
   Felici, G.; Feng, C. Q.; Feng, J. H.; Fritsch, M.; Fu, C. D.; Gao,
   Y.; Gao, Y.; Gao, Y.; Gao, Y. G.; Garzia, I.; Ge, P. T.; Geng, C.;
   Gersabeck, E. M.; Gilman, A.; Goetzen, K.; Gong, L.; Gong, W. X.;
   Gradl, W.; Greco, M.; Gu, L. M.; Gu, M. H.; Gu, S.; Gu, Y. T.; Guan,
   C. Y.; Guo, A. Q.; Guo, L. B.; Guo, R. P.; Guo, Y. P.; Guskov, A.;
   Han, T. T.; Han, W. Y.; Hao, X. Q.; Harris, F. A.; Hüsken, H.; He,
   K. L.; Heinsius, F. H.; Heinz, C. H.; Held, T.; Heng, Y. K.; Herold,
   C.; Himmelreich, M.; Holtmann, T.; Hou, Y. R.; Hou, Z. L.; Hu, H. M.;
   Hu, J. F.; Hu, T.; Hu, Y.; Huang, G. S.; Huang, L. Q.; Huang, X. T.;
   Huang, Y. P.; Huang, Z.; Hussain, T.; Ikegami Andersson, W.; Imoehl,
   W.; Irshad, M.; Jaeger, S.; Janchiv, S.; Ji, Q.; Ji, Q. P.; Ji, X. B.;
   Ji, X. L.; Jiang, H. B.; Jiang, X. S.; Jiao, J. B.; Jiao, Z.; Jin,
   S.; Jin, Y.; Johansson, T.; Kalantar-Nayestanaki, N.; Kang, X. S.;
   Kappert, R.; Kavatsyuk, M.; Ke, B. C.; Keshk, I. K.; Khoukaz, A.;
   Kiese, P.; Kiuchi, R.; Kliemt, R.; Koch, L.; Kolcu, O. B.; Kopf, B.;
   Kuemmel, M.; Kuessner, M.; Kupsc, A.; Kurth, M. G.; Kühn, W.; Lane,
   J. J.; Lange, J. S.; Larin, P.; Lavania, A.; Lavezzi, L.; Lei, Z. H.;
   Leithoff, H.; Lellmann, M.; Lenz, T.; Li, C.; Li, C. H.; Li, Cheng;
   Li, D. M.; Li, F.; Li, G.; Li, H.; Li, H.; Li, H. B.; Li, H. J.; Li,
   J. L.; Li, J. Q.; Li, J. S.; Li, Ke; Li, L. K.; Li, Lei; Li, P. R.;
   Li, S. Y.; Li, W. D.; Li, W. G.; Li, X. H.; Li, X. L.; Li, Z. Y.;
   Liang, H.; Liang, H.; Liang, H.; Liang, Y. F.; Liang, Y. T.; Liao,
   L. Z.; Libby, J.; Lin, C. X.; Liu, B. J.; Liu, C. X.; Liu, D.; Liu,
   F. H.; Liu, Fang; Liu, Feng; Liu, H. B.; Liu, H. M.; Liu, Huanhuan;
   Liu, Huihui; Liu, J. B.; Liu, J. L.; Liu, J. Y.; Liu, K.; Liu, K. Y.;
   Liu, Ke; Liu, L.; Liu, M. H.; Liu, P. L.; Liu, Q.; Liu, Q.; Liu, S. B.;
   Liu, Shuai; Liu, T.; Liu, W. M.; Liu, X.; Liu, Y.; Liu, Y. B.; Liu,
   Z. A.; Liu, Z. Q.; Lou, X. C.; Lu, F. X.; Lu, F. X.; Lu, H. J.; Lu,
   J. D.; Lu, J. G.; Lu, X. L.; Lu, Y.; Lu, Y. P.; Luo, C. L.; Luo, M. X.;
   Luo, P. W.; Luo, T.; Luo, X. L.; Lusso, S.; Lyu, X. R.; Ma, F. C.;
   Ma, H. L.; Ma, L. L.; Ma, M. M.; Ma, Q. M.; Ma, R. Q.; Ma, R. T.;
   Ma, X. X.; Ma, X. Y.; Maas, F. E.; Maggiora, M.; Maldaner, S.; Malde,
   S.; Malik, Q. A.; Mangoni, A.; Mao, Y. J.; Mao, Z. P.; Marcello, S.;
   Meng, Z. X.; Messchendorp, J. G.; Mezzadri, G.; Min, T. J.; Mitchell,
   R. E.; Mo, X. H.; Mo, Y. J.; Muchnoi, N. Yu.; Muramatsu, H.; Nakhoul,
   S.; Nefedov, Y.; Nerling, F.; Nikolaev, I. B.; Ning, Z.; Nisar, S.;
   Olsen, S. L.; Ouyang, Q.; Pacetti, S.; Pan, X.; Pan, Y.; Pathak, A.;
   Patteri, P.; Pelizaeus, M.; Peng, H. P.; Peters, K.; Pettersson, J.;
   Ping, J. L.; Ping, R. G.; Poling, R.; Prasad, V.; Qi, H.; Qi, H. R.;
   Qi, K. H.; Qi, M.; Qi, T. Y.; Qi, T. Y.; Qian, S.; Qian, W. -B.;
   Qian, Z.; Qiao, C. F.; Qin, L. Q.; Qin, X. S.; Qin, Z. H.; Qiu, J. F.;
   Qu, S. Q.; Rashid, K. H.; Ravindran, K.; Redmer, C. F.; Rivetti, A.;
   Rodin, V.; Rolo, M.; Rong, G.; Rosner, Ch.; Rump, M.; Sang, H. S.;
   Sarantsev, A.; Schelhaas, Y.; Schnier, C.; Schoenning, K.; Scodeggio,
   M.; Shan, D. C.; Shan, W.; Shan, X. Y.; Shangguan, J. F.; Shao, M.;
   Shen, C. P.; Shen, P. X.; Shen, X. Y.; Shi, H. C.; Shi, R. S.; Shi,
   X.; Shi, X. D.; Song, W. M.; Song, Y. X.; Sosio, S.; Spataro, S.;
   Su, K. X.; Su, P. P.; Sui, F. F.; Sun, G. X.; Sun, H. K.; Sun, J. F.;
   Sun, L.; Sun, S. S.; Sun, T.; Sun, W. Y.; Sun, W. Y.; Sun, X.; Sun,
   Y. J.; Sun, Y. K.; Sun, Y. Z.; Sun, Z. T.; Tan, Y. H.; Tan, Y. X.;
   Tang, C. J.; Tang, G. Y.; Tang, J.; Teng, J. X.; Thoren, V.; Uman, I.;
   Wang, B.; Wang, C. W.; Wang, D. Y.; Wang, H. J.; Wang, H. P.; Wang,
   K.; Wang, L. L.; Wang, M.; Wang, M. Z.; Wang, Meng; Wang, W.; Wang,
   W. H.; Wang, W. P.; Wang, X.; Wang, X. F.; Wang, X. L.; Wang, Y.;
   Wang, Y.; Wang, Y. D.; Wang, Y. F.; Wang, Y. Q.; Wang, Y. Y.; Wang,
   Z.; Wang, Z. Y.; Wang, Ziyi; Wang, Zongyuan; Wei, D. H.; Weidenkaff,
   P.; Weidner, F.; Wen, S. P.; White, D. J.; Wiedner, U.; Wilkinson,
   G.; Wolke, M.; Wollenberg, L.; Wu, J. F.; Wu, L. H.; Wu, L. J.; Wu,
   X.; Wu, Z.; Xia, L.; Xiao, H.; Xiao, S. Y.; Xiao, Z. J.; Xie, X. H.;
   Xie, Y. G.; Xie, Y. H.; Xing, T. Y.; Xu, G. F.; Xu, Q. J.; Xu, W.;
   Xu, X. P.; Yan, F.; Yan, L.; Yan, W. B.; Yan, W. C.; Yan, Xu; Yang,
   H. J.; Yang, H. X.; Yang, L.; Yang, S. L.; Yang, Y. X.; Yang, Yifan;
   Yang, Zhi; Ye, M.; Ye, M. H.; Yin, J. H.; You, Z. Y.; Yu, B. X.; Yu,
   C. X.; Yu, G.; Yu, J. S.; Yu, T.; Yuan, C. Z.; Yuan, L.; Yuan, X. Q.;
   Yuan, Y.; Yuan, Z. Y.; Yue, C. X.; Yuncu, A.; Zafar, A. A.; Zeng,
   Y.; Zhang, B. X.; Zhang, Guangyi; Zhang, H.; Zhang, H. H.; Zhang,
   H. H.; Zhang, H. Y.; Zhang, J. J.; Zhang, J. L.; Zhang, J. Q.; Zhang,
   J. W.; Zhang, J. Y.; Zhang, J. Z.; Zhang, Jianyu; Zhang, Jiawei;
   Zhang, L. Q.; Zhang, Lei; Zhang, S.; Zhang, S. F.; Zhang, Shulei;
   Zhang, X. D.; Zhang, X. Y.; Zhang, Y.; Zhang, Y. H.; Zhang, Y. T.;
   Zhang, Yan; Zhang, Yao; Zhang, Yi; Zhang, Z. H.; Zhang, Z. Y.; Zhao,
   G.; Zhao, J.; Zhao, J. Y.; Zhao, J. Z.; Zhao, Lei; Zhao, Ling; Zhao,
   M. G.; Zhao, Q.; Zhao, S. J.; Zhao, Y. B.; Zhao, Y. X.; Zhao, Z. G.;
   Zhemchugov, A.; Zheng, B.; Zheng, J. P.; Zheng, Y.; Zheng, Y. H.;
   Zhong, B.; Zhong, C.; Zhou, L. P.; Zhou, Q.; Zhou, X.; Zhou, X. K.;
   Zhou, X. R.; Zhu, A. N.; Zhu, J.; Zhu, K.; Zhu, K. J.; Zhu, S. H.;
   Zhu, T. J.; Zhu, W. J.; Zhu, W. J.; Zhu, Y. C.; Zhu, Z. A.; Zou,
   B. S.; Zou, J. H.; ( Besiii Collaboration )
2021ChPhC..45b3002A    Altcode:
  Using a dedicated data sample taken in 2018 on the J/ψ peak, we
  perform a detailed study of the trigger efficiencies of the BESIII
  detector. The efficiencies are determined from three representative
  physics processes, namely Bhabha scattering, dimuon production
  and generic hadronic events with charged particles. The combined
  efficiency of all active triggers approaches 100% in most cases, with
  uncertainties small enough not to affect most physics analyses. *
  Supported in part by National Key Basic Research Program of China
  (2015CB856700); National Natural Science Foundation of China (NSFC)
  (11625523, 11635010, 11735014, 11822506, 11835012, 11935015,
  11935016, 11935018, 11961141012); the Chinese Academy of Sciences
  (CAS) Large-Scale Scientific Facility Program; Joint Large-Scale
  Scientific Facility Funds of the NSFC and CAS (U1732263, U1832207);
  CAS Key Research Program of Frontier Sciences (QYZDJ-SSW-SLH003,
  QYZDJ-SSW-SLH040); 100 Talents Program of CAS; INPAC and Shanghai Key
  Laboratory for Particle Physics and Cosmology; ERC (758462); German
  Research Foundation DFG under Contracts Nos. Collaborative Research
  Center CRC 1044, FOR 2359; Istituto Nazionale di Fisica Nucleare,
  Italy; Ministry of Development of Turkey (DPT2006K-120470); National
  Science and Technology fund; Olle Engkvist Foundation (200-0605); STFC
  (United Kingdom); The Knut and Alice Wallenberg Foundation (Sweden)
  (2016.0157); The Royal Society, UK (DH140054, DH160214); The Swedish
  Research Council; U. S. Department of Energy (DE-FG02-05ER41374,
  DE-SC-0012069)

---------------------------------------------------------
Title: The noncommutative values of quantum observables
Authors: Kong, Otto C. W.; Liu, Wei-Yin
2021ChJPh..69...70K    Altcode: 2019arXiv190309071K
  We discuss the notion about physical quantities as having values
  represented by real numbers, and its limiting to describe nature to be
  understood in relation to our appreciation that the quantum theory is a
  better theory of natural phenomena than its classical analog. Getting
  from the algebra of physical observables to their values on a fixed
  state is, at least for classical physics, really a homomorphic map from
  the algebra into the real number algebra. The limitation of the latter
  to represent the values of quantum observables with noncommutating
  algebraic relation is obvious. We introduce and discuss the idea of
  the noncommutative values of quantum observables and its feasibility,
  arguing that at least in terms of the representation of such a value
  as an infinite set of complex number, the idea makes reasonable sense
  theoretically as well as practically.

---------------------------------------------------------
Title: Multi-wavelength photometry during the 2018 superoutburst of
    the WZ Sge-type dwarf nova EG Cancri
Authors: Kimura, Mariko; Isogai, Keisuke; Kato, Taichi; Kojiguchi,
   Naoto; Wakamatsu, Yasuyuki; Ohnishi, Ryuhei; Sugiura, Yuki;
   Matsumoto, Hanami; Sumiya, Sho; Ito, Daiki; Nikai, Kengo; Matsumoto,
   Katsura; Shugarov, Sergey Yu; Katysheva, Natalia; Itoh, Hiroshi;
   Dubovsky, Pavol A.; Kudzej, Igor; Akitaya, Hiroshi; Oide, Kohei;
   Kanai, Takahiro; Ishioka, Chihiro; Uzawa, Yoshinori; Oasa, Yumiko;
   Vanmunster, Tonny; Oksanen, Arto; Tordai, Tamás; Murata, Katsuhiro
   L.; Shiraishi, Kazuki; Adachi, Ryo; Oeda, Motoki; Tachibana, Yutaro;
   Kiyota, Seiichiro; Pavlenko, Elena P.; Antonyuk, Kirill; Antonyuk,
   Oksana; Pit, Nikolai; Sosnovskij, Aleksei; Babina, Julia; Baklanov,
   Alex; Kawabata, Koji S.; Kawabata, Miho; Nakaoka, Tatsuya; Yamanaka,
   Masayuki; Kasai, Kiyoshi; Miller, Ian; Brincat, Stephen M.; Liu, Wei;
   Sasada, Mahito; Nogami, Daisaku
2021PASJ...73....1K    Altcode: 2020PASJ..tmp..247K; 2020arXiv200811871K
  We report on the multi-wavelength photometry of the 2018 superoutburst
  in EG Cnc. We have detected stage A superhumps and long-lasting
  late-stage superhumps via the optical photometry and have constrained
  the binary mass ratio and its possible range. The median value of
  the mass ratio is 0.048 and the upper limit is 0.057, which still
  implies that EG Cnc is one of the possible candidates for period
  bouncers. This object also showed multiple rebrightenings in this
  superoutburst which are the same as those in its previous superoutburst
  in 1996-1997, despite the difference in the main superoutburst. This
  would represent that the rebrightening type is inherent to each
  object and is independent of the initial disk mass at the beginning
  of superoutbursts. We also found that B - I and J - K<SUB>s</SUB>
  colors were unusually red just before the rebrightening phase and
  became bluer during the quiescence between rebrightenings, which would
  mean that the low-temperature mass reservoir at the outermost disk
  accreted with time after the main superoutburst. Also, the ultraviolet
  flux was sensitive to rebrightenings as well as the optical flux,
  and the U - B color became redder during the rebrightening phase,
  which would indicate that the inner disk became cooler when this object
  repeated rebrightenings. Our results thus basically support the idea
  that the cool mass reservoir in the outermost disk is responsible
  for rebrightenings.

---------------------------------------------------------
Title: Follow-up observations for IceCube-170922A: Detection of rapid
    near-infrared variability and intensive monitoring of TXS 0506+056
Authors: Morokuma, Tomoki; Utsumi, Yousuke; Ohta, Kouji; Yamanaka,
   Masayuki; Kawabata, Koji S.; Inoue, Yoshiyuki; Tanaka, Masaomi;
   Yoshida, Michitoshi; Itoh, Ryosuke; Sasada, Mahito; Tominaga, Nozomu;
   Mori, Hiroki; Kawabata, Miho; Nakaoka, Tatsuya; Chogi, Maiko; Abe,
   Taisei; Huang, Ruochen; Kawahara, Naoki; Kimura, Hiroki; Nagashima,
   Hiroki; Takagi, Kengo; Yamazaki, Yuina; Liu, Wei; Ohsawa, Ryou;
   Sako, Shigeyuki; Murata, Katsuhiro L.; Morihana, Kumiko; Gilligan,
   Christina K.; Isogai, Keisuke; Kimura, Mariko; Wakamatsu, Yasuyuki;
   Ohnishi, Ryuhei; Takayama, Masaki; Honda, Satoshi; Matsuoka, Yoshiki;
   Yamashita, Takuji; Nagataki, Shigehiro; Tanaka, Yasuyuki T.
2021PASJ...73...25M    Altcode: 2021PASJ..tmp....5M; 2020arXiv201104957M
  We present our follow-up observations to search for an
  electromagnetic counterpart of the IceCube high-energy neutrino
  IceCube-170922A. Monitoring observations of a likely counterpart,
  TXS 0506+056, are also described. First, we quickly took optical and
  near-infrared images of seven flat-spectrum radio sources within
  the IceCube error region right after the neutrino detection and
  found a rapid flux decline of TXS 0506+056 in Kanata/HONIR J-band
  data. Motivated by this discovery, intensive follow-up observations
  of TXS 0506+056 were continuously performed, including our monitoring
  imaging observations, spectroscopic observations, and polarimetric
  observations in optical and near-infrared wavelengths. TXS 0506+056
  showed a large-amplitude (~1.0 mag) variability in a time scale of
  several days or longer, although no significant variability was
  detected in a time scale of a day or shorter. TXS 0506+056 also
  showed a bluer-when-brighter trend in optical and near-infrared
  wavelengths. Structure functions of the variabilities were examined
  and indicate that TXS 0506+056 is not a special blazar in terms of
  optical variability. Polarization measurement results of TXS 0506+056
  are also discussed.

---------------------------------------------------------
Title: Observation of the Crab Nebula with LHAASO-KM2A - a performance
    study
Authors: Aharonian, F.; An, Q.; Axikegu; Bai, L. X.; Bai, Y. X.; Bao,
   Y. W.; Bastieri, D.; Bi, X. J.; Bi, Y. J.; Cai, H.; Cai, J. T.; Cao,
   Z.; Cao, Z.; Chang, J.; Chang, J. F.; Chang, X. C.; Chen, B. M.;
   Chen, J.; Chen, L.; Chen, L.; Chen, L.; Chen, M. J.; Chen, M. L.;
   Chen, Q. H.; Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen,
   Y.; Cheng, N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Dai,
   B. Z.; Dai, H. L.; Dai, Z. G.; Danzengluobu; Della Volpe, D.; Piazzoli,
   B. D'ettorre; Dong, X. J.; Fan, J. H.; Fan, Y. Z.; Fan, Z. X.; Fang,
   J.; Fang, K.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng, Y. L.; Gao,
   B.; Gao, C. D.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.;
   Gou, Q. B.; Gu, M. H.; Guo, J. G.; Guo, X. L.; Guo, Y. Q.; Guo, Y. Y.;
   Han, Y. A.; He, H. H.; He, H. N.; He, J. C.; He, S. L.; He, X. B.;
   He, Y.; Heller, M.; Hor, Y. K.; Hou, C.; Hou, X.; Hu, H. B.; Hu,
   S.; Hu, S. C.; Hu, X. J.; Huang, D. H.; Huang, Q. L.; Huang, W. H.;
   Huang, X. T.; Huang, Z. C.; Ji, F.; Ji, X. L.; Jia, H. Y.; Jiang, K.;
   Jiang, Z. J.; Jin, C.; Kuleshov, D.; Levochkin, K.; Li, B. B.; Li,
   C.; Li, C.; Li, F.; Li, H. B.; Li, H. C.; Li, H. Y.; Li, J.; Li, K.;
   Li, W. L.; Li, X.; Li, X.; Li, X. R.; Li, Y.; Li, Y. Z.; Li, Z.; Li,
   Z.; Liang, E. W.; Liang, Y. F.; Lin, S. J.; Liu, B.; Liu, C.; Liu, D.;
   Liu, H.; Liu, H. D.; Liu, J.; Liu, J. L.; Liu, J. S.; Liu, J. Y.; Liu,
   M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.; Liu, Y. N.; Liu, Z. X.; Long,
   W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma, L. L.; Ma, X. H.; Mao, J. R.;
   Masood, A.; Mitthumsiri, W.; Montaruli, T.; Nan, Y. C.; Pang, B. Y.;
   Pattarakijwanich, P.; Pei, Z. Y.; Qi, M. Y.; Ruffolo, D.; Rulev, V.;
   Sáiz, A.; Shao, L.; Shchegolev, O.; Sheng, X. D.; Shi, J. R.; Song,
   H. C.; Stenkin, Yu. V.; Stepanov, V.; Sun, Q. N.; Sun, X. N.; Sun,
   Z. B.; Tam, P. H. T.; Tang, Z. B.; Tian, W. W.; Wang, B. D.; Wang,
   C.; Wang, H.; Wang, H. G.; Wang, J. C.; Wang, J. S.; Wang, L. P.;
   Wang, L. Y.; Wang, R. N.; Wang, W.; Wang, W.; Wang, X. G.; Wang,
   X. J.; Wang, X. Y.; Wang, Y. D.; Wang, Y. J.; Wang, Y. P.; Wang,
   Z.; Wang, Z.; Wang, Z. H.; Wang, Z. X.; Wei, D. M.; Wei, J. J.;
   Wei, Y. J.; Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.; Wu,
   X. F.; Xi, S. Q.; Xia, J.; Xia, J. J.; Xiang, G. M.; Xiao, G.; Xiao,
   H. B.; Xin, G. G.; Xin, Y. L.; Xing, Y.; Xu, D. L.; Xu, R. X.; Xue,
   L.; Yan, D. H.; Yang, C. W.; Yang, F. F.; Yang, J. Y.; Yang, L. L.;
   Yang, M. J.; Yang, R. Z.; Yang, S. B.; Yao, Y. H.; Yao, Z. G.; Ye,
   Y. M.; Yin, L. Q.; Yin, N.; You, X. H.; You, Z. Y.; Yu, Y. H.; Yuan,
   Q.; Zeng, H. D.; Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhai,
   X. X.; Zhang, B. B.; Zhang, H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang,
   J. W.; Zhang, L.; Zhang, L.; Zhang, L. X.; Zhang, P. F.; Zhang, P. P.;
   Zhang, R.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang, X. P.; Zhang,
   Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. L.; Zhao, B.; Zhao, J.; Zhao,
   L.; Zhao, L. Z.; Zhao, S. P.; Zheng, F.; Zheng, Y.; Zhou, B.; Zhou,
   H.; Zhou, J. N.; Zhou, P.; Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu,
   F. R.; Zhu, H.; Zhu, K. J.; Zuo, X.; (Lhaaso Collaboration)
2021ChPhC..45b5002A    Altcode: 2020arXiv201006205A
  A sub-array of the Large High Altitude Air Shower Observatory (LHAASO),
  KM2A is mainly designed to observe a large fraction of the northern
  sky to hunt for γ-ray sources at energies above 10 TeV. Even though
  the detector construction is still underway, half of the KM2A array has
  been operating stably since the end of 2019. In this paper, we present
  the KM2A data analysis pipeline and the first observation of the Crab
  Nebula, a standard candle in very high energy γ-ray astronomy. We
  detect γ-ray signals from the Crab Nebula in both energy ranges of 10
  $ - $ 100 TeV and $ \gt $ 100 TeV with high significance, by analyzing
  the KM2A data of 136 live days between December 2019 and May 2020. With
  the observations, we test the detector performance, including angular
  resolution, pointing accuracy and cosmic-ray background rejection
  power. The energy spectrum of the Crab Nebula in the energy range 10-250
  TeV fits well with a single power-law function dN/dE = (1.13 $ \pm $
  0.05 $ _{\rm stat} $ $ \pm $ 0.08 $ _{\rm sys} $ ) $ \times $ 10 $
  ^{-14} $ $ \cdot $ (E/20 TeV) $ ^{-3.09\pm0.06_{\rm stat}\pm0.02_{\rm
  sys}} $ cm $ ^{-2} $ s $ ^{-1} $ TeV $ ^{-1} $ . It is consistent with
  previous measurements by other experiments. This opens a new window of
  γ-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray
  phenomena, such as cosmic PeVatrons, might be discovered. * Supported
  in China by National Key R&amp;D program of China under the grants
  (2018YFA0404201, 2018YFA0404202, 2018YFA0404203), by NSFC (12022502,
  11905227, 11635011, 11761141001, U1931112, 11775131, U1931201, 11905043,
  U1931108), by NSFSPC (ZR2019MA014), and in Thailand by RTA6280002 from
  Thailand Science Research and Innovation

---------------------------------------------------------
Title: Looking for the Detail and Context Devils: High-Resolution
    Salient Object Detection
Authors: Zhang, Pingping; Liu, Wei; Zeng, Yi; Lei, Yinjie; Lu, Huchuan
2021ITIP...30.3204Z    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Exploration of Low-Energy Earth-Moon Transfer Orbit Based on
    Crossing Orbit of Double Three-Body System
Authors: Zhang, Juan; Liu, Wei; Cao, Xiaofei
2021JPhCS1739a2051Z    Altcode:
  The design of low energy lunar transfer orbit and orbit optimization
  method based on crossing orbit is studied in this paper. The four-body
  problem of Sun-Earth-Moon-satellite is decoupled into two three-body
  problems of Sun-Earth-satellite and Earth-Moon-satellite. Low-energy
  lunar exploration orbit is designed by changing orbit at a certain
  intersection field through manifold of two Halo orbit of three-body
  system. A serial optimization design method for global initial value
  search and local gradient optimization are designed. When a motion
  state variable is partially modified, the differential correction
  method combined with adaptive regression algorithm is adopted. For
  the splicing points of manifolds of different systems, the velocity
  vector is modified to make the spacecraft get into the target berthing
  track, and to obtain the splicing points that can form crossing track
  of the two three-body systems. An example of orbit design is given to
  show that the Earth-Moon transfer orbit based on invariant manifold
  splicing has the characteristics of energy saving and long-time
  consumption, which can be used for the tasks with large loads and low
  time requirements. This research provides a method for the design of
  low energy lunar transfer orbit. It will benefit the energy consuming,
  material design of spacecraft, and so on.

---------------------------------------------------------
Title: On Cooling Condensation Near Magnetic Null Points and the
    Formation of Solar Coronal Rain and Prominences
Authors: Liu, Wei; Titov, Viacheslav; Downs, Cooper; Antolin, Patrick;
   Luna, Manuel; Sun, Xudong; Berger, Thomas; Yu, Sijie; Yoffe, Luke
2021cosp...43E.975L    Altcode:
  The Sun's outer atmosphere, the corona, is million-degrees hot and
  tenuous. Such hot plasma, under certain conditions, can enigmatically
  undergo a radiative cooling instability and condense into material of
  100 times cooler in the form of coronal rain or prominences. Where,
  when, and how such cooling condensation takes place remain poorly
  understood. Answers to these questions are not only important in their
  own right, but also bear implications for the fundamental question
  of coronal heating and the chromosphere-corona mass cycle. Magnetic
  fields in the magnetized corona undoubtedly play a crucial role (e.g.,
  by trapping the plasma), but where and how? We report recent imaging
  and spectroscopic observations from SDO/AIA/HMI and IRIS that can
  shed light on this puzzle. Through a systematic survey, we found that
  a large fraction of quiet-Sun condensations preferentially occur at
  the dips of coronal loops or funnels. Such dips are located at/near
  magnetic topological features, such as null points and quasi-separatrix
  layers (QSLs), which are regions characterized by high values of the
  squashing factor. We also identified evidence of magnetic reconnection
  at such locations, which can produce favorable conditions, e.g., density
  enhancement by compression and/or mass trapping in plasmoids, that can
  trigger run-away radiative cooling. We present proof-of-concept MHD
  simulations that demonstrate the role of reconnection in transporting
  cooled mass from overlying, long loops to underlying, short loops where
  it slides down as coronal rain. We will discuss the significance and
  broader implications of these results beyond the Sun.

---------------------------------------------------------
Title: Formation of α clusters in dilute neutron-rich matter
Authors: Tanaka, Junki; Yang, Zaihong; Typel, Stefan; Adachi, Satoshi;
   Bai, Shiwei; van Beek, Patrik; Beaumel, Didier; Fujikawa, Yuki; Han,
   Jiaxing; Heil, Sebastian; Huang, Siwei; Inoue, Azusa; Jiang, Ying;
   Knösel, Marco; Kobayashi, Nobuyuki; Kubota, Yuki; Liu, Wei; Lou,
   Jianling; Maeda, Yukie; Matsuda, Yohei; Miki, Kenjiro; Nakamura,
   Shoken; Ogata, Kazuyuki; Panin, Valerii; Scheit, Heiko; Schindler,
   Fabia; Schrock, Philipp; Symochko, Dmytro; Tamii, Atsushi; Uesaka,
   Tomohiro; Wagner, Vadim; Yoshida, Kazuki; Zenihiro, Juzo; Aumann,
   Thomas
2021Sci...371..260T    Altcode:
  The surface of neutron-rich heavy nuclei, with a neutron skin created by
  excess neutrons, provides an important terrestrial model system to study
  dilute neutron-rich matter. By using quasi-free α cluster-knockout
  reactions, we obtained direct experimental evidence for the formation of
  α clusters at the surface of neutron-rich tin isotopes. The observed
  monotonous decrease of the reaction cross sections with increasing
  mass number, in excellent agreement with the theoretical prediction,
  implies a tight interplay between α-cluster formation and the neutron
  skin. This result, in turn, calls for a revision of the correlation
  between the neutron-skin thickness and the density dependence of
  the symmetry energy, which is essential for understanding neutron
  stars. Our result also provides a natural explanation for the origin
  of α particles in α decay.

---------------------------------------------------------
Title: Probing the Puzzle of Fermi Long-Duration Gamma-Ray Flares
    by Data-driven Global MHD Simulations
Authors: Jin, Meng; Manchester, Ward, IV; Effenberger, Frederic;
   Petrosian, Vahe; Nitta, Nariaki; Liu, Wei; Omodei, Nicola; Li, Gang;
   Pesce-Rollins, Melissa; Allafort, Alice
2021cosp...43E.906J    Altcode:
  With the increasing number of long-duration gamma-ray solar flares
  &gt;100 MeV observed by Fermi/LAT, it poses a puzzle on the particle
  acceleration and transport mechanisms. The recent detections of
  behind-the-limb (BTL) solar flares (e.g., 2014 September 1 event),
  in which the gamma-ray emission region is located away from the
  BTL flare site by up to tens of degrees in heliographic longitude,
  and on-disk flares with migration of gamma-ray emission centroid
  hours past the impulsive phase (e.g., 2012 March 7 event), present
  further new challenges on the theoretical models for interpreting the
  observations. Since most of the long-duration events are associated
  with fast CMEs, it is therefore intriguing to understand the role
  of CMEs and CME-driven shocks in these events. To probe this puzzle,
  we perform data-driven, global magnetohydrodynamics simulations of the
  CMEs associated with the long-duration gamma-ray flares and investigate
  the magnetic connectivity and evolution of the CME-driven shock, and
  their relationship, in both space and time, with the observed gamma-ray
  emission. Specifically, we derive and track the time-varying shock
  parameters over the area that is magnetically connected to gamma-ray
  emission region. Based on the modeling results, we discuss the causes
  and implications of Fermi long-duration gamma-ray events, in the
  framework of a potential shift of paradigm on particle acceleration
  in solar flares and CMEs.

---------------------------------------------------------
Title: Potential PeVatron supernova remnant G106.3+2.7 seen in the
    highest-energy gamma rays
Authors: Tibet ASγ Collaboration; Amenomori, M.; Bao, Y. W.;
   Bi, X. J.; Chen, D.; Chen, T. L.; Chen, W. Y.; Chen, Xu; Chen, Y.;
   Cirennima, Cui, S. W.; Danzengluobu, Ding, L. K.; Fang, J. H.; Fang,
   K.; Feng, C. F.; Feng, Zhaoyang; Feng, Z. Y.; Gao, Qi; Gou, Q. B.;
   Guo, Y. Q.; Guo, Y. Y.; He, H. H.; He, Z. T.; Hibino, K.; Hotta, N.;
   Hu, Haibing; Hu, H. B.; Huang, J.; Jia, H. Y.; Jiang, L.; Jin, H. B.;
   Kasahara, K.; Katayose, Y.; Kato, C.; Kato, S.; Kawata, K.; Kihara,
   W.; Ko, Y.; Kozai, M.; Labaciren, Le, G. M.; Li, A. F.; Li, H. J.; Li,
   W. J.; Lin, Y. H.; Liu, B.; Liu, C.; Liu, J. S.; Liu, M. Y.; Liu, W.;
   Lou, Y. -Q.; Lu, H.; Meng, X. R.; Munakata, K.; Nakada, H.; Nakamura,
   Y.; Nanjo, H.; Nishizawa, M.; Ohnishi, M.; Ohura, T.; Ozawa, S.;
   Qian, X. L.; Qu, X. B.; Saito, T.; Sakata, M.; Sako, T. K.; Shao, J.;
   Shibata, M.; Shiomi, A.; Sugimoto, H.; Takano, W.; Takita, M.; Tan,
   Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo, S.; Wang, H.; Wu,
   H. R.; Xue, L.; Yamamoto, Y.; Yang, Z.; Yokoe, Y.; Yuan, A. F.; Zhai,
   L. M.; Zhang, H. M.; Zhang, J. L.; Zhang, X.; Zhang, X. Y.; Zhang,
   Y.; Zhang, Yi; Zhang, Ying; Zhao, S. P.; Zhaxisangzhu, Zhou, X. X.
2021NatAs...5..460T    Altcode: 2021NatAs.tmp...41T; 2021arXiv210902898A
  Cosmic rays (protons and other atomic nuclei) are believed to gain
  energies of petaelectronvolts (PeV) and beyond at astrophysical
  particle accelerators called `PeVatrons' inside our Galaxy. Although
  a characteristic feature of a PeVatron is expected to be a hard
  gamma-ray energy spectrum that extends beyond 100 teraelectronvolts
  (TeV) without a cut-off, none of the currently known sources exhibit
  such a spectrum owing to the low maximum energy of accelerated cosmic
  rays or owing to insufficient detector sensitivity around 100 TeV. Here,
  we report the observation of gamma-ray emission from the supernova
  remnant G106.3+2.7 (refs. <SUP>1,2</SUP>) above 10 TeV. This work
  provides flux data points up to and above 100 TeV and indicates that the
  very-high-energy gamma-ray emission above 10 TeV is well correlated with
  a molecular cloud<SUP>3</SUP> rather than with the pulsar PSR J2229+6114
  (refs. <SUP>4-8</SUP>). Regarding the gamma-ray emission mechanism of
  G106.3+2.7, this morphological feature appears to favour a hadronic
  origin via the π<SUP>0</SUP> decay caused by accelerated relativistic
  protons<SUP>9</SUP> over a leptonic origin via the inverse Compton
  scattering by relativistic electrons<SUP>10,11</SUP>. Furthermore, we
  point out that an X-ray flux upper limit on the synchrotron spectrum
  would provide important information to firmly establish the hadronic
  scenario as the mechanism of particle acceleration at the source.

---------------------------------------------------------
Title: Probing the Puzzle of Fermi Long-Duration Gamma-Ray Flares
    by Data-driven Global MHD Simulations
Authors: Jin, M.; Petrosian, V.; Liu, W.; Nitta, N.; Omodei, N.;
   Effenberger, F.; Li, G.; Pesce-Rollins, M.; Allafort, A.; Manchester,
   W.
2020AGUFMSH008..03J    Altcode:
  With the ever growing number of long-duration, &gt;100 MeV gamma-ray
  solar flares observed by Fermi/LAT, it poses a puzzle on the underlying
  particle acceleration and transport mechanisms. Further challenges
  come from (i) recent detection of gamma-rays in behind-the-limb (BTL)
  flares (e.g., the 2014 September 1 event), in which the gamma-ray
  emission region is located away from the BTL flare site by tens of
  degrees in heliographic longitude, and (ii) migration of gamma-ray
  emission centroids on the solar disk hours past the impulsive phase
  (e.g., the 2012 March 7 event). Most of the long-duration events are
  associated with fast CMEs, it is thus necessary to understand the role
  of CMEs and CME-driven shocks in these events. To probe this puzzle,
  we perform data-driven, global magnetohydrodynamics simulations of CMEs
  associated with the long-duration gamma-ray flares. We investigate
  the magnetic connectivity and evolution of the CME-driven shocks,
  and their relationship, in both space and time, with the observed
  gamma-ray emission. Specifically, we derive and track the time-varying
  shock parameters over the area that is magnetically connected to the
  gamma-ray emission region. Based on the modeling results, we discuss
  the causes of Fermi long-duration gamma-ray events. In particular, we
  address the possibility of CME shock-accelerated particles traveling
  back to the Sun to produce gamma-rays, a scenario that bears potentially
  paradigm-shifting implications on particle acceleration and transport
  in solar eruptive events including flares and CMEs.

---------------------------------------------------------
Title: Radial Diffusion of Energetic Protons in the Earth's Inner
    Magnetosphere
Authors: Lyu, X.; Tu, W.; Liu, W.
2020AGUFMSM0330011L    Altcode:
  Radial diffusion is one of the main source mechanisms of ring current
  ions and it could also contribute to the ring current loss by outward
  radial diffusion to the magnetopause. However, the relative contribution
  of radial diffusion to the dynamics of ring current ions has not been
  well quantified. Our work uses a 1D radial diffusion with charge
  exchange loss to simulate the long-term variations of ring current
  protons observed by Van Allen Probes to quantitatively study how
  much of the dynamics could be explained by radial diffusion. We first
  convert the observed proton flux over the period of November 2012 to
  September 2013 to phase space densities (PSD) as a function of adiabatic
  invariants (μ, K, L<SUP>*</SUP>) using TS04 magnetic model. Then the
  PSD variation at L*=5.5 is used as our outer boundary condition. Our
  model uses empirical formulae of radial diffusion coefficient and
  charge exchange lifetime as inputs but including a free parameter
  in each formula to account for its uncertainties. The free parameter
  values are determined by best fitting the model results to PSD data
  at given μ and K values. The simulation results show that our model
  generally captures the transport and acceleration of ring current
  protons at μ=30,50,80 MeV/G and K=0.11G G<SUP>1/2</SUP>R<SUB>E</SUB>,
  which demonstrates that radial diffusion is the dominant source of
  &gt;75 keV protons in the ring current. The observed fast decay of PSD
  at lower μ and slow decay at higher μ is also well captured by the
  charge exchange loss in the model. However, fast dropouts of PSD are
  observed over a wide range of L*. The large-L* dropout at L*&gt;4 is
  reproduced by the model with outward radial diffusion to the reduced
  outer boundary. But the smaller-L* loss (on the time scale of hours) is
  too fast to be explained by charge exchange, which could potentially be
  due to other loss mechanisms including EMIC wave scattering and field
  line curvature scattering. These loss mechanisms will be included in
  our model in the future.

---------------------------------------------------------
Title: Solar Prominence Bubbles and Associated Plasma Instabilities:
    IRIS Observations and MHD Modeling
Authors: Liu, W.; Berger, T. E.; Fan, Y.
2020AGUFMSH0010014L    Altcode:
  Solar prominences are cool and dense plasma in the hot corona. The
  so-called prominence bubbles are mysterious, dome-shaped, apparently
  void structures residing in the lower portions of prominences. Such
  bubbles are associated with various plasma instabilities, such as the
  Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The
  former is manifested in plumes that are often produced at the top
  boundary of a bubble and intrude upward into the dense prominence
  material. The latter is found to be triggered by shear flows at the
  bubble boundaries. We present recent observations of prominence
  bubbles by IRIS, focusing on the diagnostic potential of RT and
  KH instabilities on the physical conditions of the prominence and
  its supporting magnetic field. We search for evidence of magnetic
  flux emergence as the origin of prominence bubbles. We also present
  preliminary 3D MHD simulations of the interaction of a bipole, as a
  hypothetical bubble, emerging into an overlying prominence-carrying
  flux-rope system. The simulations can provide further clues to the
  origin and nature of prominence bubbles. We discuss their roll in mass
  ad magnetic flux transport in the solar atmosphere.

---------------------------------------------------------
Title: The HinOTORI Telescope and its remote control system
Authors: Liu, Wei; Utsumi, Yousuke; Kawabata, Koji S.; Sasada, Mahito;
   Yao, Yongqiang; Zuo, Yingxi; Lou, Zheng; Shi, Shengcai
2020SPIE11451E..57L    Altcode:
  HinOTORI is a China-Japan co-construction 50cm telescope with
  three-color (u', RC, and IC) simultaneous imager. The main purpose
  aims at identifying gravitational-wave electromagnetic counterpart and
  performing follow-up observation from ultraviolet to near-infrared
  band. The telescope locates at the Tibet plateau, China, with 5100
  meters high altitude. The construction of the telescope has already
  finished, and now it is going on commissioning. In this paper we focus
  on the system and devices for remote control of multi-devices, including
  telescope, mount, dome, three cameras, Power Distribution Units (PDUs),
  sky monitor, and so on. We will also present system performance and
  site condition based on observations collected during commissioning.

---------------------------------------------------------
Title: Probing the magnetosphere via observations of electron flux
    oscillations associated with broadband ULF waves
Authors: Sarris, T. E.; Li, X.; Temerin, M. A.; Zhao, H.; Khoo, L. Y.;
   Turner, D. L.; Liu, W.; Claudepierre, S. G.
2020AGUFMSM010..01S    Altcode:
  Electron flux oscillations are produced in the magnetosphere in
  association with broadband Ultra Low Frequency (ULF) waves. These
  oscillations are observed in the form of drift-periodic flux
  fluctuations, but are not associated with drift echoes following storm-
  or substorm-related energetic particle injections. They are observed
  in particular during quiet times, and could be used as indicators of
  ongoing radial transport processes caused by ULF waves. The amplitudes
  of such flux oscillations is dependent on a number of parameters,
  such as the local phase space density gradient, the amplitude of ULF
  waves and the width of electron energy channels. In particular, the
  latter is a critical parameter affecting the observed amplitude of
  flux oscillations, with narrower energy channel widths enabling the
  observation of higher-amplitude flux oscillations; this potentially
  explains why such features were not observed regularly before the
  Van Allen Probes era, as previous spacecraft generally had lower
  energy resolution. We present simulation and observation results
  quantitatively associating the observed flux oscillations with the
  electron detector width; we also present associations of the observed
  flux oscillations with the local phase space density gradient and
  the amplitude of electric and magnetic fluctuations in the ULF range,
  both of which are expected to also affect radial transport rates.

---------------------------------------------------------
Title: Anthropogenic aerosol forcing of the AMOC and the associated
    mechanisms in CMIP6 models
Authors: Hassan, T.; Allen, R.; Liu, W.; Randles, C. A.
2020AGUFMPP0350013H    Altcode:
  By regulating the global transport of heat, freshwater and carbon,
  the Atlantic Meridional Overturning Circulation (AMOC) serves as
  an important component of the climate system. During the late 20th
  and early 21st centuries, indirect observations and models suggest a
  weakening of the AMOC. Direct AMOC observations also suggest a weakening
  during the early 21st century, but with substantial interannual
  variability. Long-term weakening of the AMOC has been associated with
  increasing greenhouse gases (GHGs), but some modeling studies suggest
  the build up of anthropogenic aerosols (AAs) may have offset part of the
  GHG-induced weakening. Here, we quantify 1900-2020 AMOC variations and
  assess the driving mechanisms in state-of-the-art climate models from
  the Coupled Model Intercomparison Project phase 6 (CMIP6). The CMIP6 all
  forcing (GHGs, anthropogenic and volcanic aerosols, solar variability,
  and land use/land change) multi-model mean shows negligible AMOC
  changes up to 1950, followed by robust AMOC strengthening during the
  second half of the 20th century (1950-1990), and weakening afterwards
  (1990-2020). These multi-decadal AMOC variations are related to changes
  in North Atlantic atmospheric circulation, including an altered sea
  level pressure gradient, storm track activity, surface winds and heat
  fluxes, which drive changes in the subpolar North Atlantic surface
  density flux. Similar to previous studies, CMIP6 GHG simulations yield
  robust AMOC weakening, particularly during the second half of the 20th
  century. Changes in natural forcings, including solar variability and
  volcanic aerosols, yield negligible AMOC changes. In contrast, CMIP6 AA
  simulations yield robust AMOC strengthening (weakening) in response to
  increasing (decreasing) anthropogenic aerosols. Moreover, the CMIP6
  all-forcing AMOC variations and atmospheric circulation responses
  also occur in the CMIP6 AA simulations, which suggests these are
  largely driven by changes in anthropogenic aerosol emissions. Although
  aspects of the CMIP6 all-forcing multi-model mean response resembles
  observations, notable differences exist. This includes CMIP6 AMOC
  strengthening from 1950-1990, when the indirect estimates suggest AMOC
  weakening. The CMIP6 multi-model mean also underestimates the observed
  increase in North Atlantic Ocean heat content. And although the CMIP6
  North Atlantic atmospheric circulation responses-particularly the
  overall patterns-are similar to observations, the simulated responses
  are weaker than those observed, implying they are only partially
  externally forced. The possible causes of these differences include
  internal climate variability, observational uncertainties and model
  shortcomings-including excessive aerosol forcing. A handful of CMIP6
  realizations yield AMOC evolution since 1900 similar to the indirect
  observations, implying the inferred AMOC weakening from 1950-1990 (and
  even from 1930-1990) may have a significant contribution from internal
  (i.e.,~unforced) climate variability. Nonetheless, CMIP6 models yield
  robust, externally forced AMOC changes, the bulk of which are due to
  anthropogenic aerosols.

---------------------------------------------------------
Title: Panoramic SETI: on-sky results from prototype telescopes and
    instrumental design
Authors: Maire, Jérôme; Wright, Shelley A.; Werthimer, Dan; Antonio,
   Franklin P.; Brown, Aaron; Horowitz, Paul; Lee, Ryan; Liu, Wei;
   Raffanti, Rick; Wiley, James; Cosens, Maren; Heffner, Carolyn M.;
   Howard, Andrew W.; Stone, Remington P. S.; Treffers, Richard R.
2020SPIE11454E..3CM    Altcode: 2021arXiv211111080M
  The Panoramic SETI (Search for Extraterrestrial Intelligence) experiment
  (PANOSETI) aims to detect and quantify optical transients from
  nanosecond to second precision over a large field-of-view (∼4,450
  square-degrees). To meet these challenging timing and wide-field
  requirements, the PANOSETI experiment will use two assemblies of ∼45
  telescopes to reject spurious signals by coincidence detection, each
  one comprising custom-made fast photon-counting hardware combined
  with (f/1.32) focusing optics. Preliminary on-sky results from
  pairs of PANOSETI prototype telescopes (100 sq.deg.) are presented
  in terms of instrument performance and false alarm rates. We found
  that a separation of &gt;1 km between telescopes surveying the same
  field-of-view significantly reduces the number of false positives due
  to nearby sources (e.g., Cherenkov showers) in comparison to a side-
  by-side configuration of telescopes. Design considerations on the
  all-sky PANOSETI instrument and expected field-of-views are reported.

---------------------------------------------------------
Title: Mapping diffuse emission in Lyman UV band
Authors: Ji, Li; Lou, Zheng; Zhang, Jinlong; Qiu, Keqiang; Li,
   Shuangying; Sun, Wei; Yan, Shuping; Zhang, Shuinai; Qian, Yuan; Wang,
   Sen; Werner, Klaus; Fang, Taotao; Wang, Tinggui; Barnstedt, Jürgen;
   Buntrock, Sebastian; Cai, Mingsheng; Chen, Wen; Conti, Lauro; Deng,
   Lei; Diebold, Sebastian; Fu, Shaojun; Guo, Jianhua; Hanke, Lars; Hong,
   Yilin; Kalkuhl, Christoph; Kappelmann, Norbert; Kaufmann, Thomas; Lei,
   Shijun; Li, Fu; Li, Xinfeng; Liu, Wei; Meyer, Kevin; Rauch, Thomas;
   Ruan, Ping; Schaadt, Daniel M.; Schanz, Thomas; Song, Qian; Stelzer,
   Beate; Wang, Zhanshan; Yang, Jianfeng; Zhang, Wei
2020SPIE11444E..07J    Altcode: 2020arXiv201207384J
  The CAFE (Census of warm-hot intergalactic medium, Accretion, and
  Feedback Explorer) and LyRIC (Lyman UV Radiation from Interstellar
  medium and Circum-galactic medium) have been proposed to the space
  agencies in China respectively. CAFE was first proposed as a joint
  scientific CAS-ESA small space mission in 2015. LyRIC was proposed as
  the independent external payload operating on the Chinese Space Station
  (CSS) in 2019. Both missions are dedicated to mapping the Lyman UV
  emissions ( ionized oxygen (O<SUB>VI</SUB>) resonance lines at 103.2
  and 103.8 nm, and Lyman series) for the diffuse sources either in
  our Galaxy or the circum-galactic mediums of the nearby galaxies. We
  present the primary science objectives, mission concepts, the enabling
  technologies, as well as the current status.

---------------------------------------------------------
Title: Hot Plasma Flows and Oscillations in the Loop-top Region
    During the 2017 September 10 X8.2 Solar Flare
Authors: Reeves, Katharine K.; Polito, Vanessa; Chen, Bin; Galan,
   Giselle; Yu, Sijie; Liu, Wei; Li, Gang
2020ApJ...905..165R    Altcode: 2020arXiv201012049R
  In this study, we investigate motions in the hot plasma above the
  flare loops during the 2017 September 10 X8.2 flare event. We examine
  the region to the south of the main flare arcade, where there is data
  from the Interface Region Imaging Spectrograph (IRIS) and the Extreme
  ultraviolet Imaging Spectrometer (EIS) on Hinode. We find that there are
  initial blueshifts of 20-60 km s<SUP>-1</SUP> observed in this region
  in the Fe XXI line in IRIS and the Fe XXIV line in EIS, and that the
  locations of these blueshifts move southward along the arcade over the
  course of about 10 minutes. The cadence of IRIS allows us to follow
  the evolution of these flows, and we find that at each location where
  there is an initial blueshift in the Fe XXI line, there are damped
  oscillations in the Doppler velocity with periods of ∼400 s. We
  conclude that these periods are independent of loop length, ruling
  out magnetoacoustic standing modes as a possible mechanism. Microwave
  observations from the Expanded Owens Valley Solar Array (EOVSA)
  indicate that there are nonthermal emissions in the region where the
  Doppler shifts are observed, indicating that accelerated particles
  are present. We suggest that the flows and oscillations are due to
  motions of the magnetic field that are caused by reconnection outflows
  disturbing the loop-top region.

---------------------------------------------------------
Title: Two distinct electron populations in the 2001 April 25 event
Authors: Li, G.; Zhao, L.; Wang, L.; Liu, W.; Wu, X.
2020AGUFMSH008..05L    Altcode:
  We examine the release times of energetic electrons in the 2001 April
  25 event. A M2.7 flare occurred in 2001 April 25, from AR09433,
  located at N18W09. The flare was observed in X-rays by GOES and
  the Yohkoh spacecraft. The Yohkoh observation also included hard
  X-ray images for all four energy channels: L, M1, M2, and H. We use
  Yohkoh observation times as a proxy for the release time of energetic
  electrons that propagated downward, which are responsible for the hard
  X-rays. In-situ &gt; ∼ 25 keV electrons were observed by the Wind
  spacecraft. For these electrons, we obtain the release time at the Sun
  using the recently developed Fractional Velocity Dispersion Analysis
  (FVDA) method. We find that the release times of outward propagating
  energetic electrons are clearly delayed from those that propagated
  downward. Furthermore, these delayed releases are energy dependent. The
  implication of this delay on the underlying acceleration and trapping
  process of the &gt; ∼ 25 keV electrons at solar flares is discussed.

---------------------------------------------------------
Title: Panoramic SETI: overall focal plane electronics and timing
    and network protocols
Authors: Liu, Wei; Werthimer, Dan; Lee, Ryan; Antonio, Franklin;
   Aronson, Michael; Brown, Aaron; Drake, Frank; Howard, Andrew;
   Horowitz, Paul; Maire, Jerome; Raffanti, Rick; Stone, Remington;
   Treffers, Richard; Wright, Shelley A.
2020SPIE11447E..7GL    Altcode: 2021arXiv211111476L
  The PANOSETI experiment is an all-sky, all-the-time visible search
  for nanosecond to millisecond time-scale transients. The experiment
  will deploy observatory domes at several sites, each dome containing
  ~45 telescopes and covering ~4,440 square degrees. Here we describe
  the focal-plane electronics for the visible wavelength telescopes,
  each of which contains a Mother Board and four Quadrant Boards. On each
  quadrant board, 256 silicon photomultiplier (SiPM) photon detectors are
  arranged to measure pulse heights to search for nanosecond time-scale
  pulses. To simultaneously examine pulse widths over a large range of
  time scales (nanoseconds to milliseconds), the instrument implements
  both a Continuous Imaging Mode (CI-Mode) and a Pulse Height Mode
  (PH-Mode). Precise timing is implemented in the gateware with the
  White Rabbit protocol.

---------------------------------------------------------
Title: Contribution of High-energy GRB Emissions to the Spectrum of
    the Isotropic Diffuse γ-Ray Background
Authors: Yao, Yu-Hua; Chang, Xiao-Chuan; Hu, Hong-Bo; Pan, Yi-Bin;
   Zhang, Hai-Ming; Li, Hua-Yang; Qiao, Bing-Qiang; Kang, Ming-Ming;
   Yang, Chao-Wen; Liu, Wei; Guo, Yi-Qing
2020ApJ...901..106Y    Altcode:
  High-precision measurement of the isotropic diffuse γ-ray background
  (IGRB) has been extrapolated to the TeV energy region using the
  Fermi-LAT experiment. Various kinds of astrophysical sources are
  candidates for its origin. However, a consensus on the dominant source
  has been difficult to reach. Recent observations of the γ-ray emission
  of γ-ray bursts (GRBs), denoted as the synchrotron self-Compton
  (SSC) component in the afterglow phase, in the sub-TeV energy region
  by MAGIC and HESS experiments shed new light on this topic. In this
  work, we revisit the contribution from the SSC component of GRBs to
  the IGRB. First, a sample set of GRB events is obtained and examined
  using observations from Fermi-LAT. Second, the SSC component,
  described by the energy ratio R<SUB>ext</SUB> and spectral index
  β<SUB>ext</SUB>, is assigned to every GRB event. We can obtain the
  total spectrum contribution based on this GRB sample. We find that
  when R<SUB>ext</SUB> and β<SUB>ext</SUB> reach ∼20% and -1.6,
  respectively, the contribution from GRB emission dominates in the
  energy region of hundreds of GeV. We hope that the LHAASO and CTA
  experiments under construction can observe a large number of GRBs to
  fix those parameters in coming years. A surviving tail is expected,
  which can serve to check our calculations based on future satellite
  experiments such as HERD and GAMMA400.

---------------------------------------------------------
Title: Identification of Two Distinct Electron Populations in an
    Impulsive Solar Energetic Electron Event
Authors: Li, G.; Zhao, L.; Wang, L.; Liu, W.; Wu, X.
2020ApJ...900L..16L    Altcode:
  We examine the release times of energetic electrons in the 2001 April
  25 event. An M2.7 flare occurred on 2001 April 25, from AR 09433,
  located at N18W09. The flare was observed in X-rays by GOES and the
  Yohkoh spacecraft. The Yohkoh observation also included hard X-ray (HXR)
  images for all four energy channels: L, M1, M2, and H. We use Yohkoh
  observation times as a proxy for the release time of energetic electrons
  that propagated downward, which are responsible for the HXRs. In situ
  &gt;∼25 keV electrons were observed by the Wind spacecraft. For
  these electrons, we obtain the release time at the Sun using the
  recently developed Fractional Velocity Dispersion Analysis method. We
  find that the release times of outward-propagating energetic electrons
  are clearly delayed from those that propagated downward. Furthermore,
  these delayed releases are energy dependent. The implication of this
  delay on the underlying acceleration and trapping process of the
  &gt;∼25 keV electrons at solar flares is discussed.

---------------------------------------------------------
Title: Major Scientific Challenges and Opportunities in Understanding
    Magnetic Reconnection and Related Explosive Phenomena in Solar and
    Heliospheric Plasmas
Authors: Ji, H.; Karpen, J.; Alt, A.; Antiochos, S.; Baalrud, S.;
   Bale, S.; Bellan, P. M.; Begelman, M.; Beresnyak, A.; Bhattacharjee,
   A.; Blackman, E. G.; Brennan, D.; Brown, M.; Buechner, J.; Burch, J.;
   Cassak, P.; Chen, B.; Chen, L. -J.; Chen, Y.; Chien, A.; Comisso,
   L.; Craig, D.; Dahlin, J.; Daughton, W.; DeLuca, E.; Dong, C. F.;
   Dorfman, S.; Drake, J.; Ebrahimi, F.; Egedal, J.; Ergun, R.; Eyink,
   G.; Fan, Y.; Fiksel, G.; Forest, C.; Fox, W.; Froula, D.; Fujimoto,
   K.; Gao, L.; Genestreti, K.; Gibson, S.; Goldstein, M.; Guo, F.; Hare,
   J.; Hesse, M.; Hoshino, M.; Hu, Q.; Huang, Y. -M.; Jara-Almonte, J.;
   Karimabadi, H.; Klimchuk, J.; Kunz, M.; Kusano, K.; Lazarian, A.; Le,
   A.; Lebedev, S.; Li, H.; Li, X.; Lin, Y.; Linton, M.; Liu, Y. -H.;
   Liu, W.; Longcope, D.; Loureiro, N.; Lu, Q. -M.; Ma, Z-W.; Matthaeus,
   W. H.; Meyerhofer, D.; Mozer, F.; Munsat, T.; Murphy, N. A.; Nilson,
   P.; Ono, Y.; Opher, M.; Park, H.; Parker, S.; Petropoulou, M.; Phan,
   T.; Prager, S.; Rempel, M.; Ren, C.; Ren, Y.; Rosner, R.; Roytershteyn,
   V.; Sarff, J.; Savcheva, A.; Schaffner, D.; Schoeffier, K.; Scime, E.;
   Shay, M.; Sironi, L.; Sitnov, M.; Stanier, A.; Swisdak, M.; TenBarge,
   J.; Tharp, T.; Uzdensky, D.; Vaivads, A.; Velli, M.; Vishniac, E.;
   Wang, H.; Werner, G.; Xiao, C.; Yamada, M.; Yokoyama, T.; Yoo, J.;
   Zenitani, S.; Zweibel, E.
2020arXiv200908779J    Altcode:
  Magnetic reconnection underlies many explosive phenomena in the
  heliosphere and in laboratory plasmas. The new research capabilities in
  theory/simulations, observations, and laboratory experiments provide the
  opportunity to solve the grand scientific challenges summarized in this
  whitepaper. Success will require enhanced and sustained investments
  from relevant funding agencies, increased interagency/international
  partnerships, and close collaborations of the solar, heliospheric,
  and laboratory plasma communities. These investments will deliver
  transformative progress in understanding magnetic reconnection and
  related explosive phenomena including space weather events.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Galactic interstellar ratio
    <SUP>18</SUP>O/<SUP>17</SUP>O. I.
Authors: Zhang, J. S.; Liu, W.; Yan, Y. T.; Yu, H. Z.; Liu, J. T.;
   Zheng, Y. H.; Romano, D.; Zhang, Z. -Y.; Wang, J. Z.; Chen, J. L.;
   Wang, Y. X.; Zhang, W. J.; Lu, H. H.; Chen, L. S.; Zou, Y. P.; Yang,
   H. Q.; Wen, T.; Lu, F. S.
2020yCat..22490006Z    Altcode:
  The C<SUP>18</SUP>O and C<SUP>17</SUP>O J=1-0 lines were observed
  from July 1, with the Institut de Radio Astronomie Millimetrique
  (IRAM) 30m single dish telescope, at the Pico Veleta Observatory
  (Granada, Spain). The center frequencies were set at 109.782182 and
  112.359277GHz for the C<SUP>18</SUP>O and C<SUP>17</SUP>O, respectively,
  with a corresponding beam size of ~23". With the IRAM 30m we observed
  50 sources of our sample. The parameters of their observations are
  summarized in Table 1. <P />Other observations of the J=1-0 lines of
  C<SUP>18</SUP>O and C<SUP>17</SUP>O were also carried out using the
  Arizona Radio Observatory (ARO) 12m telescope on Kitt Peak, Tuscon,
  AZ, USA, with a corresponding beam size of ~64". Observations were
  performed remotely from Guangzhou University, China, in 2016 November
  and December, 2017 January, November, and December, and 2018 May and
  December. <P />Table 1 presents the parameters of the observational
  results of ARO for the sample of 260 sources, including 24 sources
  observed by both IRAM 30m and ARO 12m telescopes. <P />(3 data files).

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Title: Galactic Interstellar Sulfur Isotopes: A Radial
    <SUP>32</SUP>S/<SUP>34</SUP>S Gradient?
Authors: Yu, H. Z.; Zhang, J. S.; Henkel, C.; Yan, Y. T.; Liu, W.;
   Tang, X. D.; Langer, N.; Luan, T. C.; Chen, J. L.; Wang, Y. X.; Deng,
   G. G.; Zou, Y. P.
2020ApJ...899..145Y    Altcode: 2020arXiv200804916Y
  We present observations of <SUP>12</SUP>C<SUP>32</SUP>S,
  <SUP>12</SUP>C<SUP>34</SUP>S, <SUP>13</SUP>C<SUP>32</SUP>S,
  and <SUP>12</SUP>C<SUP>33</SUP>S J = 2-1 lines toward a large
  sample of massive star-forming regions by using the Arizona
  Radio Observatory 12 m telescope and the IRAM 30 m. Taking new
  measurements of the carbon <SUP>12</SUP>C/<SUP>13</SUP>C ratio, the
  <SUP>32</SUP>S/<SUP>34</SUP>S isotope ratio was determined from the
  integrated <SUP>13</SUP>C<SUP>32</SUP>S/<SUP>12</SUP>C<SUP>34</SUP>S
  line intensity ratios for our sample. Our analysis shows a
  <SUP>32</SUP>S/<SUP>34</SUP>S gradient from the inner Galaxy out to
  a galactocentric distance of 12 kpc. An unweighted least-squares
  fit to our data yields <SUP>32</SUP>S/<SUP>34</SUP>S = (1.56 ±
  0.17)D<SUB>GC</SUB> + (6.75 ± 1.22) with a correlation coefficient
  of 0.77. Errors represent 1σ standard deviations. Testing this
  result by (a) excluding the Galactic center region, (b) excluding all
  sources with C<SUP>34</SUP>S opacities &gt;0.25, (c) combining our
  data and old data from previous study, and (d) using different sets
  of carbon isotope ratios leads to the conclusion that the observed
  <SUP>32</SUP>S/<SUP>34</SUP>S gradient is not an artifact but persists
  irrespective of the choice of sample and carbon isotope data. A gradient
  with rising <SUP>32</SUP>S/<SUP>34</SUP>S values as a function of
  galactocentric radius implies that the solar system ratio should be
  larger than that of the local interstellar medium. With the new carbon
  isotope ratios, we indeed obtain a local <SUP>32</SUP>S/<SUP>34</SUP>S
  isotope ratio about 10% below the solar system one, as expected in the
  case of decreasing <SUP>32</SUP>S/<SUP>34</SUP>S ratios with time and
  increased amounts of stellar processing. However, taking older carbon
  isotope ratios based on a lesser amount of data, such a decrease is
  not seen. No systematic variation of <SUP>34</SUP>S/<SUP>33</SUP>S
  ratios along galactocentric distance was found. The average value is
  5.9 ± 1.5, the error denoting the standard deviation of an individual
  measurement.

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Title: Electron and positron spectra in three-dimensional
    spatial-dependent propagation model
Authors: Tian, Zhen; Liu, Wei; Yang, Bo; Fu, Xue-Dong; Xu, Hai-Bo;
   Yao, Yu-Hua; Guo, Yi-Qing
2020ChPhC..44h5102T    Altcode: 2019arXiv190410663T
  The spatial-dependent propagation (SDP) model has been demonstrated
  to account for the spectral hardening of both primary and secondary
  Cosmic Rays (CRs) nuclei above about 200 GV. In this work, we further
  apply this model to the latest AMS-02 observations of electrons and
  positrons. To investigate the effect of different propagation models,
  both homogeneous diffusion and SDP are compared. In contrast to the
  homogeneous diffusion, SDP brings about harder spectra of background
  CRs and thus enhances background electron and positron fluxes
  above tens of GeV. Thereby, the SDP model could better reproduce
  both electron and positron energy spectra when introducing a local
  pulsar. The influence of the background source distribution is also
  investigated, where both axisymmetric and spiral distributions are
  compared. We find that considering the spiral distribution leads to
  a larger contribution of positrons for energies above multi-GeV than
  the axisymmetric distribution. In the SDP model, when including a
  spiral distribution of sources, the all-electron spectrum above TeV
  energies is thus naturally described. In the meantime, the estimated
  anisotropies in the all-electrons spectrum show that in contrary to the
  homogeneous diffusion model, the anisotropy under SDP is well below
  the observational limits set by the Fermi-LAT experiment, even when
  considering a local source. * Supported by the National Key Research
  and Development Program of China (2016YFA0400200), the National Natural
  Science Foundation of China (11875264, 11635011, 11761141001, 11663006)

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Title: Indirect measurement of the 57.7 keV resonance strength
    for the astrophysical γ -ray source of the <SUP>25</SUP>Mg(p ,γ
    )<SUP>26</SUP>Al reaction
Authors: Li, Y. J.; Li, Z. H.; Li, E. T.; Li, X. Y.; Ma, T. L.; Shen,
   Y. P.; Liu, J. C.; Gan, L.; Su, Y.; Qiao, L. H.; Han, Z. Y.; Zhou,
   Y.; Su, J.; Yan, S. Q.; Zeng, S.; Wang, Y. B.; Guo, B.; Lian, G.;
   Nan, D.; Bai, X. X.; Liu, W. P.
2020PhRvC.102b5804L    Altcode:
  <SUP>25</SUP>Mg(p ,γ )<SUP>26</SUP>Al is the most important reaction
  in the Mg-Al cycle in the hydrogen burning regions of stars. Its
  cross sections at stellar energies are essential to understand
  the issues of radioactive <SUP>26</SUP>Al in the galaxy and
  meteorites. The 57.7 keV resonance dominate the <SUP>25</SUP>Mg(p
  ,γ )<SUP>26</SUP>Al astrophysical reaction rates at relative
  low temperature, but it is very difficult to measure its resonance
  strength directly, and the indirect measurement results deviate by a
  factor of about 2 by far. In this work, the angular distributions of
  <SUP>25</SUP>Mg(<SUP>7</SUP>Li,<SUP>6</SUP>He)<SUP>26</SUP>Al leading
  to 6.364 MeV and eleven low-lying states in <SUP>26</SUP>Al have
  been measured by the Q3D magnetic spectrometer of the HI-13 tandem
  accelerator. The spectroscopic factors were derived and used to deduce
  the proton width and 57.7 keV resonance strength. The astrophysical
  <SUP>25</SUP>Mg(p ,γ )<SUP>26</SUP>Al reaction rates at stellar
  energies have been updated by using the present result.

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Title: Method for retrieval of atmospheric water vapor using OH
    airglow for correction of astronomical observations
Authors: Xu, J. Y.; Liu, W. J.; Bian, J. C.; Liu, X.; Yuan, W.;
   Wang, C.
2020A&A...639A..29X    Altcode:
  Context. Water vapor in the atmosphere undergoes quick spatial
  and temporal variations. This has a serious impact on ground-based
  astronomical observations from the visible band to the infrared band
  resulting from water vapor attenuation and emission. <BR /> Aims: We
  seek to show how the sky spectrum of an astronomical observation can be
  used to determine the amount of precipitable water vapor (PWV) along the
  line of sight toward the science target. <BR /> Methods: In this work,
  we discuss a method to retrieve the PWV from the OH(8-3) band airglow
  spectrum. We analyzed the influences of the pressure and temperature
  of the atmosphere and the different water vapor vertical distributions
  on the PWV retrieval method in detail. Meanwhile, the accuracy of
  the method was analyzed via Monte Carlo simulations. To further
  verify the method of PWV retrieval, we carried out cross comparisons
  between the PWV retrieved from OH airglow and PWV from the standard
  star spectra of UVES using equivalent widths of telluric absorption
  lines observed from 2000 to 2016 at Cerro Paranal in Chile. <BR />
  Results: The Monte Carlo tests and the comparison between the two
  different methods prove the availability the PWV retrieval method
  from OH airglow. These results show that using OH airglow spectra
  in astronomical observations, PWVs along the same line of sight as
  the astronomical observations can be retrieved in real time. <BR />
  Conclusions: We provide a quick and economical method for retrieving the
  water vapor along the same line of sight of astronomical observation
  in the real time. This is especially helpful to correcting the effect
  of water vapor on astronomical observations.

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Title: Studies of drag-free control methods for
    space-basedgravitational-wave detection
Authors: GAO, Yang; LIU, Wei
2020SSPMA..50g9503G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Astrophysical <SUP>22</SUP>Mg(p, γ)<SUP>23</SUP>Al
    reaction rates from asymptotic normalization coefficient of
    <SUP>23</SUP>Ne→<SUP>22</SUP>Ne+n
Authors: Li, Xin-Yue; Guo, Bing; Li, Zhi-Hong; Liu, Wei-Ping
2020ChPhC..44g4001L    Altcode:
  The radionuclide <SUP>22</SUP>Na generates the emission of a
  characteristic 1.275 MeV $\gamma$?--&gt; -ray. This is a potential
  astronomical observable, whose occurrence is suspected in classical
  novae. The $^{22}{{\rm{Mg}}}(p,\,\gamma)^{23}{{\rm{Al}}}$?--&gt;
  reaction is relevant to the nucleosynthesis of <SUP>22</SUP>Na in
  Ne-rich novae. In this study, employing the adiabatic distorted wave
  approximation and continuum discretized coupled channel methods,
  the squared neutron asymptotic normalization coefficients
  (ANCs) for the virtual decay of $^{23}{{\rm{Ne}}}$?--&gt;
  $\to$?--&gt; $^{22}{{\rm{Ne}}}$?--&gt; + n were extracted,
  and determined as $(0.483\pm0.060)$?--&gt; fm<SUP>-1</SUP> and
  $(9.7\pm2.3)$?--&gt; fm<SUP>-1</SUP> for the ground state and the
  first excited state from the experimental angular distributions
  of ${}^{22}{{\rm{Ne}}}(d,\,p){}^{23}{{\rm{Ne}}}$?--&gt;
  populating the ground state and the first excited state of
  $^{23}{{\rm{Ne}}}$?--&gt; , respectively. Then, the squared proton
  ANC of ${}^{23}{{\rm{Al}}}_{\rm{g.s.}}$?--&gt; was obtained as
  $C_{d5/2}^{2}({}^{23}{{\rm{Al}}})=(2.65\pm0.33)\times10^{3}$?--&gt;
  fm<SUP>-1</SUP> according to the charge symmetry of
  the strong interaction. The astrophysical S-factors and
  reaction rates for the direct capture contribution in
  ${}^{22}{{\rm{Mg}}}(p,\,\gamma){}^{23}{{\rm{Al}}}$?--&gt;
  were also presented. Furthermore, the proton width of the
  first excited state of $^{23}{{\rm{Al}}}$?--&gt; was derived
  to be $(57\pm14)$?--&gt; eV from the neutron ANC of its mirror
  state in $^{23}{{\rm{Ne}}}$?--&gt; and used to compute the
  contribution from the first resonance of $^{23}{{\rm{Al}}}$?--&gt;
  . This result demonstrates that the direct capture dominates the
  $^{22}{{\rm{Mg}}}(p,\,\gamma)^{23}{{\rm{Al}}}$?--&gt; reaction at
  most temperatures of astrophysical relevance for $0.33 \lt T_9
  \lt 0.64$?--&gt; . * Supported by the National Key Research and
  Development Program of China (2016YFA0400502), the National Natural
  Science Foundation of China (11975316, 11490561, 11535004, 11775013),
  the Continuous Basic Scientific Research Project (WDJC-2019-13) and
  the 973 Program (2013CB834406)

---------------------------------------------------------
Title: A Systematic Observational Study on Galactic Interstellar Ratio
    <SUP>18</SUP>O/<SUP>17</SUP>O. I. C<SUP>18</SUP>O and C<SUP>17</SUP>O
    J = 1-0 Data Analysis
Authors: Zhang, J. S.; Liu, W.; Yan, Y. T.; Yu, H. Z.; Liu, J. T.;
   Zheng, Y. H.; Romano, D.; Zhang, Z. -Y.; Wang, J. Z.; Chen, J. L.;
   Wang, Y. X.; Zhang, W. J.; Lu, H. H.; Chen, L. S.; Zou, Y. P.; Yang,
   H. Q.; Wen, T.; Lu, F. S.
2020ApJS..249....6Z    Altcode: 2020arXiv200700361Z
  The interstellar oxygen isotopic ratio of <SUP>18</SUP>O/<SUP>17</SUP>O
  can reflect the relative amount of the secular enrichment by ejecta
  from high-mass versus intermediate-mass stars. Previous observations
  found a Galactic gradient of <SUP>18</SUP>O/<SUP>17</SUP>O,
  i.e., low ratios in the Galactic center and large values in the
  Galactic disk, which supports the inside-out formation scenario of
  our Galaxy. However, there are not many observed objects and, in
  particular, there are not many at large galactocentric distances. For
  this reason, we started a systematic study on Galactic interstellar
  <SUP>18</SUP>O/<SUP>17</SUP>O, through observations of C<SUP>18</SUP>O
  and C<SUP>17</SUP>O multi-transition lines toward a large sample of
  286 sources (at least one order of magnitude larger than previous
  ones), from the Galactic center region to the far outer Galaxy (∼22
  kpc). In this article, we present our observations of J = 1-0 lines
  of C<SUP>18</SUP>O and C<SUP>17</SUP>O, with the 12 m antenna of
  the Arizona Radio Observatory (ARO 12 m) and the Institut de Radio
  Astronomie Millimétrique (IRAM) 30 m telescopes. Among our IRAM 30 m
  sample of 50 targets, we detected successfully both C<SUP>18</SUP>O
  and C<SUP>17</SUP>O 1-0 lines for 34 sources. Similarly, our sample
  of 260 targets for ARO 12 m observations resulted in the detection of
  both lines for 166 sources. The C<SUP>18</SUP>O optical depth effect
  on our ratio results, evaluated by fitting results of C<SUP>17</SUP>O
  spectra with hyperfine components (assuming ${\tau }_{C18O}=4{\tau
  }_{C17O}$ ) and our radiative transfer and excitation model nonlocal
  thermodynamic equilibrium (non-LTE) model calculation for the strongest
  source, was found to be insignificant. Beam dilution does not seem to
  be a problem either, which was supported by the fact that there is no
  systematic variation between the isotopic ratio and the heliocentric
  distance, and ratios are consistently measured from two telescopes
  for most of those detected sources. With this study we obtained
  <SUP>18</SUP>O/<SUP>17</SUP>O isotopic ratios for a large sample of
  molecular clouds with different galactocentric distances. Our results,
  though there are still very few detections made for sources in the outer
  Galaxy, confirm the apparent <SUP>18</SUP>O/<SUP>17</SUP>O gradient
  of <SUP>18</SUP>O/<SUP>17</SUP>O=(0.10 ± 0.03)R<SUB>GC</SUB>+(2.95 ±
  0.30), with a Pearson's rank correlation coefficient of R = 0.69. This
  is supported by the newest Galactic chemical evolution model including
  the impact of massive stellar rotators and novae. Our future J =
  2-1 and J = 3-2 observations of C<SUP>18</SUP>O and C<SUP>17</SUP>O
  toward the same sample would be important to determine their physical
  parameters (opacities, abundances, etc.) and further accurately
  determine the Galactic radial gradient of the isotopic ratio
  <SUP>18</SUP>O/<SUP>17</SUP>O.

---------------------------------------------------------
Title: Space target extraction and detection for wide-field
    surveillance
Authors: Liu, D.; Wang, X.; Xu, Z.; Li, Y.; Liu, W.
2020A&C....3200408L    Altcode:
  A wide-field surveillance system with a long exposure time has a
  stronger capability of space target detection. However, it also produces
  some complicated situations that make it difficult to detect space
  targets; some stars appear as streak-like sources, countless object
  points, and possible discontinuous or nonlinear target trajectories. We
  present a space target detection method with high detection probability
  and low computational cost to overcome these obstacles. Firstly, the
  improved adaptive threshold method and the omnidirectional morphological
  filtering method are implemented to remove stars and noise. Secondly,
  the relative inter frame motion distance can be used as the basis for
  predicting the valid state transition region in each image. Finally,
  a state transition multistage hypothesis testing method is proposed
  to detect targets with linear, nonlinear, continuous or discontinuous
  trajectories. As demonstrated by the experimental results in simulated
  image sequences and real image sequences, the proposed algorithm can
  effectively detect space targets in wide-field surveillance with
  long exposure time, and has a high detection probability and low
  computational cost.

---------------------------------------------------------
Title: An Empirical Power Density-Based Friction Law and Its
    Implications for Coherent Landslide Mobility
Authors: Deng, Yu; Yan, Shuaixing; Scaringi, Gianvito; Liu, Wei;
   He, Siming
2020GeoRL..4787581D    Altcode:
  The evolution of the shear resistance at the base of a
  coherent landslide body can effectively control its dynamic
  behavior. High-velocity rotary shear experiments have allowed
  scientists to explore stress-strain conditions close to those found
  in large landslides and faults. These experiments have led to two
  alternative models being proposed, which describe the evolution
  of the shear resistance through friction laws that depend either on
  normal stress or on velocity. Here, we discuss an integrated approach,
  first proposed to study seismic fault behavior, that reconciles these
  two models under a single parameter—the power density—which we
  utilize for the first time to investigate landslide dynamics. Using
  thermodynamic and process-based considerations, different soil and
  rock types can be related to different weakening mechanisms, which in
  turn can determine different landslide behaviors.

---------------------------------------------------------
Title: Entanglement-based secure quantum cryptography over 1,120
    kilometres
Authors: Yin, Juan; Li, Yu-Huai; Liao, Sheng-Kai; Yang, Meng; Cao,
   Yuan; Zhang, Liang; Ren, Ji-Gang; Cai, Wen-Qi; Liu, Wei-Yue; Li,
   Shuang-Lin; Shu, Rong; Huang, Yong-Mei; Deng, Lei; Li, Li; Zhang,
   Qiang; Liu, Nai-Le; Chen, Yu-Ao; Lu, Chao-Yang; Wang, Xiang-Bin; Xu,
   Feihu; Wang, Jian-Yu; Peng, Cheng-Zhi; Ekert, Artur K.; Pan, Jian-Wei
2020Natur.582..501Y    Altcode:
  Quantum key distribution (QKD)<SUP>1-3</SUP> is a theoretically
  secure way of sharing secret keys between remote users. It has been
  demonstrated in a laboratory over a coiled optical fibre up to 404
  kilometres long<SUP>4-7</SUP>. In the field, point-to-point QKD has been
  achieved from a satellite to a ground station up to 1,200 kilometres
  away<SUP>8-10</SUP>. However, real-world QKD-based cryptography targets
  physically separated users on the Earth, for which the maximum distance
  has been about 100 kilometres<SUP>11,12</SUP>. The use of trusted
  relays can extend these distances from across a typical metropolitan
  area<SUP>13-16</SUP> to intercity<SUP>17</SUP> and even intercontinental
  distances<SUP>18</SUP>. However, relays pose security risks, which
  can be avoided by using entanglement-based QKD, which has inherent
  source-independent security<SUP>19,20</SUP>. Long-distance entanglement
  distribution can be realized using quantum repeaters<SUP>21</SUP>,
  but the related technology is still immature for practical
  implementations<SUP>22</SUP>. The obvious alternative for extending
  the range of quantum communication without compromising its security
  is satellite-based QKD, but so far satellite-based entanglement
  distribution has not been efficient<SUP>23</SUP> enough to support
  QKD. Here we demonstrate entanglement-based QKD between two ground
  stations separated by 1,120 kilometres at a finite secret-key rate of
  0.12 bits per second, without the need for trusted relays. Entangled
  photon pairs were distributed via two bidirectional downlinks from
  the Micius satellite to two ground observatories in Delingha and
  Nanshan in China. The development of a high-efficiency telescope and
  follow-up optics crucially improved the link efficiency. The generated
  keys are secure for realistic devices, because our ground receivers
  were carefully designed to guarantee fair sampling and immunity to all
  known side channels<SUP>24,25</SUP>. Our method not only increases the
  secure distance on the ground tenfold but also increases the practical
  security of QKD to an unprecedented level.

---------------------------------------------------------
Title: Prospects for a multi-TeV gamma-ray sky survey with the LHAASO
    water Cherenkov detector array
Authors: Aharonian, F.; Alekseenko, V.; An, Q.; Axikegu; Bai, L. X.;
   Bao, Y. W.; Bastieri, D.; Bi, X. J.; Cai, H.; Cao, Zhe; Cao, Zhen;
   Chang, J.; Chang, J. F.; Chang, X. C.; Chao, S. P.; Chen, B. M.;
   Chen, J.; Chen, L.; Chen, L.; Chen, M. L.; Chen, M. J.; Chen, Q. H.;
   Chen, S. H.; Chen, S. Z.; Chen, T. L.; Chen, X. L.; Chen, Y.; Cheng,
   N.; Cheng, Y. D.; Cui, S. W.; Cui, X. H.; Cui, Y. D.; Dai, B. Z.;
   Dai, H. L.; Dai, Z. G.; Danzengluobu; D'Ettorre Piazzoli, B.; Fang,
   J.; Fan, J. H.; Fan, Y. Z.; Feng, C. F.; Feng, L.; Feng, S. H.; Feng,
   Y. L.; Gao, B.; Gao, Q.; Gao, W.; Ge, M. M.; Geng, L. S.; Gong, G. H.;
   Gou, Q. B.; Gu, M. H.; Guo, Y. Q.; Guo, Y. Y.; Han, Y. A.; He, H. H.;
   He, J. C.; Heller, M.; He, S. L.; He, Y.; Hou, C.; Huang, D. H.;
   Huang, Q. L.; Huang, W. H.; Huang, X. T.; Hu, H. B.; Hu, S.; Jia,
   H. Y.; Jiang, K.; Ji, F.; Jin, C.; Ji, X. L.; Levochkin, K.; Liang,
   E. W.; Liang, Y. F.; Li, Cheng; Li, Cong; Li, F.; Li, H.; Li, H. B.;
   Li, H. C.; Li, H. M.; Li, J.; Li, K.; Li, W. L.; Li, X.; Li, X. R.;
   Li, Y.; Li, Z.; Li, Z.; Liu, B.; Liu, C.; Liu, D.; Liu, H. D.; Liu,
   H.; Liu, J.; Liu, J. Y.; Liu, M. Y.; Liu, R. Y.; Liu, S. M.; Liu, W.;
   Liu, Y. N.; Liu, Z. X.; Long, W. J.; Lu, R.; Lv, H. K.; Ma, B. Q.; Ma,
   L. L.; Mao, J. R.; Masood, A.; Ma, X. H.; Mitthumsiri, W.; Montaruli,
   T.; Nan, Y. C.; Pattarakijwanich, P.; Pei, Z. Y.; Qiao, B. Q.; Qi,
   M. Y.; Ruffolo, D.; Rulev, V.; Sáiz, A.; Shao, L.; Shchegolev, O.;
   Sheng, X. D.; Shi, J. R.; Stenkin, Y.; Stepanov, V.; Sun, Z. B.; Tam,
   P. H. T.; Tang, Z. B.; Tian, W. W.; Volpe, D. D.; Wang, C.; Wang, H.;
   Wang, H. G.; Wang, J. C.; Wang, L. Y.; Wang, W.; Wang, W.; Wang, X. G.;
   Wang, X. Y.; Wang, X. J.; Wang, Y. D.; Wang, Y. J.; Wang, Y. N.; Wang,
   Y. P.; Wang, Z.; Wang, Z. H.; Wang, Z. X.; Wei, D. M.; Wei, J. J.;
   Wen, T.; Wu, C. Y.; Wu, H. R.; Wu, S.; Wu, W. X.; Wu, X. F.; Xiang,
   G. M.; Xiao, G.; Xin, G. G.; Xing, Y.; Xu, R. X.; Xue, L.; Yan, D. H.;
   Yang, C. W.; Yang, F. F.; Yang, L. L.; Yang, M. J.; Yang, R. Z.; Yang,
   S. B.; Yao, Y. H.; Yao, Z. G.; Ye, Y. M.; Yin, L. Q.; Yin, N.; You,
   X. H.; You, Z. Y.; Yuan, Q.; Yu, Y. H.; Jiang, Z. J.; Zeng, H. D.;
   Zeng, T. X.; Zeng, W.; Zeng, Z. K.; Zha, M.; Zhang, B. B.; Zhang,
   H. M.; Zhang, H. Y.; Zhang, J. L.; Zhang, J. W.; Zhang, L.; Zhang,
   P. F.; Zhang, P. P.; Zhang, S. R.; Zhang, S. S.; Zhang, X.; Zhang,
   X. P.; Zhang, Yi; Zhang, Yong; Zhang, Y. F. G.; Zhao, B.; Zhao, J.;
   Zhao, L.; Zhao, L. Z.; Zheng, F.; Zheng, Y.; Zhou, J. N.; Zhou, P.;
   Zhou, R.; Zhou, X. X.; Zhu, C. G.; Zhu, F. R.; Zhu, H.; Zhu, K. J.;
   Zuo, X.; LHAASO Collaboration
2020ChPhC..44f5001A    Altcode: 2020arXiv200204819G
  The Water Cherenkov Detector Array (WCDA) is a major component of
  the Large High Altitude Air Shower Array Observatory (LHAASO), a new
  generation cosmic-ray experiment with unprecedented sensitivity,
  currently under construction. WCDA is aimed at the study of
  TeV $\gamma$?--&gt; -rays. In order to evaluate the prospects of
  searching for TeV $\gamma$?--&gt; -ray sources with WCDA, we present a
  projection of the one-year sensitivity of WCDA to TeV $\gamma$?--&gt;
  -ray sources from TeVCat using an all-sky approach. Out of 128 TeVCat
  sources observable by WCDA up to a zenith angle of $45^\circ$?--&gt; ,
  we estimate that 42 would be detectable in one year of observations at
  a median energy of 1 TeV. Most of them are Galactic sources, and the
  extragalactic sources are Active Galactic Nuclei (AGN). * Supported by
  National Natural Science Foundation of China (11761141001, 11635011,
  11873005). The LHAASO project is supported by the National Key R &amp;
  D Program of China (2018YFA0404200), the Chinese Academy of Sciences,
  the Key Laboratory of Particle Astrophysics, IHEP, CAS

---------------------------------------------------------
Title: Best focus approach of HinOTORI telescope
Authors: Liu, Wei; Nagashima, Hiroki; Kawabata, Koji; Sasada, Mahito;
   Yao, Yongqiang; Shi, Shengcai
2020SPIE11455E..1TL    Altcode:
  HinOTORI is a 50cm telescope which is co-constructed and shared by
  China and Japan. It can image in u', Rc and Ic bands simultaneously,
  its main scientific observation targets are gravitational waves (GWs)
  optical counterparts (OTs). The installation of the telescope has been
  finished, and the engineering first light observation was carried out in
  May 2018. This paper will give an overall introduction and parameters
  of the telescope and then concentrate on a focusing method, which aims
  at obtaining the best focus position from the fitting equation. The
  reason of the best position shifting is also discussed.

---------------------------------------------------------
Title: Constraining the External Capture to the <SUP>16</SUP>O
    Ground State and the E 2 S Factor of the <SUP>12</SUP>C (α ,γ
    )<SUP>16</SUP>O Reaction
Authors: Shen, Y. P.; Guo, B.; deBoer, R. J.; Li, Z. H.; Li, Y. J.;
   Tang, X. D.; Pang, D. Y.; Adhikari, S.; Basu, C.; Su, J.; Yan, S. Q.;
   Fan, Q. W.; Liu, J. C.; Chen, C.; Han, Z. Y.; Li, X. Y.; Lian, G.;
   Ma, T. L.; Nan, W.; Nan, W. K.; Wang, Y. B.; Zeng, S.; Zhang, H.;
   Liu, W. P.
2020PhRvL.124p2701S    Altcode:
  The <SUP>12</SUP>C (α ,γ )<SUP>16</SUP>O reaction is one of the most
  crucial reactions in nuclear astrophysics. The E 2 external capture to
  the <SUP>16</SUP>O ground state (GS) has not been emphasized in previous
  analyses but may make a significant contribution to the <SUP>12</SUP>C
  (α ,γ )<SUP>16</SUP>O cross section depending on the value of the
  GS asymptotic normalization coefficient (ANC). In the present work,
  we determine this ANC to be 337 ±45 fm<SUP>-1 /2</SUP> through the
  <SUP>12</SUP>C (<SUP>11</SUP>B, <SUP>7</SUP>Li) <SUP>16</SUP>O reaction
  using a high-precision magnetic spectrograph. This sheds light on
  the existing large discrepancy of more than 2 orders of magnitude
  between the previously reported ANC values. Based on the new ANC, we
  experimentally constrain the GS external capture and show that through
  interference with the high energy tail of the 2<SUP>+</SUP> subthreshold
  state, a substantial enhancement in the GS S<SUB>E 2</SUB>(300 ) factor
  can be obtained (70 ±7 keV b ) compared to that of a recent review
  (45 keV b), resulting in an increase of the total S factor from 140 to
  162 keV b, which is now in good agreement with the value obtained by
  reproducing supernova nucleosynthesis calculations with the solar-system
  abundances. This work emphasizes that the external capture contribution
  for the ground state transition cannot be neglected in future analyses
  of the <SUP>12</SUP>C(α ,γ )<SUP>16</SUP>O reaction.

---------------------------------------------------------
Title: Deep Learning for Supernova Remnants Detection and Localization
Authors: Liu, W.; Yu, X. C.; Wang, B. Y.
2020ASPC..522..451L    Altcode: 2020adass..27..451L
  Detecting candidates of supernova remnants (SNRs) in the interstellar
  medium is a challenging task because SNRs have weak radio signals
  and irregular shapes. The use of a convolutional neural network is a
  deep learning method that can help us extract various features from
  images. To extract SNRs from astronomical images and estimate the
  positions of SNR candidates, we design the SNR-Net model composed
  of a training component and a detection component. In addition,
  migration learning is used to initialize the network parameters, which
  improves the speed and accuracy of network training.To accelerate the
  scientific computing process, we take advantage of innovative hardware
  architecture, such as deep learning optimized graphics processing units,
  which increase the speed of computation by a factor of 5. A case study
  suggests that SNR-Net may be applicable to detecting extended sources
  in the images automatically.

---------------------------------------------------------
Title: Carbon and nutrient export from intertidal sand systems
    elucidated by <SUP>224</SUP>Ra/<SUP>228</SUP>Th disequilibria
Authors: Cai, Pinghe; Wei, Lin; Geibert, Walter; Koehler, Dennis;
   Ye, Ying; Liu, Wei; Shi, Xiangming
2020GeCoA.274..302C    Altcode:
  We propose an alternative scheme for the use of
  <SUP>224</SUP>Ra/<SUP>228</SUP>Th disequilibria to investigate
  carbon and nutrient export from a permeable sandy seabed. Sediment
  profiles of dissolved <SUP>224</SUP>Ra, total <SUP>224</SUP>Ra
  and <SUP>228</SUP>Th were determined at two different intertidal
  sand systems - an intertidal sandy beach near Weitou Bay in Fujian
  (China), and a tidal sand flat in the Wadden Sea near Cuxhaven
  (Germany). Dramatic deficit of total <SUP>224</SUP>Ra relative to
  <SUP>228</SUP>Th was identified in the upper 20 or 30 cm sand layer
  over the sand systems. We construct a simple two-dimensional advective
  cycling model to simulate interfacial fluid transport in a sand system
  that is subject to periodic tidal inundation and swash actions. Based on
  the <SUP>224</SUP>Ra/<SUP>228</SUP>Th disequilibria in the sediment,
  the model gives estimates of 20.3, 9.1, and 1.9 L m<SUP>-2</SUP>
  h<SUP>-1</SUP> for water exchange flux at the high tide, mid-tide, and
  low tide position over the sandy beach at Weitou Bay, respectively. In
  comparison, the model provides an estimate of 7.2 L m<SUP>-2</SUP>
  h<SUP>-1</SUP> for water exchange flux at the tidal sand flat in the
  Wadden Sea. <P />The production of dissolved inorganic carbon (DIC) in
  porewater is the rate-limiting step for DIC export from the sandy beach
  into the sea, and can be reasonably simulated as a first-order kinetic
  reaction. The pattern of interfacial fluid transport over the beach
  facilitates a horizontal zonation of redox condition in the sediment,
  which evolves progressively from a fully oxic state at the high tide
  position to a suboxic state at the low tide position. There is clear
  evidence of nitrogen loss via denitrification in the suboxic status,
  and we estimate a nitrogen removal rate of 3.3 mmolN m<SUP>-2</SUP>
  d<SUP>-1</SUP> at this site. For the two intertidal sand systems,
  DIC export fluxes range from 20.1 to 89.4 mmolC m<SUP>-2</SUP>
  d<SUP>-1</SUP>, comparable in magnitude to fluxes determined in organic
  rich estuarine sediments. In the meantime, export fluxes of dissolved
  inorganic nitrogen (DIN) change from 0.8 to 18.6 mmolN m<SUP>-2</SUP>
  d<SUP>-1</SUP>. Overall, this study suggests that the role of sandy
  sediments in the biogeochemical cycling of carbon and nutrients needs
  to be revisited.

---------------------------------------------------------
Title: Optical telescope with Cassegrain metasurfaces
Authors: Liu, Xuan; Deng, Junhong; Li, King Fai; Jin, Mingke; Tang,
   Yutao; Zhang, Xuecai; Cheng, Xing; Wang, Hong; Liu, Wei; Li, Guixin
2020Nanop...9...12L    Altcode:
  The Cassegrain telescope, made of a concave primary mirror and a
  convex secondary mirror, is widely utilized for modern astronomical
  observation. However, the existence of curved mirrors inevitably
  results in bulky configurations. Here, we propose a new design of the
  miniaturized Cassegrain telescope by replacing the curved mirrors with
  planar reflective metasurfaces. The focusing and imaging properties of
  the Cassegrain metasurface telescopes are experimentally verified for
  circularly polarized incident light at near infrared wavelengths. The
  concept of the metasurface telescopes can be employed for applications
  in telescopes working at infrared, Terahertz, and microwave and even
  radio frequencies.

---------------------------------------------------------
Title: Systematic observations on Galactic Interstellar isotope ratios
Authors: Zhang, J. S.; Yan, Y. T.; Liu, W.; Yu, H. Z.; Chen, J. L.;
   Henkel, C.
2020IAUGA..30..278Z    Altcode:
  We are performing systematic observation studies on the Galactic
  interstellar isotopic ratios, including <SUP>18</SUP>O/<SUP>17</SUP>O,
  <SUP>12</SUP>C/<SUP>13</SUP>C, <SUP>14</SUP>N/<SUP>15</SUP>N and
  <SUP>32</SUP>S/<SUP>34</SUP>S. Our strategy focuses on combination
  of multi-transition observation data toward large samples with
  different Galactocentric distances. Our preliminary results show
  positive Galactic radial gradients of <SUP>18</SUP>O/<SUP>17</SUP>O
  and <SUP>12</SUP>C/<SUP>13</SUP>C. In both cases, the ratio increases
  with the Galactocentric distance, which agrees with the inside-out
  scenario of our Galaxy. Observations of other isotopes such as
  <SUP>14</SUP>N/<SUP>15</SUP>N and <SUP>32</SUP>S/<SUP>34</SUP>S are
  on-going.

---------------------------------------------------------
Title: Major Scientific Challenges and Opportunities in Understanding
    Magnetic Reconnection and Related Explosive Phenomena throughout
    the Universe
Authors: Ji, H.; Alt, A.; Antiochos, S.; Baalrud, S.; Bale, S.;
   Bellan, P. M.; Begelman, M.; Beresnyak, A.; Blackman, E. G.; Brennan,
   D.; Brown, M.; Buechner, J.; Burch, J.; Cassak, P.; Chen, L. -J.;
   Chen, Y.; Chien, A.; Craig, D.; Dahlin, J.; Daughton, W.; DeLuca, E.;
   Dong, C. F.; Dorfman, S.; Drake, J.; Ebrahimi, F.; Egedal, J.; Ergun,
   R.; Eyink, G.; Fan, Y.; Fiksel, G.; Forest, C.; Fox, W.; Froula, D.;
   Fujimoto, K.; Gao, L.; Genestreti, K.; Gibson, S.; Goldstein, M.; Guo,
   F.; Hesse, M.; Hoshino, M.; Hu, Q.; Huang, Y. -M.; Jara-Almonte, J.;
   Karimabadi, H.; Klimchuk, J.; Kunz, M.; Kusano, K.; Lazarian, A.;
   Le, A.; Li, H.; Li, X.; Lin, Y.; Linton, M.; Liu, Y. -H.; Liu, W.;
   Longcope, D.; Loureiro, N.; Lu, Q. -M.; Ma, Z-W.; Matthaeus, W. H.;
   Meyerhofer, D.; Mozer, F.; Munsat, T.; Murphy, N. A.; Nilson, P.;
   Ono, Y.; Opher, M.; Park, H.; Parker, S.; Petropoulou, M.; Phan, T.;
   Prager, S.; Rempel, M.; Ren, C.; Ren, Y.; Rosner, R.; Roytershteyn,
   V.; Sarff, J.; Savcheva, A.; Schaffner, D.; Schoeffier, K.; Scime, E.;
   Shay, M.; Sitnov, M.; Stanier, A.; TenBarge, J.; Tharp, T.; Uzdensky,
   D.; Vaivads, A.; Velli, M.; Vishniac, E.; Wang, H.; Werner, G.; Xiao,
   C.; Yamada, M.; Yokoyama, T.; Yoo, J.; Zenitani, S.; Zweibel, E.
2020arXiv200400079J    Altcode:
  This white paper summarizes major scientific challenges and
  opportunities in understanding magnetic reconnection and related
  explosive phenomena as a fundamental plasma process.

---------------------------------------------------------
Title: Two Numerical Methods for the 3D Anisotropic Propagation of
    Galactic Cosmic Rays
Authors: Liu, Wei; Lin, Su-jie; Hu, Hong-bo; Guo, Yi-qing; Li, Ai-feng
2020ApJ...892....6L    Altcode: 2019arXiv190902908L
  Conventional cosmic-ray propagation models usually assume an isotropic
  diffusion coefficient to account for the random deflection of cosmic
  rays by the turbulent interstellar magnetic field. Such models very
  successfully explain many observational phenomena related to the
  propagation of Galactic cosmic rays, such as broken power-law energy
  spectra, secondary-to-primary ratios, etc. However, the isotropic
  diffusion presupposition is facing severe challenges from recent
  observations. In particular, such observations on the large-scale
  anisotropy of TeV cosmic rays show that the dipole direction differs
  from the prediction of the conventional model. One possible reason
  is that the large-scale regular magnetic field, which leads to an
  anisotropic diffusion of cosmic rays, has not been included in the model
  provided by the public numerical packages. In this work, we propose
  two numerical schemes to solve the three-dimensional anisotropic
  transport equation: the pseudo-source method and Hundsdorfer-Verwer
  scheme. Both methods are verified by reproducing the measured B/C and
  proton spectrum and the radial variation of spectral index expected by
  former 2D simulation. As a demonstration of the prediction capability,
  dipole anisotropy is also calculated by a toy simulation with a rough
  magnetic field.

---------------------------------------------------------
Title: Spot Model for Identifications of Periods in Asynchronous
    Polars
Authors: Wang, Qishan; Qian, Shengbang; Han, Zhongtao; Fang, Xiaohui;
   Zang, Lei; Liu, Wei
2020ApJ...892...38W    Altcode: 2020arXiv201113123W
  We improved the discless accretion models in Wynn &amp; King considering
  the effects of the changing aspect due to the white dwarf (WD) spin
  and the variable feeding intensity caused by the asynchronism, and set
  up a more general spot model that is not sensitive to the different
  forms of these effects and can be applied for the period analysis
  of the optical and X-ray light curve. The spot model can produce the
  power spectra compatible with the observations, and its simulations
  limit the ratio P<SUB>spin</SUB>/P<SUB>orb</SUB> &lt; 2 between the
  powers at the WD spin and the binary orbital frequencies, which is
  a strong criterion for identification of periods. Then we recognize
  the periods for CD Ind, BY Cam, and 1RXS J083842.1-282723. The spot
  model reveals a complex accretion geometry in the asynchronous polars
  (APs), which may indicate that the complex magnetic field causes their
  asynchronism. We think 1RXS J083842.1-282723 is a prepolar because of
  its highest asynchronism and stable light curve. Giving the unstable
  accretion process in APs, the period analysis of the long-term light
  curve will make the orbital signal prominent.

---------------------------------------------------------
Title: Rupture Process of the 26 May 2019 M<SUB>w</SUB> 8.0 Northern
    Peru Intermediate-Depth Earthquake and Insights Into Its Mechanism
Authors: Liu, Wei; Yao, Huajian
2020GeoRL..4787167L    Altcode:
  In the Nazca-South American subduction zone, the subducted slab is
  flattened beneath northern Andes, called the Peruvian flat slab. The
  2019 M<SUB>w</SUB> 8.0 northern Peru intermediate-depth normal-faulting
  earthquake occurred at the leading edge of the Peruvian flat slab, where
  the slab rebends and sinks into greater depths. Here we investigate
  this earthquake by back projection analysis and finite fault inversion
  using seismic waveforms at teleseismic distances. The rupture process
  indicates that this earthquake ruptured mainly along strike (353°)
  ~150 km north-northwestward within ~55 s (average rupture velocity
  ~2.7 km/s), resulting in two major slip areas with three high slip rate
  areas, which are consistent with three high-frequency energy radiation
  subevents. Our study suggests that such a heterogeneous rupture may be
  caused by slab bending forces and dehydration embrittlement associated
  with morphology of the slab.

---------------------------------------------------------
Title: Real-time abnormal light curve detection based on a Gated
    Recurrent Unit network
Authors: Yan, Rui-Qing; Liu, Wei; Zhu, Meng; Wang, Yi-Jing; Dai, Cong;
   Cao, Shuo; Wu, Kang; Liang, Yu-Chen; Yu, Xian-Chuan; Zhang, Meng-Fei
2020RAA....20....7Y    Altcode:
  Targeting the problem of high real-time requirements in astronomical
  data processing, this paper proposes a real-time early warning model
  for light curves based on a Gated Recurrent Unit (GRU) network. Using
  the memory function of the GRU network, a prediction model of the light
  curve is established, and the model is trained using the collected
  light curve data, so that the model can predict a star magnitude value
  for the next moment based on historical star magnitude data. In this
  paper,we calculate the difference between the model prediction value
  and the actual observation value and set a threshold. If the difference
  exceeds the set threshold, the observation value at the next moment is
  considered to be an abnormal value, and a warning is given. Astronomers
  can carry out further certification based on the early warning and in
  combinationwith other means of observation. Themethod proposed in this
  paper can be applied to real-time observations in time domain astronomy.

---------------------------------------------------------
Title: High-energy-density physics based on HIAF
Authors: Kang, Wei; Du, Yingchao; Cao, Shuchun; Zhao, Hongwei; Lei,
   Yu; Wang, Yuyu; He, Bin; Sheng, Lina; Song, Yuanhong; Xiao, Guoqing;
   Zhang, Yanning; Li, Fuli; Cheng, Rui; Wang, Younian; Zhang, Lin; Zhao,
   Zongqing; Yang, Jiancheng; Zhao, Quantang; Qi, Wei; Chen, Yanhong;
   Ma, Bubo; Wang, Xing; Hu, Zhanghu; Liu, Wei; Hoffmann, Dieter; Gao,
   Fei; Su, Youwu; Xu, Zhongfeng; Zhan, Wenlong; Zhang, Ya; Wu, Dong;
   Zhao, Xiaoying; Zhang, Xiaoan; Wan, Feng; Qi, Xin; Chen, Benzheng;
   Zhang, Zimin; Cao, Leifeng; Deng, Zhigang; Ren, Jieru; Huang, Wenhui;
   Yang, Jie; Zhou, Xianming; Zhou, Zheng; Li, Jinyu; Zhang, Shizheng;
   Zhou, Weimin; Yang, Lei; Zhao, Yongtao; Tang, Chuanxiang; Li, Jianxing
2020SSPMA..50k2004K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: X-ray merger shock and radio relic in Abell 1367
Authors: Ge, C.; Sun, M.; Liu, R.; Rudnick, L.; Sarazin, C.; Forman,
   W.; Jones, C.; Chen, H.; Liu, W.; Yagi, M.; Boselli, A.; Fossati,
   M.; Gavazzi, G.
2020AAS...23545904G    Altcode:
  Abell 1367 is a dynamically young galaxy cluster with at least two
  subclusters merging along the SE-NW direction. With the wide-field
  XMM-Newton mosaic, we discover a previously unknown merger shock at
  the NW edge of the cluster. This shock region also corresponds to a
  radio relic, which could be produced by the shock re-acceleration of
  pre-existing relativistic seed electrons. We suggest that some of the
  relativistic seed electrons originate from late-type, star-forming
  galaxies through stripping. We expect mergers in spiral-rich galaxy
  groups or proto-clusters to also generate radio relics in these systems.

---------------------------------------------------------
Title: Fluctuation and inertia
Authors: Shu, Liangsuo; Liu, Xiaokang; Cui, Kaifeng; Liu, Zhichun;
   Liu, Wei
2020NuPhB.95014873S    Altcode: 2018arXiv180110018S
  How the principle of inertia survives quantum fluctuations is an
  interesting question. Smolin has proposed a hypothesis that quantum
  fluctuations are in fact real statistical fluctuations. In this work,
  combining the works on Hawking-Unruh radiation and Jacobson's idea
  in his thermodynamics derivation of Einstein equation, we confirmed
  Smolin's guess: the quantum fluctuations leading to Hawking-Unruh
  radiation, satisfying the fluctuation theorem, are statistical
  fluctuations. Therefore, inertia is found to be a result of the
  second law of thermodynamics: the principle of entropy increases
  has the tendency to eliminate the effects of fluctuations and makes
  accelerated observers express inertia force.

---------------------------------------------------------
Title: A strange star scenario for the formation of isolated
    millisecond pulsars
Authors: Jiang, Long; Wang, Na; Chen, Wen-Cong; Li, Xiang-Dong; Liu,
   Wei-Min; Gao, Zhi-Fu
2020A&A...633A..45J    Altcode: 2019arXiv191111275J
  According to the recycling model, neutron stars in low-mass
  X-ray binaries were spun up to millisecond pulsars (MSPs), which
  indicates that all MSPs in the Galactic plane ought to be harbored
  in binaries. However, about 20% Galactic field MSPs are found to be
  solitary. To interpret this problem, we assume that the accreting
  neutron star in binaries may collapse and become a strange star when
  it reaches some critical mass limit. Mass loss and a weak kick induced
  by asymmetric collapse during the phase transition (PT) from neutron
  star to strange star can result in isolated MSPs. In this work, we use a
  population-synthesis code to examine the PT model. The simulated results
  show that a kick velocity of ∼60 km s<SUP>-1</SUP> can produce ∼6 ×
  10<SUP>3</SUP> isolated MSPs and birth rate of ∼6.6 × 10<SUP>-7</SUP>
  yr<SUP>-1</SUP> in the Galaxy, which is approximately in agreement
  with predictions from observations. For the purpose of comparisons
  with future observation, we also give the mass distributions of radio
  and X-ray binary MSPs, along with the delay time distribution.

---------------------------------------------------------
Title: Detection of GWAC Abnormal Light Transform Based on Sparse
    Autoencoder
Authors: Zhu, M.; Liu, W.; Yu, X. C.; Duan, F. Q.; Zhang, Y. G.
2020ASPC..527..563Z    Altcode: 2020adass..29..563Z
  The Geographic Wide Angle Camera Array (GWAC) is an important
  ground-based observation device for the Sino-French astronomical
  satellite project. It can get millions of light curves in just 15
  seconds every night. This gives GWAC the advantages of observation and
  research in gravitational microlenses (important probe observations
  of exoplanets), flare stars, unknown transient objects (Gravitational
  Wave Bursts). These transient sources have anomalous characteristics
  in light and appear infrequently. It is a challenging task to
  detect the celestial bodies with abnormal light from the observed
  light curve. In order to improve the unfavorable conditions of
  artificial interpretation of a light curve, such as low efficiency
  and unavoidable errors or omissions, this paper proposes a light
  curve anomaly detection method based on Sparse AutoEncoder (SAE). To
  prove the effectiveness of the proposed algorithm, we performed some
  experiments on the algorithm and compared it with K-means in terms
  of false positive rate and time consumption. We identified 3 types of
  unknown mutations and some individual outliers, which will be tracked
  for deeper analysis. Experimental results show that the method has
  better performance in anomaly detection.

---------------------------------------------------------
Title: Probing the solar corona with Sun-grazing comets: comparing
    MHDsimulations with EUV observations
Authors: Jia, Y. D.; Pesnell, W. D.; Liu, W.; Downs, C.; Bryans, P.
2019AGUFMSH13A..03J    Altcode:
  Sun -grazing comets can dive within one solar radii of the Sun
  's surface. The cometary materials expand along the comet's orbit,
  and undergo various stages of fierce thermal-chemical reactions on
  the scales of seconds to minutes. These reactions ionize cometary
  ions through successive charge states , which is revealed by certain
  emission lines in the AIA images. Such plasma reaction processes are
  significantly affected by the transient structures in the corona, and
  thus these structures are revealed by the structures and shapes of the
  comet tail. We combine three numerical models: a global corona model,
  particle transportation model, and cometary plasma interaction model
  into one framework to simulate the interaction of Sun -grazing comets
  in the low corona. In our framework, cometary ejecta are vaporized
  and then ionized via multiple channels, and then confined by the
  coronal magnetic field. Constrained by imaging observations of the
  and cometary interaction images, we apply our framework to trace back
  to the local condition of the ambient corona, and its spatiotemporal
  variation. Previously, our model confirmed the importance of the
  ambient magnetic field vector in shaping the tail. In this study,
  we use the C/2011 W3 (Lovejoy) perihelion to determine the local
  plasma and field conditions in the corona. Our framework is capable of
  resolving structures from thousands of meters to tens of million meters,
  so we can identify the fine spatial variations in plasma density and
  magnetic field intensity, which may be visible in future/on-going
  close-up coronal observations.

---------------------------------------------------------
Title: Global Magnetohydrodynamics Simulation of EUV Waves and Shocks
    from the X8.2 Eruptive Flare on 2017 September 10
Authors: Jin, M.; Liu, W.; Cheung, C. M. M.; Nitta, N.; DeRosa,
   M. L.; Manchester, W.; Ofman, L.; Downs, C.; Petrosian, V.; Omodei,
   N.; Moschou, S. P.; Sokolov, I.
2019AGUFMSH32A..01J    Altcode:
  As one of the largest flare-CME eruptions during solar cycle 24, the
  2017 September 10 X8.2 flare event is associated with spectacular
  global EUV waves that transverse almost the entire visible solar
  disk, a CME with speed &gt; 3000 km/s, which is one of the fastest
  CMEs ever recorded, and &gt;100 MeV Gamma-ray emission lasting for
  more than 12 hours. All these unique observational features pose new
  challenge on current numerical models to reproduce the multi-wavelength
  observations. To take this challenge, we simulate the September 10
  event using a global MHD model (AWSoM: Alfven Wave Solar Model) within
  the Space Weather Modeling Framework and initiate CMEs by Gibson-Low
  flux rope. We assess several important observed and physical inputs
  (e.g., flux rope properties, polar magnetic field) in the model to
  better reproduce the multi-wavelength observations. We find that the
  simulated EUV wave morphology and kinematics are sensitive to the
  orientation of the initial flux rope introduced to the source active
  region. An orientation with the flux-rope axis in the north-south
  direction produces the best match to the observations, which suggests
  that EUV waves may potentially be used to constrain the flux-rope
  geometry for such limb or behind-the-limb eruptions that lack good
  magnetic field observations. By further combining with the white
  light and radio observations, we demonstrate the flux rope-corona
  interaction can greatly impact the early phase shock evolution (e.g.,
  geometry and shock parameters) therefore plays a significant role
  for particle acceleration near the Sun in this event. By propagating
  the CMEs into the heliosphere and beyond the Earth and Mars orbits, we
  compare the model results with the in-situ measurements and demonstrate
  the importance of input polar magnetic field on the realistic CME
  modeling therefore space weather forecasting.

---------------------------------------------------------
Title: On the nature of the X-ray outbursts in Be/X-ray binaries
Authors: Yan, Jingzhi; Liu, Wei; Zhang, Peng; Liu, Qingzhong
2019IAUS..346..146Y    Altcode:
  Be/X-ray binaries are a major subclass of high mass X-ray binaries. Two
  different X-ray outbursts are displayed in the X-ray light curves of
  such systems. It is generally believed that the X-ray outbursts are
  connected with the neutron star periastron passage of the circumstellar
  disk around the Be star. The optical emission of the Be star should
  be very important to understand the X-ray emission of the compact
  object. We have monitored several Be/X-ray binaries photometrically
  and spectroscopically in the optical band. The relationship between
  the optical emission and X-ray activity is described, which is very
  useful to explain the X-ray outbursts in Be/X-ray binaries.

---------------------------------------------------------
Title: Observations and simulations of electron flux oscillations
    in response to broadband ULF wave
Authors: Sarris, T. E.; Li, X.; Temerin, M. A.; Zhao, H.; Khoo, L. Y.;
   Liu, W.
2019AGUFMSM23F3272S    Altcode:
  It has recently been demonstrated through simulations and observations
  that electron flux oscillations are produced in the magnetosphere in
  association with broadband Ultra Low Frequency (ULF) waves. These
  oscillations are observed in the form of drift-periodic flux
  fluctuations, but are not associated with drift echoes following
  storm- or substorm-related energetic particle injections. They are
  observed in particular during quiet times, and it has been shown
  that they could indicate ongoing radial transport processes caused by
  ULF waves. It has also been shown that the width of electron energy
  channels is a critical parameter affecting the observed amplitude of
  flux oscillations, with narrower energy channel widths enabling the
  observation of higher-amplitude flux oscillations; this potentially
  explains why such features were not observed regularly before the Van
  Allen Probes era, as previous spacecraft generally had lower energy
  resolution. The amplitude of electric and magnetic fluctuations in
  the ULF range are directly related to the amplitude of the resulting
  flux oscillations. We extend these initial results by investigating
  analytic functions that can associate the observed flux oscillations
  with electric and magnetic fluctuations and with Phase Space Density
  gradients, both of which are expected to also affect radial transport
  rates.

---------------------------------------------------------
Title: Loop-top oscillations observed with IRIS spatially correlated
    with nonthermal emission from EOVSA in the September 10 2017 X8 Flare
Authors: Reeves, K.; Polito, V.; Galan, G.; Yu, S.; Chen, B.; Liu,
   W.; Li, G.
2019AGUFMSH13D3416R    Altcode:
  he September 10 2017 X8 flare was a spectacular limb event complete with
  a fast coronal mass ejection, a fully global EUV wave, a bright flare
  loop arcade, and strong emission ranging from microwave to white-light
  continuum and gamma-rays. We examine the IRIS Fe XXI data from this
  event. Fe XXI is a coronal line that is formed at about 10 MK. The IRIS
  pointing was just south of the main cusp-shaped loop structure visible
  in AIA, but it did capture most of the flare arcade on the limb. We find
  that the majority of the emission in the loops is slightly red shifted,
  with speeds of about 20 km/s, probably due to chromospheric evaporation
  and an inclined viewing angle. During the period from 16:05 - 16:15
  UT, we find that faint blue-shifted regions appear at the top of the
  flare loops, indicating plasma flows of 20-60 km/s. After the initial
  blue shift at each location, the Fe XXI Doppler velocities exhibit a
  damped oscillation with a period of about 40 sec. Interestingly, in
  the minutes before the blue-shifted loop-top emission was observed,
  the Expanded Owens Valley Solar Array observed nonthermal microwave
  emission at the same location above the loop-tops, possibly indicative
  of particle acceleration there. We will discuss possible mechanisms
  for these observations.

---------------------------------------------------------
Title: A new statistical study on the properties of cusp
Authors: Xiao, C.; Liu, W.
2019AGUFMSM51D3227X    Altcode:
  A statistical study of the mid- and high-altitude (2~9R<SUB>E</SUB>)
  cusp is conducted with nine years (2001~2009) of data from the
  Cluster spacecraft. The location, size and properties of the cusp
  region are studied statistically in this work. The survey shows that
  (1) the relations between X and Z are nearly linear for the poleward,
  the equatorward boundaries and the center of the cusp respectively,
  (2) the relationship between the cusp distance width in X direction
  and Z can be expressed by a quadratic function, (3) the cusp region
  is almost dawn-dusk symmetry for the distance width in X direction and
  dawn-dusk asymmetry for the latitudinal width (the difference between
  the invariant latitude of the poleward and the equatorward boundaries),
  and (4) by using a new orbit-sampling methodology to order the data
  in space, the statistical distributions of the magnetic field and
  plasma parameters (including ion density, temperature and speed) in
  XZ plane. The new cusp statistical method proposed in this work will
  provide reference for future cusp research.

---------------------------------------------------------
Title: On the Excitation of ULF Waves after Interplanetary
    Shock-induced Impulses
Authors: Zhang, D.; Liu, W.
2019AGUFMSM51C3203Z    Altcode:
  We study the generation of the ULF wave during shock-related
  sudden impulse in the Earth magnetosphere using Van Allen Probes
  measurement. Among the 63 shock-related sudden impulses, there
  are 39 cases with ULF wave induced and we find that in strong wave
  cases the impulse frequency appears correlated to the induced wave
  frequency which, at the same time, appears correlated to the local
  eigen frequency. Our results show that the shock-related ULF wave can
  be excited in the magnetosphere on condition that the shock-induced
  impulse frequency matches the local eigen frequency. We also find
  that the frequency of the first period of shock-related impulse is
  likely determined by the local fast-mode speed instead of local eigen
  frequency, which shows that the characteristic of the first impulse
  period is more likely related to a propagation mechanism rather than
  field-line resonance. A more detailed study using MMS measurement on
  how shock impulse propagates from solar wind into magnetosphere is
  in process.

---------------------------------------------------------
Title: Anisotropies of different mass compositions of cosmic rays
Authors: Qiao, Bing-Qiang; Liu, Wei; Guo, Yi-Qing; Yuan, Qiang
2019JCAP...12..007Q    Altcode: 2019arXiv190512505Q
  The spectral hardenings of cosmic ray nuclei above ~ 200 GV followed by
  softenings around 10 TV, the knee of the all-particle spectrum around
  PeV energies, as well as the pattern change of the amplitude and phase
  of the large-scale anisotropies around 100 TeV indicate the complexities
  of the origin and transportation of Galactic cosmic rays. It has been
  shown that nearby source(s) are most likely to be the cause of such
  spectral features of both the spectra and the anisotropies. In this
  work, we study the anisotropy features of different mass composition
  (or mass groups) of cosmic rays in this nearby source model. We show
  that even if the spectral features from the nearby source component
  is less distinctive compared with the background component from e.g.,
  the population of distant sources, the anisotropy features are more
  remarkable to be identified. Measurements of the anisotropies of each
  mass composition (group) of cosmic rays by the space experiments such
  as DAMPE and HERD and the ground-based experiments such as LHAASO in the
  near future are expected to be able to critically test this scenario.

---------------------------------------------------------
Title: Calculation of corotation electric field in the inner
    magnetosphere based on Van Allen Probes measurements
Authors: Liu, W.; Zhao, Z.
2019AGUFMSM51F3247L    Altcode:
  Corotation electric field is important in the inner magnetosphere
  topology, which was usually calculated by assuming 24h corotation
  period. However, some studies found that plasmasphere corotation
  lag exists which suggests the overestimation of corotation electric
  field in previous calculations. In this study, we use electric
  field measurements from Van Allen Probes mission from 2013 to 2017 to
  statistically calculate the distribution of large-scale electric field
  in the inner magnetosphere. A new method is subsequently developed to
  separate corotation electric field from convection electric field. Our
  research shows electric field is inversely proportional to the square
  of L, and, with the assumption of dipole magnetic field, the rotation
  period of plasmasphere is estimated as 27h, consistent with previous
  studies with EUV imaging of the plasmasphere. Based on the research,
  a new empirical model of innermagnetospheric corotation electric field
  was estibalished, which is significant for a more accurate understanding
  the large-scale electric field in the inner magnetosphere.

---------------------------------------------------------
Title: High-energy Observations of Solar Flares During Solar Cycle
    24th with the Fermi Large Area Telescope
Authors: Omodei, N.; Pesce-Rollins, M.; Longo, F.; Petrosian, V.;
   Liu, W.; Jin, M.
2019AGUFMSH12B..02O    Altcode:
  The Fermi Large Area Telescope (LAT) observations of the active Sun
  provide the largest sample of detected solar flares with emission
  greater than 30 MeV to date. These include detections of impulsive
  and hours-long sustained emission coincident with GOES X-ray flares as
  well as very fast Coronal Mass Ejections (CME). Of particular interest
  is the first detection of &gt;100 MeV gamma-ray emission from three
  solar flares whose positions behind the limb were confirmed by the
  STEREO spacecrafts and the 2017 September 10 X8.2 flare associated with
  Ground Level Enhancement 72. Fermi-LAT detections of solar flares at
  high energy present a unique opportunity to explore the mechanisms of
  high-energy emission and particle acceleration and transport in solar
  flares. We will review the Fermi-LAT observations of solar flares during
  Solar Cycle 24, including correlation studies with Solar Energetic
  Particles (SEP) and CMEs, and highlight possible interpretations and
  theoretical modeling.

---------------------------------------------------------
Title: Cooling Condensation at Coronal Null Points and
    Quasi-Separatrix Layers Involving Magnetic Reconnection
Authors: Liu, W.; Sun, X.; Yu, S.; Luna Bennasar, M.; Antolin, P.;
   Titov, V. S.; Downs, C.; Berger, T. E.
2019AGUFMSH11C3394L    Altcode:
  The solar corona, Sun's outer atmosphere, is million-degrees hot and
  tenuous. This hot plasma, under certain conditions, can enigmatically
  undergo a radiative cooling instability and condense into material of
  100 times cooler in the form of prominences or coronal rain. Where,
  when, and how such cooling condensation takes place remain poorly
  understood. Answers to these questions are not only of scientific
  importance in their own right, but also bear implications for the
  fundamental question of coronal heating and the chromosphere-corona
  mass cycle. Magnetic fields in the magnetized corona undoubtedly play
  a crucial role (e.g., by trapping the plasma), but where and how? We
  report recent imaging and spectroscopic observations from SDO/AIA/HMI
  and IRIS that can shed light on these puzzles. Through a systematic
  survey, we found that a large fraction of quiet-Sun condensations
  preferentially occur at the dips of coronal loops or funnels. Such dips
  are located at/near magnetic topological features, such as null points
  and quasi-separatrix layers (QSLs), which are regions characterized by
  high values of the squashing factor. We also identified evidence of
  magnetic reconnection at such locations, which can produce favorable
  conditions, e.g., density enhancement by compression and/or mass
  trapping in plasmoids, that can trigger run-away radiative cooling. We
  present proof-of-concept MHD simulations that demonstrate the role of
  reconnection in transporting cooled mass from overlying, long loops to
  underlying, short loops where it slide down as coronal rain. We will
  discuss the significance and broader implications of these results
  beyond solar physics.

---------------------------------------------------------
Title: Simulations and software development for the Hard X-ray Imager
    onboard ASO-S
Authors: Su, Yang; Liu, Wei; Li, You-Ping; Zhang, Zhe; Hurford,
   Gordon J.; Chen, Wei; Huang, Yu; Li, Zhen-Tong; Jiang, Xian-Kai;
   Wang, Hao-Xiang; Xia, Fan-Xiao-Yu; Chen, Chang-Xue; Yu, Wen-Hui; Yu,
   Fu; Wu, Jian; Gan, Wei-Qun
2019RAA....19..163S    Altcode:
  China’s first solar mission, the Advanced Space-based Solar
  Observatory (ASO-S), is now changing from Phase B to Phase C. Its
  main scientific objectives are summarized as ‘1M2B’, namely
  magnetic field and two types of bursts (solar flares and coronal
  mass ejections). Among the three scientific payloads, Hard X-ray
  Imager (HXI) observes images and spectra of X-ray bursts in solar
  flares. In this paper, we briefly report on the progresses made by
  the HXI science team (data and software team) during the design phase
  (till May 2019). These include simulations of HXI imaging, optimization
  of HXI grids, development of imaging algorithms, estimation of orbital
  background, as well as in-orbit calibration plan. These efforts provided
  guidance for the engineering, improved HXI’s imaging capability and
  reduced the cost of the instrument.

---------------------------------------------------------
Title: VizieR Online Data Catalog: A complete sample of broad-line
    AGN from SDSS-DR7 (Liu+, 2019)
Authors: Liu, H. -Y.; Liu, W. -J.; Dong, X. -B.; Zhou, H.; Wang, T.;
   Lu, H.; Yuan, W.
2019yCat..22430021L    Altcode:
  The SDSS is a comprehensive imaging and spectroscopic survey using a
  dedicated 2.5m telescope located at Apache Point Observatory to image
  over 10000deg<SUP>2</SUP> of sky and to perform follow-up spectroscopic
  observations. The telescope uses a wide-field imager (filters ugriz)
  and a 640-fiber-fed pair of multiobjects double spectrographs covering
  the wavelength 3800-9200Å with a resolution varying from 1850 to
  2200. <P />We have compiled a sample of 14584 type 1 AGNs based
  on detection of a broad Hα line from a total of about one million
  SDSS DR7 spectroscopic objects. Part I of the catalog (see Table 1)
  is composed of the basic information of these sources. Part II of the
  catalog (see Table 2) includes the emission line measurements derived
  from the spectral analysis in this work. Finally, in part III of
  the catalog (Table 3), we supplement photometric measurements in the
  optical, ultraviolet (UV), near-infrared (NIR), mid-infrared (MIR),
  X-ray, and radio drawn from GALEX, 2MASS, WISE, ROSAT, and FIRST;
  see Section 4.3.3 for further details. <P />(3 data files).

---------------------------------------------------------
Title: Correction of Off-axis Aberration of the China Near Earth
    Object Survey Telescope with 10k CCD
Authors: Zhaori, G. T.; Zhao, H. B.; Liu, W.; Li, B.
2019AcASn..60...52Z    Altcode:
  The SI600S (4k×4k) CCD of CNEOST (China Near Earth Object Survey
  Telescope) now has been upgraded to STA1600LN (10k×10k), with the
  image region size that becomes larger, and the observation field of
  view (FoV) of telescope that enlarges from 4 to 9 °<SUP>2</SUP>. And
  correspondingly, the diameter of the original available FoV is expanded,
  from 3.14° to 4.28°, which is improved by 36% compared with the
  original design. Moreover, the thickness of the field lens increases
  by 8.75 mm. These two factors lead to the result that the off-axis
  aberration increases and image quality becomes worse. In order to
  solve this problem, based on the original optical design parameter
  of the telescope, we try to improve the image quality with the ZEMAX
  optical design software. The method is to design an additional field
  corrector to correct the off-axis aberration. The corrector is composed
  of two lenses with all spherical surfaces, and placed in front of the
  existing field lens. Furthermore, we put forward a new optical design
  which expands the available FoV from 14.38 to 28.27 °<SUP>2</SUP>.

---------------------------------------------------------
Title: Indication of nearby source signatures of cosmic rays from
    energy spectra and anisotropies
Authors: Liu, Wei; Guo, Yi-Qing; Yuan, Qiang
2019JCAP...10..010L    Altcode: 2018arXiv181209673L
  The origin of Galactic cosmic rays (GCRs) remains a mystery after
  more than one century of their discovery. The diffusive propagation
  of charged particles in the turbulent Galactic magnetic field makes us
  unable to trace back to their acceleration sites. Nevertheless, nearby
  GCR source(s) may leave imprints on the locally measured energy spectra
  and the anisotropies of the arrival direction. In this work we propose
  a simple but natural description of the GCR production and propagation,
  within a two-zone disk-halo diffusion scenario together with a nearby
  source, to understand the up-to-date precise measurements of the energy
  spectra and anisotropies of GCRs. We find that a common energy scale of
  ~100 TeV appears in both energy spectra of protons and helium nuclei
  measured recently by CREAM and large-scale anisotropies detected by
  various experiments. These results indicate that one or more local
  sources are very likely important contributors to GCRs below 100 TeV
  . This study provides a probe to identify source(s) of GCRs by means
  of joint efforts of spectral and anisotropy measurements.

---------------------------------------------------------
Title: Lijiang 2.4-meter Telescope and its instruments
Authors: Wang, Chuan-Jun; Bai, Jin-Ming; Fan, Yu-Feng; Mao, Ji-Rong;
   Chang, Liang; Xin, Yu-Xin; Zhang, Ju-Jia; Lun, Bao-Li; Wang, Jian-Guo;
   Zhang, Xi-Liang; Ying, Mei; Lu, Kai-Xing; Wang, Xiao-Li; Ji, Kai-Fan;
   Xiong, Ding-Rong; Yu, Xiao-Guang; Ding, Xu; Ye, Kai; Xing, Li-Feng; Yi,
   Wei-Min; Xu, Liang; Zheng, Xiang-Ming; Feng, Yuan-Jie; He, Shou-Sheng;
   Wang, Xue-Li; Liu, Zhong; Chen, Dong; Xu, Jun; Qin, Song-Nian; Zhang,
   Rui-Long; Tan, Hui-Song; Li, Zhi; Lou, Ke; Li, Jian; Liu, Wei-Wei
2019RAA....19..149W    Altcode: 2019arXiv190505915W
  The Lijiang 2.4-meter Telescope (LJT), the largest common-purpose
  optical telescope in China, has been available to the worldwide
  astronomical community since 2008. It is located at the Gaomeigu site,
  Lijiang Observatory (LJO), in the southwest of China. The site has very
  good observational conditions. During its 10-year operation, several
  instruments have been equipped on the LJT. Astronomers can perform both
  photometric and spectral observations. The main scientific goals of LJT
  include recording photometric and spectral evolution of supernovae,
  reverberation mapping of active galactic nuclei, investigating the
  physical properties of binary stars and near-earth objects (comets
  and asteroids), and identification of exoplanets and all kinds of
  transients. Until now, the masses of 41 high accretion rate black
  holes have been measured, and more than 168 supernovae have been
  identified by the LJT. More than 190 papers related to the LJT have
  been published. In this paper, the general observation conditions of
  the Gaomeigu site is introduced at first. Then, the structure of the
  LJT is described in detail, including the optical, mechanical, motion
  and control system. The specification of all the instruments and some
  detailed parameters of the YFOSC is also presented. Finally, some
  important scientific results and future expectations are summarized.

---------------------------------------------------------
Title: A Method to Detect Radio Frequency Interference Based on
    Convolutional Neural Networks
Authors: DAI, C.; ZUO, S. F.; Liu, W.; Li, J. X.; Zhu, M.; Wu, F. Q.;
   Yu, X. C.
2019ASPC..523...71D    Altcode:
  RFI is an important challenge for radio astronomy. In this paper, we
  adopt a deep convolution neural network with a symmetrical structure,
  the U-Net, to detect RFI. The U-Net can perform the classification
  task of clean signal and RFI. It extracts the features of RFI for
  learning RFI distribution pattern and then calculates the probability
  value of RFI for each pixel. Then we set a threshold to get the results
  flagged by RFI. Experiments on Tianlai data (A radio telescope-array,
  the observing time is from 20:15:45 to 24:18:45 on 27th of September
  2016, and the frequency is from 744MHz to 756MHz) show that, compared
  with the traditional RFI flagging method, this approach can get almost
  consistent results with satisfying accuracy and take into account
  the relationship between different baselines, which contributes to
  correctly and effectively flag RFI.

---------------------------------------------------------
Title: Panoramic SETI: An all-sky fast time-domain observatory
Authors: Wright, Shelley; Antonio, Franklin P.; Aronson, Michael L.;
   Chaim-Weismann, Samuel A.; Cosens, Maren; Drake, Frank D.; Horowitz,
   Paul; Howard, Andrew W.; Liu, Wei; Maire, Jerome; Siemion, Andrew
   P. V.; Raffanti, Rick; Shippee, Guillaume D.; Stone, Remington P. S.;
   Treffers, Richard R.; Uttamchandani, Avinash; Werthimer, Dan; Wiley,
   James
2019BAAS...51g.264W    Altcode: 2019astro2020U.264W
  We are designing an optical and near-infrared observatory designed
  to greatly enlarge the current SETI phase space. The Pulsed All-sky
  Near-infrared Optical SETI (PANOSETI) observatory will be a dedicated
  SETI facility that aims to increase sky area searched, wavelengths
  covered, number of stellar systems observed, and duration of time
  monitored.

---------------------------------------------------------
Title: Measurement of the cosmic ray proton spectrum from 40 GeV to
    100 TeV with the DAMPE satellite
Authors: An, Q.; Asfandiyarov, R.; Azzarello, P.; Bernardini, P.;
   Bi, X. J.; Cai, M. S.; Chang, J.; Chen, D. Y.; Chen, H. F.; Chen,
   J. L.; Chen, W.; Cui, M. Y.; Cui, T. S.; Dai, H. T.; D'Amone, A.;
   De Benedittis, A.; De Mitri, I.; Di Santo, M.; Ding, M.; Dong, T. K.;
   Dong, Y. F.; Dong, Z. X.; Donvito, G.; Droz, D.; Duan, J. L.; Duan,
   K. K.; D'Urso, D.; Fan, R. R.; Fan, Y. Z.; Fang, F.; Feng, C. Q.;
   Feng, L.; Fusco, P.; Gallo, V.; Gan, F. J.; Gao, M.; Gargano, F.; Gong,
   K.; Gong, Y. Z.; Guo, D. Y.; Guo, J. H.; Guo, X. L.; Han, S. X.; Hu,
   Y. M.; Huang, G. S.; Huang, X. Y.; Huang, Y. Y.; Ionica, M.; Jiang,
   W.; Jin, X.; Kong, J.; Lei, S. J.; Li, S.; Li, W. L.; Li, X.; Li,
   X. Q.; Li, Y.; Liang, Y. F.; Liang, Y. M.; Liao, N. H.; Liu, C. M.;
   Liu, H.; Liu, J.; Liu, S. B.; Liu, W. Q.; Liu, Y.; Loparco, F.; Luo,
   C. N.; Ma, M.; Ma, P. X.; Ma, S. Y.; Ma, T.; Ma, X. Y.; Marsella,
   G.; Mazziotta, M. N.; Mo, D.; Niu, X. Y.; Pan, X.; Peng, W. X.;
   Peng, X. Y.; Qiao, R.; Rao, J. N.; Salinas, M. M.; Shang, G. Z.;
   Shen, W. H.; Shen, Z. Q.; Shen, Z. T.; Song, J. X.; Su, H.; Su, M.;
   Sun, Z. Y.; Surdo, A.; Teng, X. J.; Tykhonov, A.; Vitillo, S.; Wang,
   C.; Wang, H.; Wang, H. Y.; Wang, J. Z.; Wang, L. G.; Wang, Q.; Wang,
   S.; Wang, X. H.; Wang, X. L.; Wang, Y. F.; Wang, Y. P.; Wang, Y. Z.;
   Wang, Z. M.; Wei, D. M.; Wei, J. J.; Wei, Y. F.; Wen, S. C.; Wu, D.;
   Wu, J.; Wu, L. B.; Wu, S. S.; Wu, X.; Xi, K.; Xia, Z. Q.; Xu, H. T.;
   Xu, Z. H.; Xu, Z. L.; Xu, Z. Z.; Xue, G. F.; Yang, H. B.; Yang, P.;
   Yang, Y. Q.; Yang, Z. L.; Yao, H. J.; Yu, Y. H.; Yuan, Q.; Yue, C.;
   Zang, J. J.; Zhang, F.; Zhang, J. Y.; Zhang, J. Z.; Zhang, P. F.;
   Zhang, S. X.; Zhang, W. Z.; Zhang, Y.; Zhang, Y. J.; Zhang, Y. L.;
   Zhang, Y. P.; Zhang, Y. Q.; Zhang, Z.; Zhang, Z. Y.; Zhao, H.; Zhao,
   H. Y.; Zhao, X. F.; Zhou, C. Y.; Zhou, Y.; Zhu, X.; Zhu, Y.; Zimmer, S.
2019SciA....5.3793A    Altcode: 2019arXiv190912860A
  The precise measurement of the spectrum of protons, the most abundant
  component of the cosmic radiation, is necessary to understand the
  source and acceleration of cosmic rays in the Milky Way. This work
  reports the measurement of the cosmic ray proton fluxes with kinetic
  energies from 40 GeV to 100 TeV, with two and a half years of data
  recorded by the DArk Matter Particle Explorer (DAMPE). This is the
  first time an experiment directly measures the cosmic ray protons up
  to ~100 TeV with a high statistics. The measured spectrum confirms
  the spectral hardening found by previous experiments and reveals a
  softening at ~13.6 TeV, with the spectral index changing from ~2.60 to
  ~2.85. Our result suggests the existence of a new spectral feature of
  cosmic rays at energies lower than the so-called knee, and sheds new
  light on the origin of Galactic cosmic rays.

---------------------------------------------------------
Title: Analysis of the 1.3-1.7 yr Oscillation Relationship between
    Solar and Geomagnetic Activities
Authors: Qian, Ya-wen; Feng, Song; Deng, Lin-hua; Liu, Wei-hang
2019ChA&A..43..365Q    Altcode: 2019ChA&A..43..365Y
  The study on the 1.3-1.7 yr period of the solar and geomagnetic
  activities is very important for understanding the possible physical
  processes in the solar-terrestrial coupling system. The sunspot is
  the most prominent magnetic field structure in the solar photosphere,
  and the Ap index is an important indicator for the global geomagnetic
  activity level. The 1.3-1.7 yr period for the sunspot number and the
  geomagnetic Ap index is obtained by the synchro-squeezing wavelet
  transform, and the phase relationship between them is studied by
  the cross-correlation analysis. The main results are as follows: (1)
  The 1.3-1.7 yr period of the geomagnetic Ap index and sunspot number
  exhibits an intermittent evolutionary characteristics, and changes
  continuously with the time; (2) the geomagnetic Ap index has a higher
  periodic component in the odd solar cycles than the neighboring even
  solar cycles, which is characterized by fluctuations; (3) the phase
  relationship between the geomagnetic Ap index and the sunspot number
  is not always invariant, in most cases the geomagnetic Ap index lags
  behind the sunspot number, except in the 18th and 22th solar cycles.

---------------------------------------------------------
Title: Study on the 3D anisotropic propagation of Galactic cosmic rays
Authors: Hu, H.; Liu, W.; Lin, S. J.; Guo, Y. Q.
2019ICRC...36...80H    Altcode: 2019PoS...358...80H
  No abstract at ADS

---------------------------------------------------------
Title: Using Real-Time Drilling Data to Characterize Water-Ice on
    the Moon
Authors: Joshi, D. R.; Eustes, A. W.; Rostami, J.; Dreyer, C.; Zody,
   Z.; Liu, W.
2019LPICo2152.5127J    Altcode:
  This paper offers the details of the design of the test drill unit
  based on heritage drill systems used by NASA and others. The paper
  discusses the acquisition and analysis of the drilling data to assess
  the strength and water content in the PSRs.

---------------------------------------------------------
Title: Quasi-Periodic Pulsations Observed in White Light at the Loop
    Top of the SOL2017-09-10 X8.2 Flare
Authors: Zhao, Junwei; Liu, Wei
2019AAS...23421002Z    Altcode:
  An X8.2 flare occurred on September 10, 2017 near the Sun's west
  limb. Simultaneously with the observations of the SDO/AIA's multiple
  UV/EUV channels, the continuum intensity of the SDO/HMI also observed
  the evolution of the post-flare loop above the solar limb. This gives
  us a rare opportunity to analyze the post-flare loop in visible light,
  UV, and EUV channels. Quasi-periodic pulsations, with a period close
  to about 8 minutes, are found in all these channels during the rise
  of the loop top. We study the spatial and temporal relations of
  the pulsations observed in different wavelengths, and find that EUV
  pulsations occurred about 2-3 minutes earlier, and 2-6 Mm higher in
  altitude, than the pulsations observed in UV and white light. While
  the UV observations show many similarities in the pulsations with
  the white light observations, the UV intensity decayed with the
  rise of the loop but the white light intensity grew for about 20 more
  minutes. These observations help shed light on our understanding of the
  magnetohydrodynamics of the flare's loop-top, as well as the emission
  mechanism of the white light off the solar limb.

---------------------------------------------------------
Title: On the Origin of Quasi-periodic Fast-mode Propagating Wave
Trains (QFPs): A Statistical Survey
Authors: Silver, Jay; Liu, Wei; Ofman, Leon
2019AAS...23421001S    Altcode:
  The magnetized solar corona hosts a variety of waves that are physically
  important and can serve as useful diagnostic tools. One type of such
  coronal waves are Quasi-periodic Fast-mode Propagating wave trains
  (QFPs), which were first detected in extreme ultraviolet (EUV) by
  the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics
  Observatory (SDO). QFPs are not uncommon and are generally associated
  with some, but not all solar flares and/or coronal mass ejections
  (CMEs). To search for physical conditions that can contribute to QFP
  production, we carried out a systematic survey of QFPs from the full
  SDO mission. We found that about 1/5 of global EUV waves were associated
  with QFPs. We also conducted a comparative study of two active regions
  (ARs) visible between October and November 2014, AR12192 and AR12205,
  with very different levels of QFP activity. AR12205 produced less
  flares but more QFPs, which were all associated with blow-out,
  eruptive flares and global EUV waves. In contrast, AR12192 produced
  more (mostly confined) flares, but with virtually no QFPs and less
  CMEs. This suggests that blow-out eruptions could be a necessary,
  but not sufficient condition for QFP production and/or detectability.

---------------------------------------------------------
Title: Long-lasting Conjugate Coronal Dimmings Produced by a Filament
Eruption: Implications for Global Magnetic Connectivity
Authors: Kocher, Manan; Liu, Wei; Downs, Cooper
2019AAS...23411104K    Altcode:
  Coronal dimmings, typically observed at extreme ultraviolet (EUV)
  wavelengths, are commonly associated with solar eruptions, such as
  coronal mass ejections (CMEs) and eruptive filaments. They offer
  critical clues to our understanding of the underlying mechanisms and
  consequences of solar eruptions. We present a study of an intriguing
  dimming event associated with a quiescent filament eruption on March 6,
  2018 observed by SDO/AIA, STEREO/SECCHI, and IRIS. There were notably
  sigmoid-shaped, conjugate dimmings that appeared concurrently in
  multiple EUV channels, but evolved asymmetrically with time. One of
  the double dimmings lasted more than two days, which clearly sets it
  apart from the typical lifetime of several hours in previously reported
  dimmings. We investigated the temperature and density evolution of the
  dimming features, as well as the eruptive filament itself. We uncovered
  large-scale magnetic field connectivity between the conjugate dimmings
  and remote coronal holes where brightenings were observed around the
  time of the eruption. These remote brightenings are possible precursors
  of the eruption or manifestations of its associated global magnetic
  reconfiguration process. These results are significant because they
  allow us to use dimmings as tracers to probe the Sun's magnetic
  connectivity and the mechanisms responsible for the initiation of
  space-weather driving solar eruptions.

---------------------------------------------------------
Title: Coronal Condensation at Preferential Topological Locations:
    The Birth of Solar Prominences and Coronal Rain
Authors: Liu, Wei; Sun, Xudong; Yu, Sijie; Antolin, Patrick; Titov,
   Viacheslav; Downs, Cooper; Berger, Thomas
2019AAS...23412502L    Altcode:
  The million-degree hot and tenuous solar coronal plasma, under
  certain conditions, can enigmatically undergo a radiative cooling
  instability and condense into material of 100 times cooler in the form
  of prominences or coronal rain. Where, when, and how such cooling
  condensation takes place remain poorly understood. Answers to these
  questions are not only of scientific importance in their own right,
  but also bear implications for the fundamental question of coronal
  heating and the chromosphere-corona mass cycle. Magnetic fields in the
  magnetized corona undoubtedly play a crucial role (e.g., by trapping the
  plasma), but where and how? We report recent imaging and spectroscopic
  observations from SDO/AIA/HMI and IRIS that can shed light on these
  puzzles. Through a systematic survey, we found that a large fraction
  of quiet-Sun condensations preferentially occur at the dips of coronal
  loops or funnels. Such dips are located at/near magnetic topological
  features, such as null points and quasi-separatrix layers (QSLs), which
  are regions characterized by high values of the squashing factor. We
  also identified evidence of magnetic reconnection at such locations,
  which can produce favorable conditions, e.g., density enhancement
  by compression and/or mass trapping in plasmoids, that can trigger
  run-away radiative cooling. We will discuss the significance and
  broader implications of these novel observations.

---------------------------------------------------------
Title: The Global EUV Wave Associated with the SOL2017-09-10 X8.2
Flare: SDO/AIA Observations and Data-constrained MHD Simulations
Authors: Liu, Wei; Jin, Meng; Ofman, Leon; DeRosa, Marc L.
2019AAS...23430701L    Altcode:
  While large-scale extreme ultraviolet (EUV) waves associated with
  coronal mass ejections (CMEs) and solar flares are common, the EUV
  wave triggered by the X8 flare-CME eruption on 2017 September 10
  was an extreme. This was, to the best of our knowledge, the first
  detection of an EUV wave traversing the full-Sun corona over the entire
  visible disk and off-limb circumference, manifesting a truly global
  nature. In addition to commonly observed reflections, it had strong
  transmissions in and out of both polar coronal holes, at elevated
  wave speeds of &gt;2000 km/s within them. With an exceptionally large
  wave amplitude, it produced significant compressional heating to local
  coronal plasma. We present detailed analysis of SDO/AIA observations,
  global magnetic field extrapolations with the potential-field source
  surface (PFSS) model, and data-constrained MHD simulations of this
  event using the University of Michigan Alfven Wave Solar Model
  (AWSoM). By comparing the observations and simulations, we benchmark
  diagnostics of the magnetic field strengths and thermal properties of
  the solar corona on global scales. We discuss the future prospects of
  using such extreme EUV waves as probes for global coronal seismology,
  an area yet to be fully exploited.

---------------------------------------------------------
Title: Major Scientific Challenges and Opportunities in Understanding
    Magnetic Reconnection and Related Explosive Phenomena throughout
    the Universe
Authors: Ji, Hantao; Alt, A.; Antiochos, S.; Baalrud, S.; Bale, S.;
   Bellan, P. M.; Begelman, M.; Beresnyak, A.; Blackman, E. G.; Brennan,
   D.; Brown, M.; Buechner, J.; Burch, J.; Cassak, P.; Chen, L. -J.;
   Chen, Y.; Chien, A.; Craig, D.; Dahlin, J.; Daughton, W.; DeLuca, E.;
   Dong, C. F.; Dorfman, S.; Drake, J.; Ebrahimi, F.; Egedal, J.; Ergun,
   R.; Eyink, G.; Fan, Y.; Fiksel, G.; Forest, C.; Fox, W.; Froula, D.;
   Fujimoto, K.; Gao, L.; Genestreti, K.; Gibson, S.; Goldstein, M.;
   Guo, F.; Hesse, M.; Hoshino, M.; Hu, Q.; Huang, Y. -M.; Jara-Almonte,
   J.; Karimabadi, H.; Klimchuk, J.; Kunz, M.; Kusano, K.; Lazarian,
   A.; Le, A.; Li, H.; Li, X.; Lin, Y.; Linton, M.; Liu, Y. -H.; Liu,
   W.; Longcope, D.; Louriero, N.; Lu, Q. -M.; Ma, Z. -W.; Matthaeus,
   W. H.; Meyerhofer, D.; Mozer, F.; Munsat, T.; Murphy, N. A.; Nilson,
   P.; Ono, Y.; Opher, M.; Park, H.; Parker, S.; Petropoulou, M.; Phan,
   T.; Prager, S.; Rempel, M.; Ren, C.; Ren, Y.; Rosner, R.; Roytershteyn,
   V.; Sarff, J.; Savcheva, A.; Schaffner, D.; Schoeffier, K.; Scime, E.;
   Shay, M.; Sitnov, M.; Stanier, A.; TenBarge, J.; Tharp, T.; Uzdensky,
   D.; Vaivads, A.; Velli, M.; Vishniac, E.; Wang, H.; Werner, G.; Xiao,
   C.; Yamada, M.; Yokoyama, T.; Yoo, J.; Zenitani, S.; Zweibel, E.
2019BAAS...51c...5J    Altcode: 2019astro2020T...5J
  This is a group white paper of 100 authors (each with explicit
  permission via email) from 51 institutions on the topic of magnetic
  reconnection which is relevant to 6 thematic areas. Grand challenges
  and research opportunities are described in observations, numerical
  modeling and laboratory experiments in the upcoming decade.

---------------------------------------------------------
Title: Lake Water Depth Controlling Archaeal Tetraether Distributions
in Midlatitude Asia: Implications for Paleo Lake-Level Reconstruction
Authors: Wang, H.; He, Y.; Liu, W.; Zhou, A.; Kolpakova, M.;
   Krivonogov, S.; Liu, Z.
2019GeoRL..46.5274W    Altcode:
  Lake-level reconstructions, related to terrestrial hydrological
  changes, are important for our understanding of past and future
  climates. Currently, however, reliable lake-level proxies are still
  limited. Here we report distributions of archaeal tetraether lipids in
  70 surface sediment samples collected from 55 lakes in midlatitude
  Asia. We have found that among various lake physico-chemical
  characteristics, the relative abundances of crenarchaeol and
  Hydroxylated isoprenoid glycerol dialkyl glycerol tetraethers (%cren
  and %OH-GDGTs) are best correlated with lake water depth, due to a
  preference of Thaumarchaeota, the producer of these biomarkers, for a
  niche in subsurface lake water. This supports the recent hypothesis
  based on single-lake investigations that %cren and %OH-GDGTs are
  potentially novel lake-level proxies. Our results also suggest that
  %OH-GDGTs is less affected by soil input than %cren. Nevertheless, other
  confounding factors should be well constrained and local/site-specific
  calibrations are needed before the two molecular proxies are used
  quantitatively in down-core applications.

---------------------------------------------------------
Title: Earth wind as a possible source of lunar surface hydration
Authors: Wang, H. Z.; Zhang, J.; Shi, Q. Q.; Saito, Y.; Degeling,
   A. W.; Rae, I. J.; Liu, J.; Guo, R. L.; Yao, Z. H.; Tian, A. M.; Fu,
   X. H.; Zong, Q. G.; Liu, J. Z.; Ling, Z. C.; Sun, W. J.; Bai, S. C.;
   Chen, J.; Yao, S. T.; Zhang, H.; Wei, Y.; Liu, W. L.; Xia, L. D.;
   Chen, Y.; Feng, Y. Y.; Fu, S. Y.; Pu, Z. Y.
2019arXiv190304095W    Altcode:
  Understanding the sources of lunar water is crucial for studying the
  history of lunar evolution, and also the solar wind interaction with
  the Moon and other airless bodies. Recent observations revealed lunar
  hydration is very likely a surficial dynamic process driven by solar
  wind. Solar wind is shielded over a period of 3-5 days as the Moon
  passes through the Earth's magnetosphere, during which a significant
  loss of hydration is expected from previous works.Here we study lunar
  hydration inside the magnetosphere using orbital spectral data, which
  unexpectedly found that the polar surficial OH/H2O abundance remains
  at the same level when in the solar wind and in the magnetosphere. We
  suggest that particles from the magnetosphere (Earth wind, naturally
  different from solar wind) contribute to lunar hydration. From lunar
  orbital plasma observations, we find the existence of optimal energy
  ranges, other than 1 keV as previously thought, for surface hydration
  formation. These optimal energy ranges deduced from space observations
  may provide strong implications for laboratory experiments simulating
  lunar hydration processes.

---------------------------------------------------------
Title: Surface Tension of the Black Hole Horizon
Authors: Shu, Liangsuo; Cui, Kaifeng; Liu, Xiaokang; Liu, Zhichun;
   Liu, Wei
2019ForPh..6700076S    Altcode: 2018arXiv180203577S
  The idea of treating the horizon of a black hole as a stretched
  membrane with surface tension has a long history. In this work, we
  discuss the microscopic origin of the surface tension of the horizon
  in quantum pictures of spaces, which are Bose-Einstein condensates
  of gravitons. The horizon is a phase interface of gravitons, the
  surface tension of which is found to be a result of the difference
  in the strength of the interaction between the gravitons on its two
  sides. The gravitational source, such as a Schwarzschild black hole,
  creates a transitional zone by changing the energy and distribution
  of its surrounding gravitons. Archimedes' principle for gravity can
  be expressed as follows: "the gravity on an object is equal to the
  weight of the gravitons that it displaces."

---------------------------------------------------------
Title: The on-orbit calibration of DArk Matter Particle Explorer
Authors: Ambrosi, G.; An, Q.; Asfandiyarov, R.; Azzarello, P.;
   Bernardini, P.; Cai, M. S.; Caragiulo, M.; Chang, J.; Chen, D. Y.;
   Chen, H. F.; Chen, J. L.; Chen, W.; Cui, M. Y.; Cui, T. S.; Dai, H. T.;
   D'Amone, A.; De Benedittis, A.; De Mitri, I.; Ding, M.; Di Santo, M.;
   Dong, J. N.; Dong, T. K.; Dong, Y. F.; Dong, Z. X.; Droz, D.; Duan,
   K. K.; Duan, J. L.; D'Urso, D.; Fan, R. R.; Fan, Y. Z.; Fang, F.;
   Feng, C. Q.; Feng, L.; Fusco, P.; Gallo, V.; Gan, F. J.; Gao, M.;
   Gao, S. S.; Gargano, F.; Garrappa, S.; Gong, K.; Gong, Y. Z.; Guo,
   J. H.; Hu, Y. M.; Huang, G. S.; Huang, Y. Y.; Ionica, M.; Jiang, D.;
   Jiang, W.; Jin, X.; Kong, J.; Lei, S. J.; Li, S.; Li, X.; Li, W. L.;
   Li, Y.; Liang, Y. F.; Liang, Y. M.; Liao, N. H.; Liu, C. M.; Liu,
   H.; Liu, J.; Liu, S. B.; Liu, W. Q.; Liu, Y.; Loparco, F.; Ma, M.;
   Ma, P. X.; Ma, S. Y.; Ma, T.; Ma, X. Q.; Ma, X. Y.; Marsella, G.;
   Mazziotta, M. N.; Mo, D.; Niu, X. Y.; Pan, X.; Peng, X. Y.; Peng,
   W. X.; Qiao, R.; Rao, J. N.; Salinas, M. M.; Shang, G. Z.; Shen,
   W. H.; Shen, Z. Q.; Shen, Z. T.; Song, J. X.; Su, H.; Su, M.; Sun,
   Z. Y.; Surdo, A.; Teng, X. J.; Tian, X. B.; Tykhonov, A.; Vitillo,
   S.; Wang, C.; Wang, H.; Wang, H. Y.; Wang, J. Z.; Wang, L. G.; Wang,
   Q.; Wang, S.; Wang, X. H.; Wang, X. L.; Wang, Y. F.; Wang, Y. P.;
   Wang, Y. Z.; Wang, Z. M.; Wen, S. C.; Wei, D. M.; Wei, J. J.; Wei,
   Y. F.; Wu, D.; Wu, J.; Wu, L. B.; Wu, S. S.; Wu, X.; Xi, K.; Xia,
   Z. Q.; Xin, Y. L.; Xu, H. T.; Xu, Z. H.; Xu, Z. L.; Xu, Z. Z.; Xue,
   G. F.; Yang, H. B.; Yang, P.; Yang, Y. Q.; Yang, Z. L.; Yao, H. J.;
   Yu, Y. H.; Yuan, Q.; Yue, C.; Zang, J. J.; Zhang, D. L.; Zhang, F.;
   Zhang, J. B.; Zhang, J. Y.; Zhang, J. Z.; Zhang, L.; Zhang, P. F.;
   Zhang, S. X.; Zhang, W. Z.; Zhang, Y.; Zhang, Y. J.; Zhang, Y. Q.;
   Zhang, Y. L.; Zhang, Y. P.; Zhang, Z.; Zhang, Z. Y.; Zhao, H.; Zhao,
   H. Y.; Zhao, X. F.; Zhou, C. Y.; Zhou, Y.; Zhu, X.; Zhu, Y.; Zimmer, S.
2019APh...106...18A    Altcode: 2019arXiv190702173A
  The DArk Matter Particle Explorer (DAMPE), a satellite-based cosmic
  ray and gamma-ray detector, was launched on December 17, 2015, and
  began its on-orbit operation on December 24, 2015. In this work we
  document the on-orbit calibration procedures used by DAMPE and report
  the calibration results of the Plastic Scintillator strip Detector
  (PSD), the Silicon-Tungsten tracKer-converter (STK), the BGO imaging
  calorimeter (BGO), and the Neutron Detector (NUD). The results are
  obtained using Galactic cosmic rays, bright known GeV gamma-ray
  sources, and charge injection into the front-end electronics of each
  sub-detector. The determination of the boundary of the South Atlantic
  Anomaly (SAA), the measurement of the live time, and the alignments of
  the detectors are also introduced. The calibration results demonstrate
  the stability of the detectors in almost two years of the on-orbit
  operation.

---------------------------------------------------------
Title: Classification of large-scale stellar spectra based on deep
    convolutional neural network
Authors: Liu, W.; Zhu, M.; Dai, C.; He, D. Y.; Yao, Jiawen; Tian,
   H. F.; Wang, B. Y.; Wu, K.; Zhan, Y.; Chen, B. -Q.; Luo, A. -Li;
   Wang, R.; Cao, Y.; Yu, X. C.
2019MNRAS.483.4774L    Altcode: 2018MNRAS.tmp.2885L
  Classification of stellar spectra from voluminous spectra is a
  very important and challenging task. In order to better classify
  stellar spectra, inspired by the principle of deep convolutional
  neural network (CNN), we propose a supervised algorithm for stellar
  spectra classification based on 1-D stellar spectra convolutional
  neural network (1-D SSCNN). In 1-D SSCNN, we modify the traditional
  2-D convolutional neural network into 1-D network to adapt to the
  spectral classification. On the basis of using convolution algorithm,
  the spectral features are extracted and used for classification. We
  firstly use the stellar spectra data to train a 1-D SSCNN to obtain
  a well-trained model, and then we apply the well-trained model to
  classify the unknown spectra. To evaluate the performance of the
  proposed algorithms, we apply 1-D SSCNN to classify three spectral
  types: F-type spectra, G-type spectra and K-type spectra and ten
  subclasses of K-type spectra: A0-type, A5-type, F0-type, F5-type,
  G0-type, G5-type, K0-type, K5-type, M0-type and M5-type spectra from
  Sloan Digital Sky Survey (SDSS). Our 1-D SSCNN algorithm obtain higher
  classification accuracy compared with Support Vector Machine (SVM),
  Random Forest (RF) and Artificial neural network (ANN).

---------------------------------------------------------
Title: A deep learning approach for detecting candidates of supernova
    remnants
Authors: Liu, Wei; Zhu, Meng; Dai, Cong; Wang, Bing-Yi; Wu, Kang;
   Yu, Xian-Chuan; Tian, Wen-Wu; Zhang, Meng-Fei; Wang, Hong-Feng
2019RAA....19...42L    Altcode:
  Detecting supernova remnant (SNR) candidates in the interstellar
  medium is a challenging task because SNRs have weak radio signals
  and irregular shapes. The use of a convolutional neural network is a
  deep learning method that can help us extract various features from
  images. To extract SNRs from astronomical images and estimate the
  positions of SNR candidates, we design the SNR-Net model composed of
  a training component and a detection component. In addition, transfer
  learning is used to initialize the network parameters, which improves
  the speed and accuracy of network training. We apply a T-T plot (of
  the different brightness temperatures of map pixels at two different
  frequencies) to calculate the spectral index of SNR candidates. To
  accelerate the scientific computing process, we take advantage of
  innovative hardware architecture, such as deep learning optimized
  graphics processing units, which increases the speed of computation
  by a factor of 5. A case study suggests that SNR-Net may be applicable
  to detecting extended sources in the images automatically.

---------------------------------------------------------
Title: Noncommutative Coordinate Picture of the Quantum Phase Space
Authors: Kong, Otto C. W.; Liu, Wei-Yin
2019arXiv190311962K    Altcode:
  We illustrate an isomorphic representation of the observable algebra
  for quantum mechanics in terms of the functions on the projective
  Hilbert space, and its Hilbert space analog, with a noncommutative
  product in terms of explicit coordinates and discuss the physical
  and dynamical picture. The isomorphism is then used as a base for the
  translation of the differential symplectic geometry of the infinite
  dimensional manifolds onto the observable algebra as a noncommutative
  geometry. Hence, we obtain the latter from the physical theory
  itself. We have essentially an extended formalism of the Schrodinger
  versus Heisenberg picture which we describe mathematically as like
  a coordinate map from the phase space, for which we have presented
  argument to be seen as the quantum model of the physical space, to the
  noncommutative geometry coordinated by the six position and momentum
  operators. The observable algebra is taken essentially as an algebra
  of formal functions on the latter operators. The work formulates the
  intuitive idea that the noncommutative geometry can be seen as an
  alternative, noncommutative coordinate, picture of familiar quantum
  phase space, at least so long as the symplectic geometry is concerned.

---------------------------------------------------------
Title: Enhanced monopole transition strength from the cluster decay
    of <SUP>13</SUP>C
Authors: Feng, Jun; Ye, YanLin; Yang, Biao; Lin, ChengJian; Jia,
   HuiMin; Pang, DanYang; Li, ZhiHuan; Lou, JianLing; Li, QiTe; Yang,
   XiaoFei; Li, Jing; Zang, HongLiang; Liu, Qiang; Jiang, Wei; Li,
   ChenGuang; Liu, Yang; Chen, ZhiQiang; Wu, HongYi; Wang, ChunGuang;
   Liu, Wei; Wang, Xiang; Li, JingJing; Luo, DiWen; Jiang, Ying; Bai,
   ShiWei; Xu, JinYan; Ma, NanRu; Sun, LiJie; Wang, DongXi
2019SCPMA..6212011F    Altcode:
  The inelastic excitations and cluster decay of
  <SUP>13</SUP>C have been measured using the reaction,
  <SUP>9</SUP>Be(<SUP>13</SUP>C,<SUP>13</SUP>C* → <SUP>9</SUP>Be +
  α)<SUP>9</SUP>Be. We observe strong excitation to the 14.3-MeV
  (1/2<SUP>-</SUP>) resonant state from the cluster-decay channel,
  leading to an enhanced monopole matrix element of (6.3 ± 0.6)
  fm<SUP>2</SUP>. This large cluster-related monopole strength is a clear
  indication of the cluster-structure domination of this state and is
  consistent with the recent prediction of the orthogonality condition
  model (OCM). It would be interesting to further explore the three-center
  molecular rotational band that is initiated from the observed band-head.

---------------------------------------------------------
Title: Global Impacts of Arctic Sea Ice Loss Mediated by the Atlantic
    Meridional Overturning Circulation
Authors: Liu, Wei; Fedorov, Alexey V.
2019GeoRL..46..944L    Altcode:
  We explore the global impacts of Arctic sea ice decline in climate
  model perturbation experiments focusing on the temporal evolution
  of induced changes. We find that climate response to a realistic
  reduction in sea ice cover varies dramatically between shorter decadal
  and longer multidecadal to centennial timescales. During the first two
  decades, when atmospheric processes dominate, sea ice decline induces
  a "bipolar seesaw" pattern in surface temperature with warming in the
  Northern and cooling in the Southern Hemisphere, leading to a northward
  displacement of the Intertropical Convergence Zone and an expansion of
  Antarctic sea ice. In contrast, on multidecadal and longer timescales,
  the weakening of the Atlantic meridional overturning circulation,
  caused by upper-ocean buoyancy anomalies spreading from the Arctic,
  mediates direct sea ice impacts and nearly reverses the original
  response pattern outside the Arctic. The Southern Hemisphere warms,
  a Warming Hole emerges in the North Atlantic, the Intertropical
  Convergence Zone shifts southward, and Antarctic sea ice contracts.

---------------------------------------------------------
Title: Can the Friction of the Nova Envelope Account for the Extra
    Angular Momentum Loss in Cataclysmic Variables?
Authors: Liu, Wei-Min; Li, Xiang-Dong
2019ApJ...870...22L    Altcode: 2018arXiv181108648L
  It has been shown that the rate of angular momentum loss (AML) in
  cataclysmic variables (CVs) below the period gap is about 2.47 times
  that caused by gravitational radiation (GR), suggesting an extra
  AML mechanism aside from GR. Several potential mechanisms have been
  proposed but none of them has been verified. In this work, we examine
  whether AML caused by friction between the expanding nova envelope
  and the donor star can account for the required AML rate. By adopting
  various expanding velocities of the envelope, we have calculated the
  evolution of CVs with typical initial parameters. Our results show
  that this friction interaction unlikely solves the extra AML problem
  unless the expanding velocities are extremely low. Thus, there should
  be a more efficient AML mechanism that plays a role in CV evolution.

---------------------------------------------------------
Title: Analysis of the 1.3-1.7 yr Oscillation Relationship between
    Solar and Geomagnetic Activities
Authors: Qian, Y. W.; Feng, S.; Deng, L. H.; Liu, W. H.
2019AcASn..60....3Q    Altcode:
  The 1.3-1.7 yr periodic study of solar and geomagnetic activities is
  very important for understanding the possible physical processes in the
  solar-terrestrial coupling system. The sunspot is the most prominent
  magnetic field structure in the solar photosphere, and the Ap index is
  an important indicator of global geomagnetic activity. The 1.3-1.7 yr
  period of the sunspot number and the geomagnetic Ap index is obtained
  by the synchro-squeezing wavelet transform, and the phase relationship
  between them is studied by cross-correlation analysis. The main results
  are as following: (1) The 1.3-1.7 yr periods of the geomagnetic Ap index
  and sunspot number exhibit intermittent evolutionary characteristics,
  and change with time; (2) the geomagnetic Ap index has a higher
  periodic component in odd solar cycles than the neighboring even
  solar cycles, which is characterized by fluctuations; (3) the phase
  relationship between geomagnetic Ap index and sunspot number is not
  always consistent, in most cases the geomagnetic Ap index lags behind
  the sunspot number, except in the 18th and 22th solar cycles.

---------------------------------------------------------
Title: Understanding the Uncertainty in the 21st Century Dynamic
Sea Level Projections: The Role of the AMOC
Authors: Chen, Changlin; Liu, Wei; Wang, Guihua
2019GeoRL..46..210C    Altcode:
  Climate models show that the largest uncertainties in the 21st century
  dynamic sea level (DSL) projections are in the high latitudes of the
  North Atlantic and Southern Oceans. We conduct an intermodel singular
  value decomposition analysis and find that the DSL uncertainties in
  these two oceans are both intrinsically connected to the uncertainty
  in the change of the Atlantic meridional overturning circulation
  (AMOC). We further conduct a freshwater hosing experiment to show
  that the AMOC decline not only accounts for the dipole pattern in the
  DSL change in the North Atlantic but also remotely induces a poleward
  shift in the Southern Hemisphere westerlies that helps build a belted
  pattern of DSL change in the Southern Ocean. Our results suggest that
  reducing the intermodel spread in the change of the AMOC can greatly
  improve the consistency of DSL projection among models not only in
  individual basins but over the global ocean.

---------------------------------------------------------
Title: Revisiting the Spatially Dependent Propagation Model with
    the Latest Observations of Cosmic-Ray Nuclei
Authors: Liu, Wei; Yao, Yu-hua; Guo, Yi-Qing
2018ApJ...869..176L    Altcode: 2018arXiv180203602L
  Recently the AMS-02 collaboration published detections of light
  cosmic-ray nuclei, including lithium, beryllium, boron, carbon,
  and oxygen. Combined with the released energy spectra of proton and
  helium, both primary and secondary spectra have a prominent hardening
  above ∼200 GV. In particular, the spectral variation of secondary
  cosmic rays is greater than the primary ones. One of the plausible
  interpretations for the above anomalies is the spatial-dependent
  diffusion model. It has successfully described various observational
  phenomena, e.g., hardening of primary nuclei, diffuse gamma-ray
  distribution and cosmic-ray anisotropy, etc. In this work, we apply
  the spatial-dependent propagation model to the latest observations,
  including both primary and secondary nuclei. Apart from the primary
  components, the spectra of secondary nuclei can be properly reproduced
  as well, especially the upturn above 200 GV. We also calculate the
  ratios of both secondary-to-primary and secondary-to-secondary. We
  find that except for the Be/B ratio, the computations of the
  spatial-dependent propagation model are in good agreement with the
  current data.

---------------------------------------------------------
Title: Global Magnetohydrodynamics Simulation of EUV Waves and Shocks
    from the X8.2 Eruptive Flare on 2017 September 10
Authors: Jin, Meng; Liu, Wei; Cheung, Mark; Nitta, Nariaki; Manchester,
   Ward; Ofman, Leon; Downs, Cooper; Petrosian, Vahe; Omodei, Nicola
2018csc..confE..66J    Altcode:
  As one of the largest flare-CME eruptions during solar cycle 24, the
  2017 September 10 X8.2 flare event is associated with spectacular
  global EUV waves that transverse almost the entire visible solar
  disk, a CME with speed &gt; 3000 km/s, which is one of the fastest
  CMEs ever recorded, and &gt;100 MeV Gamma-ray emission lasting for
  more than 12 hours. All these unique observational features pose new
  challenge on current numerical models to reproduce the multi-wavelength
  observations. To take this challenge, we simulate the September 10 event
  using a global MHD model (AWSoM: Alfven Wave Solar Model) within the
  Space Weather Modeling Framework and initiate CMEs by Gibson-Low flux
  rope. We conduct detailed comparisons of the synthesized EUV images with
  SDO/AIA observations of global EUV waves. We find that the simulated
  EUV wave morphology and kinematics are sensitive to the orientation
  of the initial flux rope introduced to the source active region. An
  orientation with the flux-rope axis in the north-south direction
  produces the best match to the observations, which suggests that EUV
  waves may potentially be used to constrain the flux-rope geometry for
  such limb or behind-the-limb eruptions that lack good magnetic field
  observations. We also compare observed and simulated EUV intensities
  in multiple AIA channels to perform thermal seismology of the global
  corona. Furthermore, we track the 3D CME-driven shock surface in the
  simulation and derive the time-varying shock parameters together with
  the dynamic magnetic connectivity between the shock and the surface
  of the Sun, with which we discuss the role of CME-driven shocks in
  the long-duration Gamma-ray events.

---------------------------------------------------------
Title: A Truly Global Extreme Ultraviolet Wave from the SOL2017-09-10
    X8.2+ Solar Flare-Coronal Mass Ejection
Authors: Liu, Wei; Jin, Meng; Downs, Cooper; Ofman, Leon; Cheung,
   Mark C. M.; Nitta, Nariaki V.
2018csc..confE..40L    Altcode:
  We report SDO/AIA observations of an extraordinary global extreme
  ultraviolet (EUV) wave triggered by the X8.2+ flare-CME eruption on 2017
  September 10. This was one of the best EUV waves ever observed with
  modern instruments, yet it was likely the last one of such magnitudes
  of Solar Cycle 24 as the Sun heads toward the minimum. Its remarkable
  characteristics include the following. (1) The wave was observed,
  for the first time, to traverse the full-Sun corona over the entire
  visible solar disk and off-limb circumference, manifesting a truly
  global nature, owing to its exceptionally large amplitude, e.g., with
  EUV enhancements by up to 300% at 1.1 Rsun from the eruption. (2)
  This leads to strong transmissions (in addition to commonly observed
  reflections) in and out of both polar coronal holes, which are usually
  devoid of EUV waves. It has elevated wave speeds &gt;2000 km/s within
  them, consistent with the expected higher fast-mode magnetosonic wave
  speeds. The coronal holes essentially serve as new "radiation centers"
  for the waves being refracted out of them, which then travel toward the
  equator and collide head-on, causing additional EUV enhancements. (3)
  The wave produces significant compressional heating to local plasma
  upon its impact, indicated by long-lasting EUV intensity changes and
  differential emission measure increases at higher temperatures (e.g.,
  log T=6.2) accompanied by decreases at lower temperatures (e.g.,
  log T=6.0). These characteristics signify the potential of such EUV
  waves for novel magnetic and thermal diagnostics of the solar corona
  on global scales.

---------------------------------------------------------
Title: Instrument Calibration of the Interface Region Imaging
    Spectrograph (IRIS) Mission
Authors: Wülser, J. -P.; Jaeggli, S.; De Pontieu, B.; Tarbell,
   T.; Boerner, P.; Freeland, S.; Liu, W.; Timmons, R.; Brannon, S.;
   Kankelborg, C.; Madsen, C.; McKillop, S.; Prchlik, J.; Saar, S.;
   Schanche, N.; Testa, P.; Bryans, P.; Wiesmann, M.
2018SoPh..293..149W    Altcode:
  The Interface Region Imaging Spectrograph (IRIS) is a NASA small
  explorer mission that provides high-resolution spectra and images of
  the Sun in the 133 - 141 nm and 278 - 283 nm wavelength bands. The
  IRIS data are archived in calibrated form and made available to the
  public within seven days of observing. The calibrations applied to
  the data include dark correction, scattered light and background
  correction, flat fielding, geometric distortion correction, and
  wavelength calibration. In addition, the IRIS team has calibrated the
  IRIS absolute throughput as a function of wavelength and has been
  tracking throughput changes over the course of the mission. As a
  resource for the IRIS data user, this article describes the details
  of these calibrations as they have evolved over the first few years
  of the mission. References to online documentation provide access to
  additional information and future updates.

---------------------------------------------------------
Title: Probing the Puzzle of Behind-the-limb γ-Ray Flares:
    Data-driven Simulations of Magnetic Connectivity and CME-driven
    Shock Evolution
Authors: Jin, Meng; Petrosian, Vahe; Liu, Wei; Nitta, Nariaki V.;
   Omodei, Nicola; Rubio da Costa, Fatima; Effenberger, Frederic; Li,
   Gang; Pesce-Rollins, Melissa; Allafort, Alice; Manchester, Ward, IV
2018ApJ...867..122J    Altcode: 2018arXiv180701427J
  Recent detections of high-energy γ-rays from behind-the-limb (BTL)
  solar flares by the Fermi Gamma-ray Space Telescope pose a puzzle and
  challenge on the particle acceleration and transport mechanisms. In
  such events, the γ-ray emission region is located away from the BTL
  flare site by up to tens of degrees in heliographic longitude. It
  is thus hypothesized that particles are accelerated at the shock
  driven by the coronal mass ejection (CME) and then travel from the
  shock downstream back to the front side of the Sun to produce the
  observed γ-rays. To test this scenario, we performed data-driven,
  global magnetohydrodynamics simulations of the CME associated with a
  well-observed BTL flare on 2014 September 1. We found that part of the
  CME-driven shock develops magnetic connectivity with the γ-ray emission
  region, facilitating transport of particles back to the Sun. Moreover,
  the observed increase in γ-ray flux is temporally correlated with (1)
  the increase of the shock compression ratio and (2) the presence of a
  quasi-perpendicular shock over the area that is magnetically connected
  to the γ-ray emitting region, both conditions favoring the diffusive
  shock acceleration (DSA) of particles. These results support the above
  hypothesis and can help resolve another puzzle, i.e., long-duration
  (up to 20 hr) γ-rays flares. We suggest that, in addition to DSA,
  stochastic acceleration by plasma turbulence may also play a role,
  especially in the shock downstream region and during the early stage
  when the shock Alfvén Mach number is small.

---------------------------------------------------------
Title: Analysis of total reaction cross sections for deuterons on
    1 p-shell-nuclei
Authors: Chen, YiDi; Zhang, Yun; Lou, JianLing; Pang, DanYang; Ye,
   YanLin; Liu, Wei; Jiang, Ying; Li, Gen
2018SCPMA..61k2011C    Altcode:
  This study aims to analyze the differential cross sections (DCSs)
  of elastic scattering and total reaction cross sections (TRCSs) of the
  loosely-bound deuteron projectile impinging on 1 p-shell nuclei, such as
  <SUP>9</SUP>Be, <SUP>12</SUP>C, and <SUP>16</SUP>O, at incident energies
  ranging between 10.6 and 171 MeV using the continuum discretized coupled
  channel (CDCC) method. By fitting the experimental data for the DCSs
  and TRCSs, energy-dependent renormalization factors for the real and
  imaginary parts of the nucleon-nucleus optical-model potentials deduced
  from the studies proposed by Koning and Delaroche (KD02) and by Watson,
  Singh, and Segel (WSS), are obtained. It is found that with the WSS
  potential, which was obtained specifically for 1 p-shell nuclei, the
  CDCC calculations can simultaneously reproduce both the DCSs and the
  TRCSs. The results show that it is important to choose appropriate
  optical potentials to describe deuteron-induced reactions.

---------------------------------------------------------
Title: Late Paleozoic to early Triassic multiple roll-back and
    oroclinal bending of the Mongolia collage in Central Asia
Authors: Xiao, Wenjiao; Windley, Brian F.; Han, Chunming; Liu, Wei;
   Wan, Bo; Zhang, Ji'en; Ao, Songjian; Zhang, Zhiyong; Song, Dongfang
2018ESRv..186...94X    Altcode:
  The architecture and mechanics of an orogen can be understood in terms
  of a system of collages that are characterized by a complex assemblage
  of multiple components, but the fundamental paleogeographic framework
  and the tectonic relationships between the different components are
  often insufficiently defined, because of unavailable data. The Central
  Asian Orogenic Belt (CAOB) provides an ideal opportunity to address
  the fundamental framework of paleogeography and tectonic relationships
  between the diverse and many components in this huge collage. In this
  paper we review several lines of available evidence, which enable us to
  propose a new tectonic model of huge roll-back in the formation of the
  accretionary tectonics of the Mongolian collage in Central Asia. In the
  early Paleozoic the Mongolia collage comprised the southern Siberian and
  the Tuva-Mongol Oroclines. The Siberia Craton and the Mongolia collage
  jointly formed a giant "tadpole-shape" within the Paleo-Asian and
  Panthanlassic oceans; its head (Siberia) was to the south, and the tail
  (Tuva-Mongol) to the northwest. The structures and tectonic zonation of
  the Mongolia collage are characteristic of multiple arcs, which have
  been separately described in detail in different segments southwards
  from the Southern Siberia-East Sayan, West Sayan-Gorny Altai-Chara,
  via the Lake Zone-Junggar-Tianshan, Gobi Altai-Beishan-Alxa, to the
  Manlay-Hegenshan-Baolidao-Solonker segments. Almost all segments
  underwent Early Paleozoic to Permian, or even Triassic, frontal
  subduction and accretion, while rifting in the Late Carboniferous
  to Permian or Triassic occurred in the outward/oceanward (westward)
  advancing Mongolian collage. Therefore, we suggest that a huge complex
  roll-back, active from the Carboniferous to Permian or even to late
  Triassic, facilitated the formation of the Mongolian collage. The
  outward multiple roll-back process was compatible and almost coeval
  with the start of the Tuva-Mongol Orocline and rotation of the Siberian
  Craton, as confirmed by paleomagnetic and structural data. During the
  roll-back processes an archipelago paleogeography was formed behind the
  frontal subduction and accretion, in which independent arcs or terranes
  were amalgamated or collided to form composite arcs or terranes either
  simultaneously or at slightly different times. The roll-back process was
  affected by the collision of the Kazakhstan collage along the Chara and
  Karamay zones in the Early Permian, the collision of the Tarim Craton
  along the South Tianshan zone in the Early Permian, the collision of the
  Dunhuang Block along the Liuyuan zone in the Early Permian-Triassic, the
  collision of the Alxa block along the Qugan Qulu zone in the Permian,
  and the collision of the North China Craton along the Solonker zone
  in the Middle-Late Triassic. The tectonic styles and architecture of
  accretionary orogenic belts like the CAOB are characterized both by
  the amalgamation of multiple terranes and by oroclinal bending. The
  systematic anatomy of the multiple roll-back processes and their
  interactions with the adjacent collages shed light on the evolving
  orogenic architecture and the crustal accretionary history of orogens.

---------------------------------------------------------
Title: Investigating Sub-Pixel 45-Second Periodic Wobble in SDO/AIA
    Data from January to August 2012
Authors: Yuan, Ding; Liu, Wei; Walsh, Robert
2018SoPh..293..147Y    Altcode:
  Artifacts could mislead interpretations in astrophysical observations. A
  thorough understanding of an instrument will help in distinguishing
  physical processes from artifacts. In this article, we investigate an
  artifact of the Atmospheric Imaging Assembly (AIA) onboard the Solar
  Dynamics Observatory. Time-series data and wavelet spectra revealed
  periodic intensity perturbations in small regions over the entire
  image in certain AIA extreme ultraviolet (EUV) passbands at a period of
  about 45 seconds. These artificial intensity variations are prominently
  detected in regions with sharp intensity contrast, such as sunspot light
  bridges. This artifact was caused by a periodic pointing wobble of the
  two AIA telescopes ATA 2 (193 and 211 Å channels) and ATA 3 (171 Å
  and UV channels), to a lesser extent, while the other two telescopes
  were not found to be affected. The peak-to-peak amplitude of the wobble
  was about 0.2 pixel in ATA 2 and 0.1 pixel in ATA 3. This artifact was
  intermittent and affected the data of seven months from 18 January to 28
  August 2012, as a result of a thermal adjustment to the telescopes. We
  recommend that standard pointing-correction techniques, such as local
  correlation tracking, should be applied before any detailed scientific
  analysis that requires sub-pixel pointing accuracy. Specifically, this
  artificial 45-second periodicity was falsely interpreted as abnormal
  sub-minute oscillations in a light bridge of a sunspot (Yuan and Walsh
  in Astron. Astrophys.594, A101, 2016).

---------------------------------------------------------
Title: High-temperature inter-mineral Cr isotope fractionation: A
    comparison of ionic model predictions and experimental investigations
    of mantle xenoliths from the North China Craton
Authors: Shen, Ji; Qin, Liping; Fang, Ziyao; Zhang, Yingnan; Liu,
   Jia; Liu, Wei; Wang, Fangyue; Xiao, Yan; Yu, Huimin; Wei, Shiqiang
2018E&PSL.499..278S    Altcode:
  Recent works have proposed that chromium (Cr) isotopes could
  be fractionated during peridotite partial melting and basaltic
  magma crystallization. However, until now, inter-mineral Cr
  isotope fractionation behavior for major mantle minerals has been
  poorly constrained. To investigate the mechanism and magnitude of
  equilibrium inter-mineral Cr isotope fractionation and to explore its
  implications for planetary mantle and crust lithology evolutions, we
  performed a systematic study of equilibrium Cr isotope fractionation
  between major mantle minerals by coupling theoretical ionic modeling
  with laboratory isotope analyses of natural samples and Cr valence
  determinations by X-ray absorption near edge spectroscopy (XANES). The
  ionic model considers both charges and coordination environments of Cr
  species in mantle minerals, which have proven to be critical factors
  affecting inter-mineral isotope fractionation. The ionic modeling
  results predict a general order of spinel (Spl) &gt; pyroxene (Py)
  ≥ olivine (Ol) in <SUP>53</SUP>Cr/<SUP>52</SUP>Cr. Systematic
  Cr isotope analyses of coexisting mantle minerals of seventeen
  peridotite xenoliths from Beiyan in the North China craton were
  performed. Chromium isotope results for different mineral pairs of
  lherzolites (e.g., Δ<SUP>53</SUP>Cr<SUB>Spl-Ol</SUB> of 0.11‰ to
  0.16‰, Δ<SUP>53</SUP>Cr<SUB>Spl-Py</SUB> of 0.04‰ to 0.11‰
  and Δ<SUP>53</SUP>Cr<SUB>Py-Ol</SUB> of 0.05‰ to 0.10‰ at 870
  °C to 970 °C), document measurable and systematic inter-mineral
  Cr isotope fractionation, in excellent agreement with the modeling
  results predicted with XANES-determined Cr<SUP>2+</SUP>/ΣCr
  values of the mineral separates. This fractionation order could
  essentially account for Cr isotope behaviors during partial melting
  and magmatic crystallization observed in terrestrial peridotites
  and lunar basalts. <P />In contrast, we found that metasomatisms
  could influence Cr isotope compositions of minerals from Beiyan
  metasomatized clinopyroxene- (Cpx-) rich lherzolites and wehrlites by
  means of mineral-melt interaction and/or kinetic diffusion, leading
  to disequilibrium inter-mineral Cr isotope fractionation.

---------------------------------------------------------
Title: Statistical Correlation Analysis of Field-Aligned Currents
    Measured by Swarm
Authors: Yang, J. -Y.; Dunlop, M. W.; Lühr, H.; Xiong, C.; Yang,
   Y. -Y.; Cao, J. -B.; Wild, J. A.; Li, L. -Y.; Ma, Y. -D.; Liu, W. -L.;
   Fu, H. -S.; Lu, H. -Y.; Waters, C.; Ritter, P.
2018JGRA..123.8170Y    Altcode:
  We investigate the statistical, dual-spacecraft correlations of
  field-aligned current (FAC) signatures between two Swarm spacecraft. For
  the first time, we infer the orientations of the current sheets of FACs
  by directly using the maximum correlations obtained from sliding data
  segments. The current sheet orientations are shown to broadly follow
  the mean shape of the auroral boundary for the lower latitudes and that
  these are most well ordered on the dusk side. Orientations at higher
  latitudes are less well ordered. In addition, the maximum correlation
  coefficients are explored as a function of magnetic local time and in
  terms of either the time shift (δt) or the shift in longitude (δlon)
  between Swarms A and C for various filtering levels and choice of
  auroral region. We find that the low-latitude FACs show the strongest
  correlations for a broad range of magnetic local time centered on dawn
  and dusk, with a higher correlation coefficient on the dusk side and
  lower correlations near noon and midnight. The positions of maximum
  correlation are sensitive to the level of low-pass filter applied to
  the data, implying temporal influence in the data. This study clearly
  reflects the two different domains of FACs: small-scale (some tens
  of kilometers), which are time variable, and large-scale (&gt;50
  km), which are rather stationary. The methodology is deliberately
  chosen to highlight the locations of small-scale influences that are
  generally variable in both time and space. We may fortuitously find a
  potential new way to recognize bursts of irregular pulsations (Pi1B)
  using low-Earth orbit satellites.

---------------------------------------------------------
Title: GeV-TeV γ -ray energy spectral break of BL Lac objects
Authors: Zhong, W.; Liu, W. G.; Zheng, Y. G.
2018Ap&SS.363..179Z    Altcode: 2018arXiv180800599Z
  In this paper, we compile the very-high-energy and high-energy spectral
  indices of 43 BL Lac objects from the literature. Based on a simple
  math model, Δ Γ_{obs}= α {{{z}}}+β , we present evidence for the
  origin of an observed spectral break that is denoted by the difference
  between the observed very-high-energy and high-energy spectral indices,
  Δ Γ_{obs}. We find by linear regression analysis that α ≠ 0 and
  β ≠ 0. These results suggest that the extragalactic background
  light attenuation and the intrinsic curvature dominate on the GeV-TeV
  γ -ray energy spectral break of BL Lac objects. We argue that the
  extragalactic background light attenuation is an exclusive explanation
  for the redshift evolution of the observed spectral break.

---------------------------------------------------------
Title: A Truly Global Extreme Ultraviolet Wave from the SOL2017-09-10
    X8.2+ Solar Flare-Coronal Mass Ejection
Authors: Liu, Wei; Jin, Meng; Downs, Cooper; Ofman, Leon; Cheung,
   Mark C. M.; Nitta, Nariaki V.
2018ApJ...864L..24L    Altcode: 2018arXiv180709847L
  We report Solar Dynamics Observatory/Atmospheric Imaging Assembly
  (SDO/AIA) observations of an extraordinary global extreme ultraviolet
  (EUV) wave triggered by the X8.2+ flare-CME eruption on 2017 September
  10. This was one of the best EUV waves ever observed with modern
  instruments, yet it was likely the last one of such magnitudes of
  Solar Cycle 24 as the Sun heads toward the minimum. Its remarkable
  characteristics include the following. (1) The wave was observed,
  for the first time, to traverse the full-Sun corona over the entire
  visible solar disk and off-limb circumference, manifesting a truly
  global nature, owing to its exceptionally large amplitude, e.g.,
  with EUV enhancements by up to 300% at 1.1 {R}<SUB>⊙ </SUB> from
  the eruption. (2) This leads to strong transmissions (in addition to
  commonly observed reflections) in and out of both polar coronal holes
  (CHs), which are usually devoid of EUV waves. It has elevated wave
  speeds &gt;2000 {km} {{{s}}}<SUP>-1</SUP> within the CHs, consistent
  with the expected higher fast-mode magnetosonic wave speeds. The CHs
  essentially serve as new “radiation centers” for the waves being
  refracted out of them, which then travel toward the equator and collide
  head-on, causing additional EUV enhancements. (3) The wave produces
  significant compressional heating to local plasma upon its impact,
  indicated by long-lasting EUV intensity changes and differential
  emission measure increases at higher temperatures (e.g., {log}T=6.2)
  accompanied by decreases at lower temperatures (e.g., {log}T=6.0). These
  characteristics signify the potential of such EUV waves for novel
  magnetic and thermal diagnostics of the solar corona on global scales.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Low-mass black holes in Sy1
    galaxies. II. SDSS-DR7 (Liu+, 2018)
Authors: Liu, H. -Y.; Yuan, W.; Dong, X. -B.; Zhou, H.; Liu, W. -J.
2018yCat..22350040L    Altcode:
  A new sample of 204 low-mass black holes (LMBHs) in active galactic
  nuclei (AGNs) is presented with black hole masses in the range of
  (1-20)x10<SUP>5</SUP>M<SUB>ȯ</SUB>. The AGNs are selected through
  a systematic search among galaxies in the Seventh Data Release
  (DR7) of the Sloan Digital Sky Survey (SDSS), and careful analyses
  of their optical spectra and precise measurement of spectral
  parameters. Combining them with our previous sample selected from
  SDSS DR4 makes it the largest LMBH sample so far, totaling over 500
  objects. Some of the statistical properties of the combined LMBH AGN
  sample are briefly discussed in the context of exploring the low-mass
  end of the AGN population. Their X-ray luminosities follow the extension
  of the previously known correlation with the [OIII] luminosity. The
  effective optical-to-X-ray spectral indices α<SUB>OX</SUB>, albeit
  with a large scatter, are broadly consistent with the extension of the
  relation with the near-UV luminosity L<SUB>2500Å</SUB>. Interestingly,
  a correlation of α<SUB>OX</SUB> with black hole mass is also found,
  with αOX being statistically flatter (stronger X-ray relative to
  optical) for lower black hole masses. Only 26 objects, mostly radio
  loud, were detected in radio at 20cm in the FIRST survey, giving a
  radio-loud fraction of 4%. The host galaxies of LMBHs have stellar
  masses in the range of 10<SUP>8.8</SUP>-10<SUP>12.4</SUP>M<SUB>ȯ</SUB>
  and optical colors typical of Sbc spirals. They are dominated by
  young stellar populations that seem to have undergone continuous star
  formation history. <P />(5 data files).

---------------------------------------------------------
Title: The nature of the lithium enrichment in the most Li-rich
    giant star
Authors: Yan, Hong-Liang; Shi, Jian-Rong; Zhou, Yu-Tao; Chen,
   Yong-Shou; Li, Er-Tao; Zhang, Suyalatu; Bi, Shao-Lan; Wu, Ya-Qian;
   Li, Zhi-Hong; Guo, Bing; Liu, Wei-Ping; Gao, Qi; Zhang, Jun-Bo; Zhou,
   Ze-Ming; Li, Hai-Ning; Zhao, Gang
2018NatAs...2..790Y    Altcode: 2018arXiv180900187Y; 2018NatAs.tmp..111Y
  About 1% of giant stars<SUP>1</SUP> have anomalously high Li
  abundances (A<SUB>Li</SUB>) in their atmospheres, conflicting
  directly with the prediction of standard stellar evolution
  models<SUP>2</SUP>. This finding makes the production and evolution
  of Li in the Universe intriguing, not only in the sense of Big Bang
  nucleosynthesis<SUP>3,4</SUP> or the interstellar medium<SUP>5</SUP>,
  but also for the evolution of stars. Decades of effort have been put
  into explaining why such extreme objects exist<SUP>6-8</SUP>, yet the
  origins of Li-rich giants are still being debated. Here, we report the
  discovery of the most Li-rich giant known to date, with a very high
  A<SUB>Li</SUB> of 4.51. This rare phenomenon was observed coincidentally
  with another short-term event: the star is experiencing its luminosity
  bump on the red giant branch. Such a high A<SUB>Li</SUB> indicates that
  the star might be at the very beginning of its Li-rich phase, which
  provides a great opportunity to investigate the origin and evolution
  of Li in the Galaxy. A detailed nuclear simulation is presented with
  up-to-date reaction rates to recreate the Li enrichment process in
  this star. Our results provide tight constraints on both observational
  and theoretical points of view, suggesting that low-mass giants can
  internally produce Li to a very high level through <SUP>7</SUP>Be
  transportation during the red giant phase.

---------------------------------------------------------
Title: Black hole as fireplace: limited communications across
    the horizon
Authors: Shu, Liangsuo; Cui, Kaifeng; Liu, Xiaokang; Liu, Zhichun;
   Liu, Wei
2018arXiv180802642S    Altcode:
  An insightful viewpoint was proposed by Susskind about AMPS firewall:
  the region behind the firewall does not exist and the firewall
  is an extension of the singularity. In this work, we provided a
  possible picture of this idea by combining Newman's complex metric and
  Dvali-Gomez BEC black holes, which are Bose-Einstein condensates of N
  gravitons. The inner space behind the horizon is a realized imaginary
  space encrusted by the real space outside the horizon. In this way,
  the singularity extents to the horizon to make a firewall for the
  infalling observer. Some gravitons escape during the fluctuation of the
  BEC black hole, resulting in a micro-transparent horizon which makes
  the firewall exposes slightly to an observer outside the horizon. This
  picture allows limited communications across the horizon.

---------------------------------------------------------
Title: Three-dimensional Velocity Measurements in Solar Prominence
    Bubbles and Combined Kelvin-Helmholtz/Rayleigh-Taylor Instability
Authors: Berger, Thomas; Hillier, Andrew; Liu, Wei
2018cosp...42E.293B    Altcode:
  We present measurements of flow velocities in solar prominences that
  display so-called "prominence bubble" events. Prominence bubbles
  are large-scale buoyant intrusions into prominences that rise from
  below and penetrate into the overlying plasma. They are believed to
  be due to magnetic flux emergence below prominences and can trigger
  Rayleigh-Taylor and Kelvin-Helmholtz instability flows as they interact
  with the overlying prominence. Prominence bubbles frequently result
  in the formation of plumes that rise into, or entirely through, the
  overlying prominence. This presents a mechanism for increasing magnetic
  flux and helicity in the associated coronal magnetic flux tubes,
  which are key for their eventual loss of equilibrium and eruptions
  as coronal mass ejections (CMEs). In this presentation, Hinode/Solar
  Optical Telescope (SOT) and Interface Region Imaging Spectrograph (IRIS)
  observations are analyzed to infer three-dimensional flow vectors
  in the "boundary layer" above several prominence bubble events. IRIS
  Doppler velocity measurements indicate flow speeds of 50-100 km/sec
  perpendicular to the sky plane, consistent with flow speeds inferred
  from combined Kelvin-Helmholtz/Rayleigh-Taylor instability analysis
  using typical quiescent prominence density and magnetic flux density
  values. With these typical values, flow speeds and magnetic flux
  densities within the bubbles can be inferred to be on the order of
  100 km/sec and 10 Gauss, respectively. We discuss the implications of
  these novel results, and in particular, the potential for strong shear
  flows at the bubble boundary to trigger Kelvin-Helmholtz instability
  waves that develop into large-scale Rayleigh-Taylor instability plumes.

---------------------------------------------------------
Title: High resolution observations of prominence rotation by Hinode
    and IRIS
Authors: Okamoto, Joten; Liu, Wei
2018cosp...42E2498O    Altcode:
  Fine structures of prominences, especially threads, and their dynamics
  provide physical information about the magnetic configuration and
  property in the corona. Here we report two events of prominence rotation
  observed by the Hinode and IRIS satellites. In the first event, we found
  transverse motions of brightening threads at speeds up to 55 km/s seen
  in the plane of the sky. Such motions appeared as sinusoidal space-time
  trajectories with a typical period of 390 s, which is consistent
  with plane-of-sky projections of rotational motions. At least 15
  episodes of such motions occurred in two days, none associated with
  any eruption. For these episodes, the plane-of-sky speed is linearly
  correlated with the vertical travel distance, suggestive of a constant
  angular speed. In the second event, spectral data taken by IRIS showed
  strong blueshifts in the top portion of the prominence with a speed
  of 30-40 km/s, while redshifts of similar speeds were detected at the
  bottom. Line width of the bright threads were significantly larger
  than those of stationary threads. These behaviors indicate rotations of
  helical prominence threads. We interpreted the activations as evidence
  of unwinding motions caused by magnetic reconnection between twisted
  prominence fields and ambient coronal fields.

---------------------------------------------------------
Title: Global Magnetohydrodynamics Simulation of EUV Waves and Shocks
    from the X8.2 Eruptive Flare on 2017 September 10
Authors: Jin, Meng; Liu, Wei; Cheung, Mark; Nitta, Nariaki; Manchester,
   Ward; Ofman, Leon; Downs, Cooper; Petrosian, Vahe; Omodei, Nicola
2018shin.confE.207J    Altcode:
  As one of the largest flare-CME eruptions during solar cycle 24, the
  2017 September 10 X8.2 flare event is associated with spectacular
  global EUV waves that transverse almost the entire visible solar
  disk, a CME with speed &gt; 3000 km/s, which is one of the fastest
  CMEs ever recorded, and &gt;100 MeV Gamma-ray emission lasting for
  more than 12 hours. All these unique observational features pose new
  challenge on current numerical models to reproduce the multi-wavelength
  observations. To take this challenge, we simulate the September 10 event
  using a global MHD model (AWSoM: Alfven Wave Solar Model) within the
  Space Weather Modeling Framework and initiate CMEs by Gibson-Low flux
  rope. We conduct detailed comparisons of the synthesized EUV images with
  SDO/AIA observations of global EUV waves. We find that the simulated
  EUV wave morphology and kinematics are sensitive to the orientation
  of the initial flux rope introduced to the source active region. An
  orientation with the flux-rope axis in the north-south direction
  produces the best match to the observations, which suggests that EUV
  waves may potentially be used to constrain the flux-rope geometry for
  such limb or behind-the-limb eruptions that lack good magnetic field
  observations. We also compare observed and simulated EUV intensities
  in multiple AIA channels to perform thermal seismology of the global
  corona. Furthermore, we track the 3D CME-driven shock surface in the
  simulation and derive the time-varying shock parameters together with
  the dynamic magnetic connectivity between the shock and the surface
  of the Sun, with which we discuss the role of CME-driven shocks in
  the long-duration Gamma-ray events.

---------------------------------------------------------
Title: Development of a compact readout system for optical CCD in
    Higashi-Hiroshima Observatory
Authors: Liu, Wei; Sako, Shigeyuki; Kawabata, Koji; Shi, Sheng-Cai;
   Yoshida, Michitoshi; Utsumi, Yousuke
2018SPIE10709E..1XL    Altcode:
  We developed a new CCD readout system for the Kanata 1.5m telescope in
  Higashi-Hiroshima Astronomical Observatory, Hiroshima University, Japan,
  based on the system originally developed by the Kiso Array Controller
  (KAC) project. In this development we aim at reducing the size and
  the cost of the system. The system consists of CCD drive circuit,
  three-order low-pass filters, differential input A/D converter,
  FPGA, LVDC board, and can be operated by Linux host. We report the
  current design and performances of this system, and the future work
  as well. This readout system will be easily applicable to many other
  astronomical instruments.

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Title: High-Energy Aspects of Solar Flares: Recent Advances in
    Observations and Models
Authors: Liu, Wei; Effenberger, Frederic; Petrosian, Vahe; Nitta,
   Nariaki; Omodei, Nicola; Rubio da Costa, Fatima; Pesce-Rollins,
   Melissa; Jin, Meng; Allafort, Alice
2018cosp...42E2050L    Altcode:
  Solar flares are one of the most spectacular manifestations of
  solar activity with significant space-weather impacts. They also
  serve as a unique laboratory for probing the underlying physics of
  wide-ranging processes, including magnetic reconnection, generation
  of plasma turbulence and shocks, particle acceleration, and plasma
  heating. Solar flares thus bear important implications for physically
  similar phenomena elsewhere in the universe, such as laboratory plasmas,
  planetary magnetospheres, and flares on other stars or near compact
  objects. In this presentation, we review recent observational and
  modeling advances in solar flare research, with a focus on high-energy
  aspects. Special attention will be paid to imaging and spectroscopic
  observations, e.g., of long-duration and behind-the-limb gamma-ray
  flares detected by Fermi, of coronal reconnection sites seen by
  RHESSI, SDO, Hinode, and IRIS, and of the flaring lower atmosphere
  (chromosphere and transition region) seen by IRIS. We will discuss
  broad physical connections of flares to other phenomena on the Sun
  (to a much greater extent than conventionally thought), such as the
  correlation between quasi-periodic flare pulsations (seen from radio to
  hard X-rays) and various MHD waves (some are directly imaged). We will
  also review relevant modeling efforts to explain these observations,
  focusing on a hybrid model of stochastic (by turbulence) plus shock
  acceleration of particles, as well as combined kinetic and radiative
  hydrodynamic simulations.

---------------------------------------------------------
Title: Interaction between cool material from Sun-grazing comets
    and the low corona
Authors: Jia, Yingdong; Pesnell, William; Liu, Wei; Downs, Cooper;
   Bryans, Paul
2018cosp...42E1613J    Altcode:
  Sun-grazing comets dive into altitudes lower than 1 solar radius from
  the chromosphere. Cool materials of temperature lower than 10 ^{3}K
  explode from the comet into the 10 ^{6} K corona. These materials
  undergone various stages of rapid chemical reactions in scales of
  seconds to minutes. Such reactions Structures in such images of
  various wavelengths indicate strong variation in ambient conditions
  of the corona. We combine three numerical models: low corona model,
  particle transportation model, and cometary plasma interaction model
  into one framework to model the interaction of Sun-grazing comets in the
  low corona. In our framework, cometary vapor are ionized via multiple
  channels, and then detained by the coronal magnetic field. In seconds,
  these ions are further ionized into their highest charge state, which
  is revealed by certain emission lines. Constrained by coronal graphs
  and cometary interaction images, we apply our framework to trace back
  to the local condition of the ambient corona, and its spatial/time
  variation. Our frame work is able to resolve structures of sub-million
  meters to tens of million meters. Once trained by multiple stages of
  the comet's journey in the low corona, this framework can identify the
  fine spatial variations in plasma density and magnetic field intensity,
  which may be visible to future close-up observations.

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Title: Are "Solar Tornadoes" Really Rotating?
Authors: Liu, Wei; Chye Low, Boon; Okamoto, Joten; Berger, Thomas
2018cosp...42E2053L    Altcode:
  Solar "tornadoes" have been proposed to explain certain vertical
  structures in prominences that exhibit apparent rotations. Yet, it
  remains highly controversial whether such motions are real rotations
  or transverse oscillations. We present a statistical study of IRIS
  observations that reveal no clear evidence of systematic or coherent
  rotations, which would otherwise result in opposite Doppler shifts,
  i.e., blueshifts on the one side of the vertical structure and redshifts
  on the other, which were not found in our sample of "tornadoes". In
  addition, we find in one particular case observed by SDO/AIA that the
  "tornado" disappeared upon the impact of an eruption that pushed
  its mass away along a primarily horizontal trajectory (presumably
  along magnetic field lines). This "tornado" shortly reformed with
  the replenishment of material from the return flow of some of the
  displaced mass back to its original location, at the dips of local
  magnetic field lines, followed by back and forth transverse oscillations
  around the dips. Such observations from both IRIS and AIA suggest that,
  at least for the cases being analyzed here, the apparent oscillatory
  motions of "tornadoes" are a result of longitudinal oscillations
  (like a pendulum) of dense and heavy prominence material about the
  local minimum of gravitational potential at the magnetic dips, an
  interpretation proposed and supported by a number of authors.

---------------------------------------------------------
Title: Cool Material in the Hot Solar Corona and the
    Chromosphere-Corona Mass Cycle
Authors: Liu, Wei; Vial, Jean-Claude; Antolin, Patrick; Sun, Xudong;
   Berger, Thomas
2018cosp...42E2052L    Altcode:
  In the million-degree hot and tenuous solar corona, under favorable
  conditions, some mass can undergo a radiative cooling instability and
  condense into material of 100 times cooler in two distinct forms -
  prominences and coronal rain. Being at similar temperatures, they
  exhibit contrasting morphologies and behaviors: a quiescent prominence
  usually consists of numerous long-lasting, filamentary downflow
  threads, while coronal rain consists of transient mass blobs falling
  at comparably higher speeds along well-defined, curved paths (e.g.,
  guided by coronal loops). We report recent imaging and spectroscopic
  observations from SDO/AIA and IRIS of a hybrid prominence-coronal
  rain complex structure that suggest different magnetic environments
  being responsible for such distinctions. We also present an ensemble
  of observations of the so-called funnel prominences that reside near
  the dips of magnetic funnels. Regardless of their morphological and
  behavioral differences, a large fraction of prominence and coronal
  rain material eventually falls back to the chromosphere and serves as
  the return flow of the so-called chromosphere-corona mass cycle (the
  other half of this cycle is the upward transport of heated mass from
  the chromosphere to the corona). We estimate the downflow mass fluxes
  in prominences and coronal rain, and compare them with the coronal
  mass budget in this cycle and with the mass loss to the solar wind
  and coronal mass ejections (CMEs). We will discuss the broad physical
  implications of these observations for fundamental questions, such as
  coronal heating and beyond.

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Title: Direct retrieval of stress and evaporation from space
    observations
Authors: Liu, W. Timothy; Xie, Xiaosu
2018cosp...42E2049L    Altcode:
  Momentum flux (stress) and latent heat flux (evaporation) at ocean
  surface are transported by turbulence, which is small scale random
  process generated/subdued by wind shear and buoyancy (vertical wind
  and density gradients). Turbulence is difficult to measure and,
  traditionally, transfer coefficients (bulk parameterization formula)
  are used to related them the mean parameter measured on ships, such
  as, wind and humidity in air, and temperature and current at ocean
  surface. Satellite sensors measure radiance and backscatter at the
  ocean surface and there is no critical reason to reproduce measurements
  of meteorological and oceanic sensors on ships. We show that direct
  retrieval of latent heat flux from the radiance measured by microwave
  radiometers mitigate errors caused by the multiplication of retrieval
  uncertainties of wind to those of temperature or humidity while facing
  the uncertainty of the transfer coefficient. We will address the
  uncertainty of retrieving strong wind caused by backscatter saturation
  and the change behavior of the transfer coefficient under tropical
  cyclone by direct stress retrieval. We will show that scatterometers
  measurements represent the vector difference between wind and current,
  the characteristic of stress rather than wind. As different from the
  prevailing winds, stress spins down the mesoscale eddies and reduce
  the kinetic energy into the ocean.

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Title: A Long-Lived Coronal Condensation Site Lasting Eight Months
Authors: Sun, Xudong; Liu, Wei; Yu, Sijie
2018cosp...42E3295S    Altcode:
  Cool plasma material, such as prominences or coronal rain, can
  form in-situ by condensation in the solar corona due to a runaway
  radiative cooling instability (a.k.a. thermal non-equilibrium). Recent
  observations and numerical simulations suggest that such condensations
  are quite common. In quiet-Sun regions, they occur preferentially
  in locations where magnetic field is weak (e.g., null points) or
  discontinuous (e.g., current sheets). Such events usually have short
  lifetimes of hours to days. Surprisingly, we observed a high-latitude
  condensation site lasting over eight months in 2014 with recurrent and
  episodic condensations fueling a funnel-shaped prominence. Uplifting
  V-shaped features suggest sustaining reconnection inside the funnel. We
  analyze the coronal magnetic topology to investigate the necessary
  condition of such a long-lived condensation site. We find that the
  site was directly above a poleward photospheric flux surge when
  the polar field polarity was close to its solar cycle reversal. The
  large-scale magnetic cancellation front may have sustained interchange
  reconnection at this location, creating suitable conditions for coronal
  plasma condensation.

---------------------------------------------------------
Title: Modeling Flare-Generated Quasi-Periodic Propagating Fast
    Magnetosonic Waves Observed by SDO/AIA
Authors: Ofman, Leon; Liu, Wei
2018cosp...42E2492O    Altcode:
  Fast-propagating (phase speeds of ∼1000 km/s) quasi-periodic,
  fast-mode wave (QFPs) accompanying many solar flares have been
  discovered by SDO/AIA (Liu et al. 2011). They typically propagate in
  funnel-like structures associated with the expanding magnetic field
  topology of the active regions (ARs), driven by flare-pulsations
  duration of impulsive phase. The fast magnetosonic waves provide
  information on the magnetic, density, and temperature structure
  through coronal seismology. While all previously reported QFP waves
  originate from a single localized flaring source, we report the first
  AIA observation and 3D MHD modeling of counter-QFPs originating from
  two 'sympathetic' flares. The waves are excited at the two sources
  associated with flare locations and connected by magnetic loops,
  by time-depended forcing, constrained by the spatial (localized) and
  quasi-periodic temporal evolution of the flare pulsations. With the
  aid of 3D MHD modeling we investigate the excitation, propagation,
  nonlinearity, and interaction of the counter-propagating waves for
  a range of key parameters, such as the properties of the flaring
  sources and the background magnetic topology. In addition to QFPs,
  we find evidence of associated waves, such as trapped fast (kink)
  modes in coronal loops, and slow mode waves propagating along the
  AR loops. Our model results are in qualitative agreement with the
  AIA-observed counter propagating waves providing the first direct
  evidence of counter-propagating fast magnetosonic waves that carry
  significant energy flux in low-corona magnetic structures.

---------------------------------------------------------
Title: The Best and Last of Solar Cycle 24 - The Global EUV Wave from
the X8 Flare-CME Eruption on 2017-Sept-10: SDO/AIA Observations and
    Data-constrained Simulations
Authors: Liu, Wei; Ofman, Leon; Nitta, Nariaki; Cheung, Mark; Downs,
   Cooper; Jin, Meng
2018cosp...42E2051L    Altcode:
  Global extreme ultraviolet (EUV) waves are commonly associated with
  coronal mass ejections (CMEs) and flares. One particular EUV wave
  that was triggered by the X8 flare-CME eruption on 2017 September
  10 was extraordinary - one of the best EUV waves ever observed with
  modern instruments (e.g., SDO/AIA and GOES/SUVI), yet likely the last
  one of such magnitudes in Cycle 24 as the Sun heads toward the solar
  minimum. We present here detailed analysis of SDO/AIA observations
  of this event and comparison with high-fidelity, data-constrained MHD
  simulations using the University of Michigan Alfven Wave Solar Model
  (AWSoM). Observational highlights include: (1) The EUV wave traverses
  almost the entire visible solar disk and circumference, manifesting its
  truly global nature. This vast range is mainly due to the exceptionally
  large wave amplitude, with EUV intensity changes by up to a factor of
  3 (as opposed to, e.g., 30% for moderate events). (2) The large wave
  amplitude also leads to the novel detection of strong transmission
  components (in addition to commonly observed reflections) into and
  through both polar coronal holes, at elevated apparent wave speeds up
  to 2600 km/s. (3) The wave also produces significant heating, indicated
  by long-lasting EUV intensity changes. As such, this EUV wave offers
  unique magnetic and thermal diagnostics of the global, CME-spawning
  corona. Our MHD simulations have largely reproduced the observed
  features. We find that the simulated EUV wave morphology and kinematics
  are sensitive to the orientation of the initial flux rope introduced to
  the host active region. An orientation with the flux-rope axis in the
  north-south direction produces the best match to the observations. This
  suggests that EUV waves may potentially be used to constrain the
  flux-rope geometry for such limb or behind-the-limb eruptions, whose
  source-region magnetic fields cannot be directly observed, and thus
  offer useful implications for space-weather predictions.

---------------------------------------------------------
Title: On the Nature of Funnel Prominences
Authors: Liu, Wei; Chye Low, Boon; Berger, Thomas
2018cosp...42E2054L    Altcode:
  It has been proposed that prominences are manifestations of a
  magneto-thermal convection process that involves ever-present dynamic
  descents of cool material threads and upflows of hot bubbles and plumes
  (Berger et al. 2011 Nature). On global scales, prominences may play
  an important role as the return flows of the chromosphere-corona
  mass cycle. A critical step in this cycle is the condensation of
  million-degree coronal plasma into T&lt;10,000 K prominence material by
  radiative cooling instability. Direct observational evidence has been
  lacking for decades, a situation that has recently changed, especially
  with the advent of the SDO mission. We present here SDO/AIA observations
  of runaway cooling in coronal loops leading to condensation at magnetic
  dips and formation of funnel-shaped prominences (e.g., Liu et al. 2012,
  2014; Berger et al. 2012 ApJL). We find that a macroscopically quiescent
  prominence is microscopically dynamic, involving the passage (through
  condensation and drainage) of a significant mass of typically 10^{15}
  gram/day (comparable to the mass of a typical CME). This picture
  is further supported by the theoretical development on spontaneous
  formation of current sheets and condensations (Low et al. 2012a, b,
  ApJ). Such funnel prominences, usually small in size, can constitute
  a new type of prominences. We suggest that similar processes could
  produce elementary building blocks of large-scale quiescent prominences
  in filament channels.

---------------------------------------------------------
Title: Quasi-periodic Counter-propagating Fast Magnetosonic Wave
Trains from Neighboring Flares: SDO/AIA Observations and 3D MHD
    Modeling
Authors: Ofman, Leon; Liu, Wei
2018ApJ...860...54O    Altcode: 2018arXiv180500365O
  Since their discovery by the Solar Dynamics Observatory/Atmospheric
  Imaging Assembly (AIA) in the extreme ultraviolet, rapid (phase
  speeds of ∼1000 km s<SUP>-1</SUP>), quasi-periodic, fast-mode
  propagating (QFP) wave trains have been observed accompanying many solar
  flares. They typically propagate in funnel-like structures associated
  with the expanding magnetic field topology of the active regions
  (ARs). The waves provide information on the associated flare pulsations
  and the magnetic structure through coronal seismology (CS). The reported
  waves usually originate from a single localized source associated with
  the flare. Here we report the first detection of counter-propagating
  QFPs associated with two neighboring flares on 2013 May 22, apparently
  connected by large-scale, trans-equatorial coronal loops. We present
  the first results of a 3D MHD model of counter-propagating QFPs in
  an idealized bipolar AR. We investigate the excitation, propagation,
  nonlinearity, and interaction of the counter-propagating waves for a
  range of key model parameters, such as the properties of the sources
  and the background magnetic structure. In addition to QFPs, we also
  find evidence of trapped fast- (kink) and slow-mode waves associated
  with the event. We apply CS to determine the magnetic field strength
  in an oscillating loop during the event. Our model results are in
  qualitative agreement with the AIA-observed counter-propagating waves
  and used to identify the various MHD wave modes associated with the
  observed event, providing insights into their linear and nonlinear
  interactions. Our observations provide the first direct evidence of
  counter-propagating fast magnetosonic waves that can potentially lead
  to turbulent cascade and carry significant energy flux for coronal
  heating in low-corona magnetic structures.

---------------------------------------------------------
Title: On the PeV knee of the cosmic ray spectrum and the TeV cutoff
    of the electron spectrum
Authors: Jin, Chao; Liu, Wei; Hu, Hong-Bo; Guo, Yi-Qing
2018PhRvD..97l3005J    Altcode: 2016arXiv161108384J
  Spectra of cosmic rays (CRs), and particularly their features, contain
  a lot of important information about the astroparticle physics and the
  fundamental physics. Realizing that the 4 PeV knee of CR nuclei and
  the 1 TeV spectral cutoff of the electron share almost the same Lorentz
  factor, we propose that CRs experience a threshold interaction with a
  new light particle X abundant in the Galaxy. The interaction CR +X →CR
  +X<SUP>'</SUP> can take place when the effective energy is sufficient
  to convert it into another heavier unknown particle X<SUP>'</SUP> (as a
  representative to all possible threshold inelastic interactions). Under
  this scenario, we can reproduce the spectral break for both the nuclei
  and the electron and predict a zigzag spectrum for them. Given that
  there are great uncertainties in experiments, our model accommodates
  a wide mass range of the X from the ultralow value to around 1 eV.

---------------------------------------------------------
Title: Loop-top flows and Footpoint Motions in the September 10 2017
    X8 Flare
Authors: Reeves, Katharine; Galan, Giselle; Polito, Vanessa; Chen,
   Bin; Liu, Wei; Li, Gang
2018tess.conf30604R    Altcode:
  The September 10 2017 X8 flare was a spectacular limb event complete
  with a coronal mass ejection and a bright flare loop arcade. We examine
  the IRIS Fe XXI data from this event. Fe XXI is a coronal line that
  is formed at about 10 MK. The IRIS pointing was just south of the main
  cusp-shaped loop structure visible in AIA, but it did capture most of
  the flare arcade on the limb. We find that the majority of the emission
  in the loops is slightly red shifted, with speeds of about 20 km/s,
  probably due to chromospheric evaporation and an inclined viewing
  angle. During the period from 16:05 - 16:15 UT, we find that faint
  blue-shifted regions appear at the tops of the loops, indicating plasma
  flows of 20-60 km/s. The location where these blue shifts are observed
  moves south along the flare arcade at a speed of about 17 km/s. The AIA
  data shows flare ribbons moving to the south at the same time, though at
  much faster speeds of 70-90 km/s. We speculate that the loop-top blue
  shifts are connected to the footpoint motions and could be signatures
  of deflected flows from the reconnection outflow jet. Interestingly,
  in the minutes before the blue-shifted loop-top emission was observed,
  the Expanded Owens Valley Solar Array observed nonthermal microwave
  emission at the loop-tops indicative of particle acceleration there.

---------------------------------------------------------
Title: OH megamasers: dense gas &amp; the infrared radiation field
Authors: Huang, Yong; Zhang, JiangShui; Liu, Wei; Xu, Jie
2018JApA...39...34H    Altcode:
  To investigate possible factors related to OH megamaser formation (OH
  MM, L<SUB>H<SUB>2</SUB>O</SUB>&gt;10 L<SUB>⊙</SUB> ), we compiled
  a large HCN sample from all well-sampled HCN measurements so far
  in local galaxies and identified with the OH MM, OH kilomasers
  (L<SUB>H<SUB>2</SUB>O</SUB>&lt;10 L<SUB>⊙</SUB> , OH kMs), OH
  absorbers and OH non-detections (non-OH MM). Through comparative
  analysis on their infrared emission, CO and HCN luminosities (good
  tracers for the low-density gas and the dense gas, respectively),
  we found that OH MM galaxies tend to have stronger HCN emission
  and no obvious difference on CO luminosity exists between OH MM and
  non-OH MM. This implies that OH MM formation should be related to the
  dense molecular gas, instead of the low-density molecular gas. It
  can be also supported by other facts: (1) OH MMs are confirmed to
  have higher mean molecular gas density and higher dense gas fraction
  (L<SUB>HCN</SUB>/L<SUB>CO</SUB> ) than non-OH MMs. (2) After taking
  the distance effect into account, the apparent maser luminosity
  is still correlated with the HCN luminosity, while no significant
  correlation can be found at all between the maser luminosity and the CO
  luminosity. (3) The OH kMs tend to have lower values than those of OH
  MMs, including the dense gas luminosity and the dense gas fraction. (4)
  From analysis of known data of another dense gas tracer <SUP>HCO+</SUP>,
  similar results can also be obtained. However, from our analysis, the
  infrared radiation field can not be ruled out for the OH MM trigger,
  which was proposed by previous works on one small sample (Darling in
  ApJ 669:L9, 2007). On the contrary, the infrared radiation field should
  play one more important role. The dense gas (good tracers of the star
  formation) and its surrounding dust are heated by the ultra-violet
  (UV) radiation generated by the star formation and the heating of the
  high-density gas raises the emission of the molecules. The infrared
  radiation field produced by the re-radiation of the heated dust in
  turn serves for the pumping of the OH MM.

---------------------------------------------------------
Title: Global Magnetohydrodynamics Simulation of EUV Waves and Shocks
    from the X8.2 Eruptive Flare on 2017 September 10
Authors: Jin, Meng; Liu, Wei; Cheung, Chun Ming Mark; Nitta, Nariaki;
   Manchester, Ward; Ofman, Leon; Downs, Cooper; Petrosian, Vahe;
   Omodei, Nicola
2018tess.conf31905J    Altcode:
  As one of the largest flare-CME eruptions during solar cycle 24, the
  2017 September 10 X8.2 flare event is associated with spectacular
  global EUV waves that transverse almost the entire visible solar
  disk, a CME with speed &gt; 3000 km/s, which is one of the fastest
  CMEs ever recorded, and &gt;100 MeV Gamma-ray emission lasting for
  more than 12 hours. All these unique observational features pose new
  challenge on current numerical models to reproduce the multi-wavelength
  observations. To take this challenge, we simulate the September 10 event
  using a global MHD model (AWSoM: Alfven Wave Solar Model) within the
  Space Weather Modeling Framework and initiate CMEs by Gibson-Low flux
  rope. We conduct detailed comparisons of the synthesized EUV images with
  SDO/AIA observations of global EUV waves. We find that the simulated
  EUV wave morphology and kinematics are sensitive to the orientation
  of the initial flux rope introduced to the source active region. An
  orientation with the flux-rope axis in the north-south direction
  produces the best match to the observations, which suggests that EUV
  waves may potentially be used to constrain the flux-rope geometry for
  such limb or behind-the-limb eruptions that lack good magnetic field
  observations. We also compare observed and simulated EUV intensities
  in multiple AIA channels to perform thermal seismology of the global
  corona. Furthermore, we track the 3D CME-driven shock surface in the
  simulation and derive the time-varying shock parameters together with
  the dynamic magnetic connectivity between the shock and the surface
  of the Sun, with which we discuss the role of CME-driven shocks in
  the long-duration Gamma-ray events.

---------------------------------------------------------
Title: A Study of Detector Response and Filter Optimization for the
    Wide Field Survey Telescope
Authors: Shi, D. D.; Zheng, X. Z.; Zhao, H. B.; Lou, Z.; Wang, H. R.;
   Qian, Y.; Liu, W.; Yao, D. Z.
2018AcASn..59...22S    Altcode:
  The Wide Field Survey Telescope (WFST) is designed to be a powerful
  survey machine with prime-focus optics, 2.5 m diameter primary mirror,
  and 3 degree field of view. It is dedicated to a northern sky imaging
  survey over 20000 square degrees area. The main science goals include:
  (1) characterizing the compositions and structures of the Milky Way
  and local universe; (2) mapping the solar system objects; and (3)
  exploring variable universe. We combine the optical throughput, charge
  coupled device (CCD) quantum response, and filter transmission with
  atmospheric transmission of a 5130 m-altitude site and sky emission
  from the site of Mauna Kea to analyze the sensitivities of the telescope
  with different types of CCD response curves. Our results denote that a
  typical blue-sensitive CCD provides a higher sensitivity in observing
  blue-color objects like supernova and quasar than a typical broadband
  CCD, but a lower sensitivity in the r, i, and z bands, leading to a
  lower survey efficiency to the same u, g, r, i, and z depths. We show
  that the wavelength range of the w filter (≃ g+r+i) can be optimized
  in terms of the energy distribution of survey targets, and give the
  optimal wavelength range of 367-795 nm for the w filter. Finally,
  we present the u, g, r, i, z, and w sensitivities as a function of
  integration time to demonstrate the capability of WFST.

---------------------------------------------------------
Title: Cyclostratigraphic calibration of the Famennian stage (Late
    Devonian, Illinois Basin, USA)
Authors: Pas, Damien; Hinnov, Linda; Day, James E. (Jed); Kodama,
   Kenneth; Sinnesael, Matthias; Liu, Wei
2018E&PSL.488..102P    Altcode:
  The Late Devonian biosphere was affected by two of the most severe
  biodiversity crises in Earth's history, the Kellwasser and Hangenberg
  events near the Frasnian-Famennian (F-F) and the Devonian-Carboniferous
  (D-C) boundaries, respectively. Current hypotheses for the causes
  of the Late Devonian extinctions are focused on climate changes and
  associated ocean anoxia. Testing these hypotheses has been impeded by
  a lack of sufficient temporal resolution in paleobiological, tectonic
  and climate proxy records. While there have been recent advances
  in astronomical calibration that have improved the accuracy of the
  Frasnian time scale and part of the Famennian, the time duration
  of the entire Famennian Stage remains poorly constrained. During
  the Late Devonian, a complete Late Frasnian-Early Carboniferous
  succession of deep-shelf deposits accumulated in the epieric sea
  in Illinois Basin of the central North-American mid-continent. A
  record of this sequence is captured in three overlapping cores (H-30,
  Sullivan and H-32). The H-30 core section spans the F-F boundary;
  the Sullivan section spans almost all of the Famennian and the H-32
  section sampled spans the interval of the Upper Famennian and the D-C
  boundary. To have the best chance of capturing Milankovitch cycles,
  2000 rock samples were collected at minimum 5-cm-interval across the
  entire sequence. Magnetic susceptibility (MS) was measured on each
  sample and the preservation of climatic information into the MS signal
  was verified through geochemical analyses and low-temperature magnetic
  susceptibility acquisition. To estimate the duration of the Famennian
  Stage, we applied multiple spectral techniques and tuned the MS signal
  using the highly stable 405 kyr cycle for Sullivan and the obliquity
  cycle for the H-30 and H-32 cores. Based on the correlation between
  the cores we constructed a Famennian floating astronomical time scale,
  which indicates a duration of 13.5 ± 0.5 myr. An uncertainty of 0.5
  myr was estimated for the uncertainties arising from the errors in the
  stratigraphic position of the F-F and D-C boundaries, and the 405 kyr
  cycle counting. Interpolated from the high-resolution U-Pb radiometric
  ages available for the Devonian-Carboniferous boundary we recalibrated
  the Frasnian-Famennian boundary numerical age to 372.4 ± 0.9 Ma.

---------------------------------------------------------
Title: Identification and mitigation of narrow spectral artifacts
    that degrade searches for persistent gravitational waves in the
    first two observing runs of Advanced LIGO
Authors: Covas, P. B.; Effler, A.; Goetz, E.; Meyers, P. M.; Neunzert,
   A.; Oliver, M.; Pearlstone, B. L.; Roma, V. J.; Schofield, R. M. S.;
   Adya, V. B.; Astone, P.; Biscoveanu, S.; Callister, T. A.; Christensen,
   N.; Colla, A.; Coughlin, E.; Coughlin, M. W.; Crowder, S. G.; Dwyer,
   S. E.; Eggenstein, H. -B.; Hourihane, S.; Kandhasamy, S.; Liu, W.;
   Lundgren, A. P.; Matas, A.; McCarthy, R.; McIver, J.; Mendell, G.;
   Ormiston, R.; Palomba, C.; Papa, M. A.; Piccinni, O. J.; Rao, K.;
   Riles, K.; Sammut, L.; Schlassa, S.; Sigg, D.; Strauss, N.; Tao,
   D.; Thorne, K. A.; Thrane, E.; Trembath-Reichert, S.; Abbott, B. P.;
   Abbott, R.; Abbott, T. D.; Adams, C.; Adhikari, R. X.; Ananyeva, A.;
   Appert, S.; Arai, K.; Aston, S. M.; Austin, C.; Ballmer, S. W.; Barker,
   D.; Barr, B.; Barsotti, L.; Bartlett, J.; Bartos, I.; Batch, J. C.;
   Bejger, M.; Bell, A. S.; Betzwieser, J.; Billingsley, G.; Birch, J.;
   Biscans, S.; Biwer, C.; Blair, C. D.; Blair, R. M.; Bork, R.; Brooks,
   A. F.; Cao, H.; Ciani, G.; Clara, F.; Clearwater, P.; Cooper, S. J.;
   Corban, P.; Countryman, S. T.; Cowart, M. J.; Coyne, D. C.; Cumming,
   A.; Cunningham, L.; Danzmann, K.; Costa, C. F. Da Silva; Daw, E. J.;
   DeBra, D.; DeRosa, R. T.; DeSalvo, R.; Dooley, K. L.; Doravari, S.;
   Driggers, J. C.; Edo, T. B.; Etzel, T.; Evans, M.; Evans, T. M.;
   Factourovich, M.; Fair, H.; Galiana, A. Fernández; Ferreira, E. C.;
   Fisher, R. P.; Fong, H.; Frey, R.; Fritschel, P.; Frolov, V. V.; Fulda,
   P.; Fyffe, M.; Gateley, B.; Giaime, J. A.; Giardina, K. D.; Goetz, R.;
   Goncharov, B.; Gras, S.; Gray, C.; Grote, H.; Gushwa, K. E.; Gustafson,
   E. K.; Gustafson, R.; Hall, E. D.; Hammond, G.; Hanks, J.; Hanson,
   J.; Hardwick, T.; Harry, G. M.; Heintze, M. C.; Heptonstall, A. W.;
   Hough, J.; Inta, R.; Izumi, K.; Jones, R.; Karki, S.; Kasprzack, M.;
   Kaufer, S.; Kawabe, K.; Kennedy, R.; Kijbunchoo, N.; Kim, W.; King,
   E. J.; King, P. J.; Kissel, J. S.; Korth, W. Z.; Kuehn, G.; Landry, M.;
   Lantz, B.; Laxen, M.; Liu, J.; Lockerbie, N. A.; Lormand, M.; MacInnis,
   M.; Macleod, D. M.; Márka, S.; Márka, Z.; Markosyan, A. S.; Maros,
   E.; Marsh, P.; Martin, I. W.; Martynov, D. V.; Mason, K.; Massinger,
   T. J.; Matichard, F.; Mavalvala, N.; McClelland, D. E.; McCormick,
   S.; McCuller, L.; McIntyre, G.; McRae, T.; Merilh, E. L.; Miller, J.;
   Mittleman, R.; Mo, G.; Mogushi, K.; Moraru, D.; Moreno, G.; Mueller,
   G.; Mukund, N.; Mullavey, A.; Munch, J.; Nelson, T. J. N.; Nguyen,
   P.; Nuttall, L. K.; Oberling, J.; Oktavia, O.; Oppermann, P.; Oram,
   Richard J.; O'Reilly, B.; Ottaway, D. J.; Overmier, H.; Palamos, J. R.;
   Parker, W.; Pele, A.; Penn, S.; Perez, C. J.; Phelps, M.; Pierro, V.;
   Pinto, I.; Principe, M.; Prokhorov, L. G.; Puncken, O.; Quetschke, V.;
   Quintero, E. A.; Radkins, H.; Raffai, P.; Ramirez, K. E.; Reid, S.;
   Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Romel, C. L.; Romie,
   J. H.; Ross, M. P.; Rowan, S.; Ryan, K.; Sadecki, T.; Sanchez, E. J.;
   Sanchez, L. E.; Sandberg, V.; Savage, R. L.; Sellers, D.; Shaddock,
   D. A.; Shaffer, T. J.; Shapiro, B.; Shoemaker, D. H.; Slagmolen,
   B. J. J.; Smith, B.; Smith, J. R.; Sorazu, B.; Spencer, A. P.; Staley,
   A.; Strain, K. A.; Sun, L.; Tanner, D. B.; Tasson, J. D.; Taylor,
   R.; Thomas, M.; Thomas, P.; Toland, K.; Torrie, C. I.; Traylor, G.;
   Tse, M.; Tuyenbayev, D.; Vajente, G.; Valdes, G.; van Veggel, A. A.;
   Vecchio, A.; Veitch, P. J.; Venkateswara, K.; Vo, T.; Vorvick, C.;
   Wade, M.; Walker, M.; Ward, R. L.; Warner, J.; Weaver, B.; Weiss,
   R.; Weßels, P.; Willke, B.; Wipf, C. C.; Wofford, J.; Worden, J.;
   Yamamoto, H.; Yancey, C. C.; Yu, Hang; Yu, Haocun; Zhang, L.; Zhu,
   S.; Zucker, M. E.; Zweizig, J.; LSC Instrument Authors
2018PhRvD..97h2002C    Altcode: 2018arXiv180107204C
  Searches are under way in Advanced LIGO and Virgo data for persistent
  gravitational waves from continuous sources, e.g. rapidly rotating
  galactic neutron stars, and stochastic sources, e.g. relic gravitational
  waves from the Big Bang or superposition of distant astrophysical
  events such as mergers of black holes or neutron stars. These searches
  can be degraded by the presence of narrow spectral artifacts (lines)
  due to instrumental or environmental disturbances. We describe a
  variety of methods used for finding, identifying and mitigating these
  artifacts, illustrated with particular examples. Results are provided
  in the form of lists of line artifacts that can safely be treated as
  non-astrophysical. Such lists are used to improve the efficiencies and
  sensitivities of continuous and stochastic gravitational wave searches
  by allowing vetoes of false outliers and permitting data cleaning.

---------------------------------------------------------
Title: XOSS Transient Discovery Report for 2018-03-09
Authors: Xu, J.; Zhang, M.; Zhang, X.; Zhao, J.; Liu, W.; Ruan, J.;
   Gao, X.
2018TNSTR.326....1X    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Ultraviolet Photooxidation of Fe2+ — Smectites and
    Implications for Mars
Authors: Rivera-Banuchi, V. B.; Liu, W.; Yee, N.; Glotch, T. D.;
   Legett, C.; Chemtob, S. M.
2018LPI....49.2550R    Altcode:
  Partial oxidation by UV radiation is shown for ferrous smectites,
  providing another alteration pathway for the production of ferric
  smectites on Mars.

---------------------------------------------------------
Title: Oxidation Pathways for Ferrous Iron Smectites on Mars and
    the Redox Evolution of Gale Crater
Authors: Chemtob, S. M.; Rivera-Banuchi, V. B.; Catalano, J. G.;
   Nickerson, R. D.; Morris, R. V.; Agresti, D. G.; Liu, W.; Yee, N.
2018LPI....49.2821C    Altcode:
  Oxidation of ferrous smectites produces nontronite and iron oxides. We
  discuss implications for the hematite-phyllosilicate facies of the
  Murray Formation.

---------------------------------------------------------
Title: Spatial Variation of Lunar Surface Hydration and the
Implications for Its Sources: Solar/Earth Winds or Others
Authors: Wang, H. Z.; Zhang, J.; Shi, Q. Q.; Khurana, K. K.; Rae,
   I. J.; Liu, J.; Guo, R. L.; Chen, J.; Tian, A. M.; Yao, S. T.; Bai,
   S. C.; Zhang, H.; Ling, Z. C.; Fu, X. H.; Wei, Y.; Liu, W. L.; Fu,
   S. Y.; Zong, Q. G.; Pu, Z. Y.
2018LPI....49.2066W    Altcode:
  We studied lunar surface hydration in the polar regions, and correlated
  its variations with incident ion flux when the Moon is inside/outside
  the magnetosphere.

---------------------------------------------------------
Title: High Resolution Digital Terrain Models of the Martian Surface:
    Compensation of the Atmosphere on CTX Imagery
Authors: Wohlfarth, K. S.; Liu, W. C.; Wu, B.; Grumpe, A.; Wöhler, C.
2018LPI....49.2498W    Altcode:
  We present a framework for the construction of high-resolution digital
  terrain models of the martian surface in the presence of strong
  atmospheric disturbances.

---------------------------------------------------------
Title: A challenge to identify an optical counterpart of the
    gravitational wave event GW151226 with Hyper Suprime-Cam
Authors: Utsumi, Yousuke; Tominaga, Nozomu; Tanaka, Masaomi; Morokuma,
   Tomoki; Yoshida, Michitoshi; Asakura, Yuichiro; Finet, François;
   Furusawa, Hisanori; Kawabata, Koji S.; Liu, Wei; Matsubayashi,
   Kazuya; Moritani, Yuki; Motohara, Kentaro; Nakata, Fumiaki; Ohta,
   Kouji; Terai, Tsuyoshi; Uemura, Makoto; Yasuda, Naoki
2018PASJ...70....1U    Altcode: 2017arXiv171000127U; 2017PASJ..tmp...21U
  We present the results of detailed analysis of an optical imaging
  survey conducted using the Subaru/Hyper Suprime-Cam (HSC) that aimed
  to identify an optical counterpart to the gravitational wave event
  GW151226. In half a night, the i- and z-band imaging survey by HSC
  covered 63.5 deg<SUP>2</SUP> of the error region, which contains
  about 7% of the LIGO localization probability, and the same field was
  observed in three different epochs. The detectable magnitude of the
  candidates in a differenced image is evaluated as i ∼ 23.2 mag for the
  requirement of at least two 5 σ detections, and 1744 candidates are
  discovered. Assuming a kilonova as an optical counterpart, we compare
  the optical properties of the candidates with model predictions. A red
  and rapidly declining light curve condition enables the discrimination
  of a kilonova from other transients, and a small number of candidates
  satisfy this condition. The presence of stellar-like counterparts in
  the reference frame suggests that the surviving candidates are likely
  to be flare stars. The fact that most of those candidates are in the
  galactic plane, |b| &lt; 5°, supports this interpretation. We also
  check whether the candidates are associated with the nearby GLADE
  galaxies, which reduces the number of contaminants even with a looser
  color cut. When a better probability map (with localization accuracy
  of ∼50 deg<SUP>2</SUP>) is available, kilonova searches of up to
  approximately 200 Mpc will become feasible by conducting immediate
  follow-up observations with an interval of 3-6 d.

---------------------------------------------------------
Title: Thermonuclear <SUP>19</SUP>F(p, {{\boldsymbol{\alpha
    }}}_{0})<SUP>16</SUP>O reaction rate
Authors: He, Jian-Jun; Lombardo, Ivano; Dell'Aquila, Daniele; Xu,
   Yi; Zhang, Li-Yong; Liu, Wei-Ping
2018ChPhC..42a5001H    Altcode: 2017arXiv170904170H
  The thermonuclear <SUP>19</SUP>F(p, {{{α }}}<SUB>0</SUB>)<SUP>16</SUP>O
  reaction rate in the temperature region 0.007-10 GK has been derived
  by re-evaluating the available experimental data, together with the
  low-energy theoretical R-matrix extrapolations. Our new rate deviates by
  up to about 30% compared to the previous results, although all rates are
  consistent within the uncertainties. At very low temperature (e.g. 0.01
  GK) our reaction rate is about 20% lower than the most recently
  published rate, because of a difference in the low energy extrapolated
  S-factor and a more accurate estimate of the reduced mass used in the
  calculation of the reaction rate. At temperatures above ∼1 GK, our
  rate is lower, for instance, by about 20% around 1.75 GK, because we
  have re-evaluated the previous data (Isoya et al., Nucl. Phys. 7, 116
  (1958)) in a meticulous way. The present interpretation is supported by
  the direct experimental data. The uncertainties of the present evaluated
  rate are estimated to be about 20% in the temperature region below
  0.2 GK, and are mainly caused by the lack of low-energy experimental
  data and the large uncertainties in the existing data. Asymptotic
  giant branch (AGB) stars evolve at temperatures below 0.2 GK, where
  the <SUP>19</SUP>F(p, {{α }})<SUP>16</SUP>O reaction may play a very
  important role. However, the current accuracy of the reaction rate
  is insufficient to help to describe, in a careful way, the fluorine
  over-abundances observed in AGB stars. Precise cross section (or
  S factor) data in the low energy region are therefore needed for
  astrophysical nucleosynthesis studies. <P />Supported by National
  Natural Science Foundation of China (11490562, 11490560, 11675229) and
  National Key Research and Development Program of China (2016YFA0400503)

---------------------------------------------------------
Title: The temporal evolution of explosive events and its implication
    on reconnection dynamics
Authors: Guo, L.; Liu, W.; De Pontieu, B.; Huang, Y. M.; Peter, H.;
   Bhattacharjee, A.
2017AGUFMSH43A2803G    Altcode:
  Transition-region explosive events and other bursts seen in extreme UV
  light are characterized by broad spectral line profiles, and the more
  violent ones show a strong enhancement of emission. They are thought
  to be driven by magnetic reconnection, because of their characteristic
  spectral profiles often indicating strong Alfvénic flows, and because
  of the fact that they typically occur where magnetic flux concentrations
  of opposite polarity intersect. In this presentation, we will focus
  on the temporal evolution of transition-region explosive events. In
  particular, we will investigate fast onsets of these events and the
  rapid oscillations of intensity during these event. The fast onset
  refers to the beginning of an explosive event, where the intensities
  and the widths of its line profiles increase dramatically (often within
  less than 10 seconds) and the rapid oscillations of intensity refer
  to blinks of emission that usually last less than 10 seconds during
  the event. In order to interpret and understand underlying mechanisms
  of these observations, we conduct numerical simulation of an explosive
  event and calculate its spectra. We observe a similar temporal evolution
  in the synthetic Si IV spectra when the explosive event is driven by
  time-dependent reconnection—plasmoid instability. The qualitative
  agreement between observations and simulations suggests that the
  temporal evolution of Si IV spectra of explosive events are closely
  related to reconnection dynamics.

---------------------------------------------------------
Title: Data-driven Simulations of Magnetic Connectivity in
    Behind-the-Limb Gamma-ray Flares and Associated Coronal Mass Ejections
Authors: Jin, M.; Petrosian, V.; Liu, W.; Nitta, N.; Omodei, N.;
   Rubio da Costa, F.; Effenberger, F.; Li, G.; Pesce-Rollins, M.
2017AGUFMSH44B..03J    Altcode:
  Recent Fermi detection of high-energy gamma-ray emission from the
  behind-the-limb (BTL) solar flares pose a puzzle on the particle
  acceleration and transport mechanisms in such events. Due to
  the large separation between the flare site and the location of
  gamma-ray emission, it is believed that the associated coronal
  mass ejections (CMEs) play an important role in accelerating and
  subsequently transporting particles back to the Sun to produce obseved
  gamma-rays. We explore this scenario by simulating the CME associated
  with a well-observed flare on 2014 September 1 about 40 degrees behind
  the east solar limb and by comparing the simulation and observational
  results. We utilize a data-driven global magnetohydrodynamics model
  (AWSoM: Alfven-wave Solar Model) to track the dynamical evolution
  of the global magnetic field during the event and investigate the
  magnetic connectivity between the CME/CME-driven shock and the Fermi
  emission region. Moreover, we derive the time-varying shock parameters
  (e.g., compression ratio, Alfven Mach number, and ThetaBN) over the
  area that is magnetically connected to the visible solar disk where
  Fermi gamma-ray emission originates. Our simulation shows that the
  visible solar disk develops connections both to the flare site and to
  the CME-driven shock during the eruption, which indicate that the CME's
  interaction with the global solar corona is critical for understanding
  such Fermi BTL events and gamma-ray flares in general. We discuss
  the causes and implications of Fermi BTL events, in the framework
  of a potential shift of paradigm on particle acceleration in solar
  flares/CMEs.

---------------------------------------------------------
Title: Magnetic Topology of a Long-Lived Coronal Condensation Site
    Lasting Eight Months
Authors: Sun, X.; Yu, S.; Liu, W.
2017AGUFMSH13A2457S    Altcode:
  It is well known that cool material, such as prominences or
  coronal rain, can form in-situ by condensation of hot coronal
  plasma due to a runaway radiative cooling instability (a.k.a. thermal
  non-equilibrium). Recent observations and numerical simulations suggest
  that such condensations are quite common, but in quiet-Sun regions,
  they occur preferentially in locations where magnetic field is weak
  (e.g., null points) or discontinuous (e.g., current sheets). Such
  events usually have short lifetimes of hours to days. Surprisingly,
  we observed a high-latitude condensation site lasting over eight
  months in 2014 with recurrent and episodic condensations fueling a
  funnel-shaped prominence. We analyze the coronal magnetic topology to
  investigate the necessary condition of such a long-lived condensation
  site. We find that the site was directly above a poleward photospheric
  flux surge when the polar field polarity was close to its solar cycle
  reversal. The large-scale magnetic cancellation front may have sustained
  interchange reconnection at this location, creating suitable conditions
  for coronal plasma condensation.

---------------------------------------------------------
Title: J-GEM observations of an electromagnetic counterpart to the
    neutron star merger GW170817
Authors: Utsumi, Yousuke; Tanaka, Masaomi; Tominaga, Nozomu; Yoshida,
   Michitoshi; Barway, Sudhanshu; Nagayama, Takahiro; Zenko, Tetsuya;
   Aoki, Kentaro; Fujiyoshi, Takuya; Furusawa, Hisanori; Kawabata, Koji
   S.; Koshida, Shintaro; Lee, Chien-Hsiu; Morokuma, Tomoki; Motohara,
   Kentaro; Nakata, Fumiaki; Ohsawa, Ryou; Ohta, Kouji; Okita, Hirofumi;
   Tajitsu, Akito; Tanaka, Ichi; Terai, Tsuyoshi; Yasuda, Naoki; Abe,
   Fumio; Asakura, Yuichiro; Bond, Ian A.; Miyazaki, Shota; Sumi,
   Takahiro; Tristram, Paul J.; Honda, Satoshi; Itoh, Ryosuke; Itoh,
   Yoichi; Kawabata, Miho; Morihana, Kumiko; Nagashima, Hiroki; Nakaoka,
   Tatsuya; Ohshima, Tomohito; Takahashi, Jun; Takayama, Masaki; Aoki,
   Wako; Baar, Stefan; Doi, Mamoru; Finet, Francois; Kanda, Nobuyuki;
   Kawai, Nobuyuki; Kim, Ji Hoon; Kuroda, Daisuke; Liu, Wei; Matsubayashi,
   Kazuya; Murata, Katsuhiro L.; Nagai, Hiroshi; Saito, Tomoki; Saito,
   Yoshihiko; Sako, Shigeyuki; Sekiguchi, Yuichiro; Tamura, Yoichi;
   Tanaka, Masayuki; Uemura, Makoto; Yamaguchi, Masaki S.
2017PASJ...69..101U    Altcode: 2017arXiv171005848U
  GW170817 is the first detected gravitational wave source from a
  neutron star merger. We present the Japanese collaboration for
  gravitational-wave electro-magnetic (J-GEM) follow-up observations
  of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows
  a 2.5 mag decline in the z band during the period between 1.7 and
  7.7 d after the merger. Such a rapid decline is not comparable with
  supernovae light curves at any epoch. The color of SSS17a also evolves
  rapidly and becomes redder during later epochs: the z - H color has
  changed by approximately 2.5 mag during the period between 0.7 and 7.7
  d. The rapid evolutions of both the color and the optical brightness are
  consistent with the expected properties of a kilonova that is powered by
  the radioactive decay of newly synthesized r-process nuclei. Kilonova
  models with Lanthanide elements can reproduce the aforementioned
  observed properties well, which suggests that r-process nucleosynthesis
  beyond the second peak takes place in SSS17a. However, the absolute
  magnitude of SSS17a is brighter than the expected brightness of the
  kilonova models with an ejecta mass of 0.01 M<SUB>⊙</SUB>, which
  suggests a more intense mass ejection (∼0.03 M<SUB>⊙</SUB>) or
  possibly an additional energy source.

---------------------------------------------------------
Title: Evolution of Post-accretion-induced Collapse Binaries: The
    Effect of Evaporation
Authors: Liu, Wei-Min; Li, Xiang-Dong
2017ApJ...851...58L    Altcode: 2017arXiv171102011L
  Accretion-induced collapse (AIC) is widely accepted to be one of
  the formation channels for millisecond pulsars (MSPs). Since the
  MSPs have high spin-down luminosities, they can immediately start to
  evaporate their companion stars after birth. In this paper, we present
  a detailed investigation on the evolution of the post-AIC binaries,
  taking into account the effect of evaporation both before and during
  the Roche-lobe overflow process. We discuss the possible influence
  of the input parameters including the evaporation efficiency, the
  initial spin period, and the initial surface magnetic field of the
  newborn neutron star. We compare the calculated results with the
  traditional low-mass X-ray binary evolution and suggest that they may
  reproduce at least part of the observed redbacks and black widows in
  the companion mass-orbital period plane depending on the mechanisms
  of angular momentum loss associated with evaporation.

---------------------------------------------------------
Title: Comparison of rotational temperature derived from ground-based
    OH airglow observations with TIMED/SABER to evaluate the Einstein
    Coefficients
Authors: Liu, W.; Xu, J.; Smith, A. K.; Yuan, W.
2017AGUFMSA13B..09L    Altcode:
  Ground-based observations of the OH(9-4, 8-3, 6-2, 5-1, 3-0) band
  airglows over Xinglong, China (40°24'N, 117°35'E) from December 2011
  to 2014 are used to calculate rotational temperatures. The temperatures
  are calculated using five commonly used Einstein coefficient
  datasets. The kinetic temperature from TIMED/SABER is completely
  independent of the OH rotational temperature. SABER temperatures are
  weighted vertically by weighting functions calculated for each emitting
  vibrational state from two SABER OH volume emission rate profiles. By
  comparing the ground-based OH rotational temperature with SABER's,
  five Einstein coefficient datasets are evaluated. The results show that
  temporal variations of the rotational temperatures are well correlated
  with SABER's; the linear correlation coefficients are higher than 0.72,
  but the slopes of the fit between the SABER and rotational temperatures
  are not equal to 1. The rotational temperatures calculated using each
  set of Einstein coefficients produce a different bias with respect
  to SABER; these are evaluated over each of vibrational levels to
  assess the best match. It is concluded that rotational temperatures
  determined using any of the available Einstein coefficient datasets
  have systematic errors. However, of the five sets of coefficients,
  the rotational temperature derived with the Langhoff et al.'s (1986)
  set is most consistent with SABER. In order to get a set of optimal
  Einstein coefficients for rotational temperature derivation, we derive
  the relative values from ground-based OH spectra and SABER temperatures
  statistically using three year data. The use of a standard set of
  Einstein coefficients will be beneficial for comparing rotational
  temperatures observed at different sites.

---------------------------------------------------------
Title: Digging into the corona: A modeling framework trained with
    Sun-grazing comet observations
Authors: Jia, Y. D.; Pesnell, W. D.; Bryans, P.; Downs, C.; Liu, W.;
   Schwartz, S. J.
2017AGUFMSH11B2437J    Altcode:
  Images of comets diving into the low corona have been captured a few
  times in the past decade. Structures visible at various wavelengths
  during these encounters indicate a strong variation of the ambient
  conditions of the corona. We combine three numerical models: a global
  coronal model, a particle transportation model, and a cometary plasma
  interaction model into one framework to model the interaction of such
  Sun-grazing comets with plasma in the low corona. In our framework,
  cometary vapors are ionized via multiple channels and then captured
  by the coronal magnetic field. In seconds, these ions are further
  ionized into their highest charge state, which is revealed by certain
  coronal emission lines. Constrained by observations, we apply our
  framework to trace back to the local conditions of the ambient corona,
  and their spatial/time variation over a broad range of scales. Once
  trained by multiple stages of the comet's journey in the low corona,
  we illustrate how this framework can leverage these unique observations
  to probe the structure of the solar corona and solar wind.

---------------------------------------------------------
Title: Broadband high-frequency waves and intermittent energy
    conversion at dipolarization fronts
Authors: Yang, J.; Cao, J.; Fu, H.; Wang, T.; Liu, W.; Yao, Z., Sr.
2017AGUFMSM13B2374Y    Altcode:
  Dipolarization front (DF) is a sharp boundary most probably separating
  the reconnection jet from the background plasma sheet. So far at this
  boundary, the observed waves are mainly in low-frequency range (e.g.,
  magnetosonic waves and lower hybrid waves). Few high-frequency waves
  are observed in this region. In this paper, we report the broadband
  high-frequency wave emissions at the DF. These waves, having frequencies
  extending from the electron cyclotron frequency fce, up to the electron
  plasma frequency fpe, could contribute 10% to the in situ measurement
  of intermittent energy conversion at the DF layer. Their generation may
  be attributed to electron beams, which are simultaneously observed at
  the DF as well. Furthermore, we find intermittent energy conversion is
  primarily to the broadband fluctuations in the lower hybrid frequency
  range although the net energy conversion is small.

---------------------------------------------------------
Title: A comparison of quiet time thermospheric winds between FPIs
    and models
Authors: Jiang, G.; Xu, J.; Wang, W.; Yuan, W.; Zhang, S.; Yu, T.;
   Zhang, X.; Huang, C.; Liu, W.; Li, Q.
2017AGUFMSA41A2612J    Altcode:
  Abstract:The Fabry-Perot Interferometer (FPI) instruments installed
  at Xinglong, (geog.: 40.2oN, 117.4oE; geom.: 35oN), Kelan (geog.:
  38.7oN, 111.6oE; geom.: 34oN) and Millstone Hill (geog.: 42.6oN,
  71.5oW; geom.: 52oN) started to measure the thermosphere neutral
  winds near 250 km since April 2010, March 2010 and November 2011,
  respectively. In this work, the joined comparison of FPI observed
  winds and two models during geomagnetic quiet time are processed for
  the study of mid-latitudinal thermosphere. The years of FPI wind data
  we use are from 2010 to 2014. The two models we use are NCAR TIE-GCM
  (Thermosphere-Ionosphere-Electrodynamics General Circulation Model of
  National Center for Atmospheric Research) and HWM07 (Horizontal Wind
  Model, version 2007). The real solar and geomagnetic conditions were
  applied to the models.

---------------------------------------------------------
Title: Variation of plasmapause location during magnetic storms:
    observations and modeling
Authors: Liu, W.
2017AGUFMSM43C2731L    Altcode:
  This paper investigates the dynamic evolutions of the plasmapause during
  magnetic storms based on in situ observations and empirical modeling
  results. Superposed epoch analysis is performed on the plasmapause
  location identified from THEMIS in situ measurements during the 61
  magnetic storms from 2009 to 2013. The evolution of the plasmapause
  is generally consistent with the theory of erosion/refilling of the
  plasmapause. From multi-spacecraft in situ measurements, we are able
  to directly calculate the plasmapause radial velocity, Vpp. It is found
  that the radial velocity is on average earthward during main phase and
  turns outward during recovery phase. The empirical plasmapause model
  by Liu et al. [2015] is further utilized to reproduce the plasmapause
  location during these 61 storms to reveal the details of the evolution,
  such as the local time dependence. It is shown that the expansion of
  the plasmapause starts firstly on the midnight sector at t0+1hr, and
  subsequently on the dawnside at t0+4hr, dayside at t0+8hr and duskside
  at t0+11hr, where t0 corresponds to the time of Dst minimum. The
  averaged Vpp is quantified based on modeling results as up to 0.17
  RE/hr earthward in the main phase and 0.08 RE/hr outward in the recovery
  phase. The knowledge of the dynamic evolution of plasmapause provided
  in this paper is valuable to understand the dynamics of the inner
  magnetosphere during magnetic storms.

---------------------------------------------------------
Title: Multiple pathways in pressure-induced phase transition
    of coesite
Authors: Liu, Wei; Wu, Xuebang; Liang, Yunfeng; Liu, Changsong;
   Miranda, Caetano R.; Scandolo, Sandro
2017PNAS..11412894L    Altcode:
  High-pressure single-crystal X-ray diffraction method with precise
  control of hydrostatic conditions, typically with helium or neon as
  the pressure-transmitting medium, has significantly changed our view
  on what happens with low-density silica phases under pressure. Coesite
  is a prototype material for pressure-induced amorphization. However,
  it was found to transform into a high-pressure octahedral (HPO) phase,
  or coesite-II and coesite-III. Given that the pressure is believed to
  be hydrostatic in two recent experiments, the different transformation
  pathways are striking. Based on molecular dynamic simulations with
  an ab initio parameterized potential, we reproduced all of the above
  experiments in three transformation pathways, including the one leading
  to an HPO phase. This octahedral phase has an oxygen hcp sublattice
  featuring 2 × 2 zigzag octahedral edge-sharing chains, however with
  some broken points (i.e., point defects). It transforms into α-PbO2
  phase when it is relaxed under further compression. We show that
  the HPO phase forms through a continuous rearrangement of the oxygen
  sublattice toward hcp arrangement. The high-pressure amorphous phases
  can be described by an fcc and hcp sublattice mixture.

---------------------------------------------------------
Title: Direct detection of a break in the teraelectronvolt cosmic-ray
    spectrum of electrons and positrons
Authors: DAMPE Collaboration; Ambrosi, G.; An, Q.; Asfandiyarov, R.;
   Azzarello, P.; Bernardini, P.; Bertucci, B.; Cai, M. S.; Chang, J.;
   Chen, D. Y.; Chen, H. F.; Chen, J. L.; Chen, W.; Cui, M. Y.; Cui,
   T. S.; D'Amone, A.; de Benedittis, A.; De Mitri, I.; di Santo, M.;
   Dong, J. N.; Dong, T. K.; Dong, Y. F.; Dong, Z. X.; Donvito, G.; Droz,
   D.; Duan, K. K.; Duan, J. L.; Duranti, M.; D'Urso, D.; Fan, R. R.;
   Fan, Y. Z.; Fang, F.; Feng, C. Q.; Feng, L.; Fusco, P.; Gallo, V.;
   Gan, F. J.; Gao, M.; Gao, S. S.; Gargano, F.; Garrappa, S.; Gong, K.;
   Gong, Y. Z.; Guo, D. Y.; Guo, J. H.; Hu, Y. M.; Huang, G. S.; Huang,
   Y. Y.; Ionica, M.; Jiang, D.; Jiang, W.; Jin, X.; Kong, J.; Lei, S. J.;
   Li, S.; Li, X.; Li, W. L.; Li, Y.; Liang, Y. F.; Liang, Y. M.; Liao,
   N. H.; Liu, H.; Liu, J.; Liu, S. B.; Liu, W. Q.; Liu, Y.; Loparco, F.;
   Ma, M.; Ma, P. X.; Ma, S. Y.; Ma, T.; Ma, X. Q.; Ma, X. Y.; Marsella,
   G.; Mazziotta, M. N.; Mo, D.; Niu, X. Y.; Peng, X. Y.; Peng, W. X.;
   Qiao, R.; Rao, J. N.; Salinas, M. M.; Shang, G. Z.; H. Shen, W.; Shen,
   Z. Q.; Shen, Z. T.; Song, J. X.; Su, H.; Su, M.; Sun, Z. Y.; Surdo,
   A.; Teng, X. J.; Tian, X. B.; Tykhonov, A.; Vagelli, V.; Vitillo, S.;
   Wang, C.; Wang, H.; Wang, H. Y.; Wang, J. Z.; Wang, L. G.; Wang, Q.;
   Wang, S.; Wang, X. H.; Wang, X. L.; Wang, Y. F.; Wang, Y. P.; Wang,
   Y. Z.; Wen, S. C.; Wang, Z. M.; Wei, D. M.; Wei, J. J.; Wei, Y. F.;
   Wu, D.; Wu, J.; Wu, L. B.; Wu, S. S.; Wu, X.; Xi, K.; Xia, Z. Q.; Xin,
   Y. L.; Xu, H. T.; Xu, Z. L.; Xu, Z. Z.; Xue, G. F.; Yang, H. B.; Yang,
   P.; Yang, Y. Q.; Yang, Z. L.; Yao, H. J.; Yu, Y. H.; Yuan, Q.; Yue,
   C.; Zang, J. J.; Zhang, C.; Zhang, D. L.; Zhang, F.; Zhang, J. B.;
   Zhang, J. Y.; Zhang, J. Z.; Zhang, L.; Zhang, P. F.; Zhang, S. X.;
   Zhang, W. Z.; Zhang, Y.; Zhang, Y. J.; Zhang, Y. Q.; Zhang, Y. L.;
   Zhang, Y. P.; Zhang, Z.; Zhang, Z. Y.; Zhao, H.; Zhao, H. Y.; Zhao,
   X. F.; Zhou, C. Y.; Zhou, Y.; Zhu, X.; Zhu, Y.; Zimmer, S.
2017Natur.552...63D    Altcode: 2017arXiv171110981A
  High-energy cosmic-ray electrons and positrons (CREs), which lose
  energy quickly during their propagation, provide a probe of Galactic
  high-energy processes and may enable the observation of phenomena such
  as dark-matter particle annihilation or decay. The CRE spectrum has been
  measured directly up to approximately 2 teraelectronvolts in previous
  balloon- or space-borne experiments, and indirectly up to approximately
  5 teraelectronvolts using ground-based Cherenkov γ-ray telescope
  arrays. Evidence for a spectral break in the teraelectronvolt energy
  range has been provided by indirect measurements, although the results
  were qualified by sizeable systematic uncertainties. Here we report
  a direct measurement of CREs in the energy range 25 gigaelectronvolts
  to 4.6 teraelectronvolts by the Dark Matter Particle Explorer (DAMPE)
  with unprecedentedly high energy resolution and low background. The
  largest part of the spectrum can be well fitted by a ‘smoothly broken
  power-law’ model rather than a single power-law model. The direct
  detection of a spectral break at about 0.9 teraelectronvolts confirms
  the evidence found by previous indirect measurements, clarifies the
  behaviour of the CRE spectrum at energies above 1 teraelectronvolt
  and sheds light on the physical origin of the sub-teraelectronvolt CREs.

---------------------------------------------------------
Title: Quiescent Prominence Dynamics Observed with the Hinode
    Solar Optical Telescope. II. Prominence Bubble Boundary Layer
    Characteristics and the Onset of a Coupled Kelvin-Helmholtz
    Rayleigh-Taylor Instability
Authors: Berger, Thomas; Hillier, Andrew; Liu, Wei
2017ApJ...850...60B    Altcode: 2017arXiv170705265B
  We analyze solar quiescent prominence bubble characteristics and
  instability dynamics using Hinode/Solar Optical Telescope data. We
  measure the bubble expansion rate, prominence downflows, and the
  profile of the boundary layer brightness and thickness as a function
  of time. The largest bubble analyzed rises into the prominence with a
  speed of about 1.3 {km} {{{s}}}<SUP>-1</SUP> until it is destabilized by
  a localized shear flow on the boundary. Boundary layer thickness grows
  gradually as prominence downflows deposit plasma onto the bubble with
  characteristic speeds of 20{--}35 {km} {{{s}}}<SUP>-1</SUP>. Lateral
  downflows initiate from the thickened boundary layer with characteristic
  speeds of 25{--}50 {km} {{{s}}}<SUP>-1</SUP>, “draining” the
  layer of plasma. Strong shear flow across one bubble boundary leads
  to an apparent coupled Kelvin-Helmholtz Rayleigh-Taylor (KH-RT)
  instability. We measure shear flow speeds above the bubble of 10 {km}
  {{{s}}}<SUP>-1</SUP> and infer interior bubble flow speeds on the order
  of 100 {km} {{{s}}}<SUP>-1</SUP>. Comparing the measured growth rate
  of the instability to analytic expressions, we infer a magnetic flux
  density across the bubble boundary of ∼10<SUP>-3</SUP> T (10 Gauss)
  at an angle of ∼ 70^\circ to the prominence plane. The results are
  consistent with the hypothesis that prominence bubbles are caused by
  magnetic flux that emerges below a prominence, setting up the conditions
  for RT, or combined KH-RT, instability flows that transport flux,
  helicity, and hot plasma upward into the overlying coronal magnetic
  flux rope.

---------------------------------------------------------
Title: The <SUP>95</SUP>Zr(n, γ)<SUP>96</SUP>Zr Cross Section from
    the Surrogate Ratio Method and Its Effect on s-process Nucleosynthesis
Authors: Yan, S. Q.; Li, Z. H.; Wang, Y. B.; Nishio, K.; Lugaro, M.;
   Karakas, A. I.; Makii, H.; Mohr, P.; Su, J.; Li, Y. J.; Nishinaka,
   I.; Hirose, K.; Han, Y. L.; Orlandi, R.; Shen, Y. P.; Guo, B.; Zeng,
   S.; Lian, G.; Chen, Y. S.; Liu, W. P.
2017ApJ...848...98Y    Altcode: 2017arXiv170904635Y
  The <SUP>95</SUP>Zr(n, γ)<SUP>96</SUP>Zr reaction cross section
  is crucial in the modeling of s-process nucleosynthesis in
  asymptotic giant branch stars because it controls the operation
  of the branching point at the unstable <SUP>95</SUP>Zr and the
  subsequent production of <SUP>96</SUP>Zr. We have carried out the
  measurement of the <SUP>94</SUP>Zr(<SUP>18</SUP>O, <SUP>16</SUP>O)
  and <SUP>90</SUP>Zr(<SUP>18</SUP>O, <SUP>16</SUP>O) reactions and
  obtained the γ-decay probability ratio of <SUP>96</SUP>Zr* and
  <SUP>92</SUP>Zr* to determine the <SUP>95</SUP>Zr(n, γ)<SUP>96</SUP>Zr
  reaction cross sections with the surrogate ratio method. Our deduced
  Maxwellian-averaged cross section of 66 ± 16 mb at 30 keV is close to
  the value recommended by Bao et al., but 30% and more than a factor
  of two larger than the values proposed by Toukan &amp; Käppeler and
  Lugaro et al., respectively, and routinely used in s-process models. We
  tested the new rate in stellar models with masses between 2 and 6
  M <SUB>⊙</SUB> and metallicities of 0.014 and 0.03. The largest
  changes—up to 80% variations in <SUP>96</SUP>Zr—are seen in models
  of mass 3-4 M <SUB>⊙</SUB>, where the <SUP>22</SUP>Ne neutron source
  is mildly activated. The new rate can still provide a match to data
  from meteoritic stardust silicon carbide grains, provided that the
  maximum mass of the parent stars is below 4 M <SUB>⊙</SUB>, for a
  metallicity of 0.03.

---------------------------------------------------------
Title: The DArk Matter Particle Explorer mission
Authors: Chang, J.; Ambrosi, G.; An, Q.; Asfandiyarov, R.; Azzarello,
   P.; Bernardini, P.; Bertucci, B.; Cai, M. S.; Caragiulo, M.; Chen,
   D. Y.; Chen, H. F.; Chen, J. L.; Chen, W.; Cui, M. Y.; Cui, T. S.;
   D'Amone, A.; De Benedittis, A.; De Mitri, I.; Di Santo, M.; Dong,
   J. N.; Dong, T. K.; Dong, Y. F.; Dong, Z. X.; Donvito, G.; Droz, D.;
   Duan, K. K.; Duan, J. L.; Duranti, M.; D'Urso, D.; Fan, R. R.; Fan,
   Y. Z.; Fang, F.; Feng, C. Q.; Feng, L.; Fusco, P.; Gallo, V.; Gan,
   F. J.; Gan, W. Q.; Gao, M.; Gao, S. S.; Gargano, F.; Gong, K.; Gong,
   Y. Z.; Guo, J. H.; Hu, Y. M.; Huang, G. S.; Huang, Y. Y.; Ionica,
   M.; Jiang, D.; Jiang, W.; Jin, X.; Kong, J.; Lei, S. J.; Li, S.; Li,
   X.; Li, W. L.; Li, Y.; Liang, Y. F.; Liang, Y. M.; Liao, N. H.; Liu,
   Q. Z.; Liu, H.; Liu, J.; Liu, S. B.; Liu, Q. Z.; Liu, W. Q.; Liu,
   Y.; Loparco, F.; Lü, J.; Ma, M.; Ma, P. X.; Ma, S. Y.; Ma, T.; Ma,
   X. Q.; Ma, X. Y.; Marsella, G.; Mazziotta, M. N.; Mo, D.; Miao, T. T.;
   Niu, X. Y.; Pohl, M.; Peng, X. Y.; Peng, W. X.; Qiao, R.; Rao, J. N.;
   Salinas, M. M.; Shang, G. Z.; Shen, W. H.; Shen, Z. Q.; Shen, Z. T.;
   Song, J. X.; Su, H.; Su, M.; Sun, Z. Y.; Surdo, A.; Teng, X. J.; Tian,
   X. B.; Tykhonov, A.; Vagelli, V.; Vitillo, S.; Wang, C.; Wang, Chi;
   Wang, H.; Wang, H. Y.; Wang, J. Z.; Wang, L. G.; Wang, Q.; Wang, S.;
   Wang, X. H.; Wang, X. L.; Wang, Y. F.; Wang, Y. P.; Wang, Y. Z.; Wen,
   S. C.; Wang, Z. M.; Wei, D. M.; Wei, J. J.; Wei, Y. F.; Wu, D.; Wu,
   J.; Wu, S. S.; Wu, X.; Xi, K.; Xia, Z. Q.; Xin, Y. L.; Xu, H. T.;
   Xu, Z. L.; Xu, Z. Z.; Xue, G. F.; Yang, H. B.; Yang, J.; Yang, P.;
   Yang, Y. Q.; Yang, Z. L.; Yao, H. J.; Yu, Y. H.; Yuan, Q.; Yue, C.;
   Zang, J. J.; Zhang, C.; Zhang, D. L.; Zhang, F.; Zhang, J. B.; Zhang,
   J. Y.; Zhang, J. Z.; Zhang, L.; Zhang, P. F.; Zhang, S. X.; Zhang,
   W. Z.; Zhang, Y.; Zhang, Y. J.; Zhang, Y. Q.; Zhang, Y. L.; Zhang,
   Y. P.; Zhang, Z.; Zhang, Z. Y.; Zhao, H.; Zhao, H. Y.; Zhao, X. F.;
   Zhou, C. Y.; Zhou, Y.; Zhu, X.; Zhu, Y.; Zimmer, S.
2017APh....95....6C    Altcode: 2017arXiv170608453T; 2017arXiv170608453C
  The DArk Matter Particle Explorer (DAMPE), one of the four scientific
  space science missions within the framework of the Strategic Pioneer
  Program on Space Science of the Chinese Academy of Sciences, is
  a general purpose high energy cosmic-ray and gamma-ray observatory,
  which was successfully launched on December 17th, 2015 from the Jiuquan
  Satellite Launch Center. The DAMPE scientific objectives include
  the study of galactic cosmic rays up to ∼ 10 TeV and hundreds of
  TeV for electrons/gammas and nuclei respectively, and the search for
  dark matter signatures in their spectra. In this paper we illustrate
  the layout of the DAMPE instrument, and discuss the results of beam
  tests and calibrations performed on ground. Finally we present the
  expected performance in space and give an overview of the mission key
  scientific goals.

---------------------------------------------------------
Title: Fermi Large Area Telescope observations of the Sun: The first
    ten years
Authors: Pesce-Rollins, M.; Omodei, N.; Allafort, A.; Petrosian, V.;
   Raino, S.; Liu, W.
2017ifs..confE.173P    Altcode: 2017PoS...312E.173P
  No abstract at ADS

---------------------------------------------------------
Title: Multi-messenger Observations of a Binary Neutron Star Merger
Authors: Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.;
   Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya,
   V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.; Agatsuma,
   K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.;
   Allen, B.; Allen, G.; Allocca, A.; Altin, P. A.; Amato, A.; Ananyeva,
   A.; Anderson, S. B.; Anderson, W. G.; Angelova, S. V.; Antier, S.;
   Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arnaud, N.; Arun,
   K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.;
   Atallah, D. V.; Aufmuth, P.; Aulbert, C.; AultONeal, K.; Austin,
   C.; Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.; Bae,
   S.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.;
   Banagiri, S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker,
   D.; Barkett, K.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia,
   M.; Barta, D.; Barthelmy, S. D.; Bartlett, J.; Bartos, I.; Bassiri,
   R.; Basti, A.; Batch, J. C.; Bawaj, M.; Bayley, J. C.; Bazzan, M.;
   Bécsy, B.; Beer, C.; Bejger, M.; Belahcene, I.; Bell, A. S.; Berger,
   B. K.; Bergmann, G.; Bero, J. J.; Berry, C. P. L.; Bersanetti, D.;
   Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko,
   I. A.; Billingsley, G.; Billman, C. R.; Birch, J.; Birney, R.;
   Birnholtz, O.; Biscans, S.; Biscoveanu, S.; Bisht, A.; Bitossi, M.;
   Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blackman, J.; Blair,
   C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bode, N.;
   Boer, M.; Bogaert, G.; Bohe, A.; Bondu, F.; Bonilla, E.; Bonnand, R.;
   Boom, B. A.; Bork, R.; Boschi, V.; Bose, S.; Bossie, K.; Bouffanais,
   Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Branchesi, M.; Brau,
   J. E.; Briant, T.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill,
   P.; Broida, J. E.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brunett,
   S.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno,
   A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cabero, M.; Cadonati, L.;
   Cagnoli, G.; Cahillane, C.; Calderón Bustillo, J.; Callister, T. A.;
   Calloni, E.; Camp, J. B.; Canepa, M.; Canizares, P.; Cannon, K. C.;
   Cao, H.; Cao, J.; Capano, C. D.; Capocasa, E.; Carbognani, F.; Caride,
   S.; Carney, M. F.; Casanueva Diaz, J.; Casentini, C.; Caudill, S.;
   Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C. B.;
   Cerdá-Durán, P.; Cerretani, G.; Cesarini, E.; Chamberlin, S. J.;
   Chan, M.; Chao, S.; Charlton, P.; Chase, E.; Chassande-Mottin, E.;
   Chatterjee, D.; Chatziioannou, K.; Cheeseboro, B. D.; Chen, H. Y.;
   Chen, X.; Chen, Y.; Cheng, H. -P.; Chia, H.; Chincarini, A.; Chiummo,
   A.; Chmiel, T.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.;
   Chu, Q.; Chua, A. J. K.; Chua, S.; Chung, A. K. W.; Chung, S.; Ciani,
   G.; Ciolfi, R.; Cirelli, C. E.; Cirone, A.; Clara, F.; Clark, J. A.;
   Clearwater, P.; Cleva, F.; Cocchieri, C.; Coccia, E.; Cohadon,
   P. -F.; Cohen, D.; Colla, A.; Collette, C. G.; Cominsky, L. R.;
   Constancio, M., Jr.; Conti, L.; Cooper, S. J.; Corban, P.; Corbitt,
   T. R.; Cordero-Carrión, I.; Corley, K. R.; Cornish, N.; Corsi, A.;
   Cortese, S.; Costa, C. A.; Coughlin, M. W.; Coughlin, S. B.; Coulon,
   J. -P.; Countryman, S. T.; Couvares, P.; Covas, P. B.; Cowan, E. E.;
   Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Coyne, R.; Creighton,
   J. D. E.; Creighton, T. D.; Cripe, J.; Crowder, S. G.; Cullen, T. J.;
   Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Dálya,
   G.; Danilishin, S. L.; D'Antonio, S.; Danzmann, K.; Dasgupta, A.;
   Da Silva Costa, C. F.; Dattilo, V.; Dave, I.; Davier, M.; Davis, D.;
   Daw, E. J.; Day, B.; De, S.; DeBra, D.; Degallaix, J.; De Laurentis,
   M.; Deléglise, S.; Del Pozzo, W.; Demos, N.; Denker, T.; Dent, T.;
   De Pietri, R.; Dergachev, V.; De Rosa, R.; DeRosa, R. T.; De Rossi,
   C.; DeSalvo, R.; de Varona, O.; Devenson, J.; Dhurandhar, S.; Díaz,
   M. C.; Di Fiore, L.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.;
   Di Pace, S.; Di Palma, I.; Di Renzo, F.; Doctor, Z.; Dolique, V.;
   Donovan, F.; Dooley, K. L.; Doravari, S.; Dorrington, I.; Douglas,
   R.; Dovale Álvarez, M.; Downes, T. P.; Drago, M.; Dreissigacker,
   C.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dupej, P.; Dwyer, S. E.;
   Edo, T. B.; Edwards, M. C.; Effler, A.; Ehrens, P.; Eichholz, J.;
   Eikenberry, S. S.; Eisenstein, R. A.; Essick, R. C.; Estevez, D.;
   Etienne, Z. B.; Etzel, T.; Evans, M.; Evans, T. M.; Factourovich,
   M.; Fafone, V.; Fair, H.; Fairhurst, S.; Fan, X.; Farinon, S.; Farr,
   B.; Farr, W. M.; Fauchon-Jones, E. J.; Favata, M.; Fays, M.; Fee,
   C.; Fehrmann, H.; Feicht, J.; Fejer, M. M.; Fernandez-Galiana, A.;
   Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Finstad, D.;
   Fiori, I.; Fiorucci, D.; Fishbach, M.; Fisher, R. P.; Fitz-Axen, M.;
   Flaminio, R.; Fletcher, M.; Fong, H.; Font, J. A.; Forsyth, P. W. F.;
   Forsyth, S. S.; Fournier, J. -D.; Frasca, S.; Frasconi, F.; Frei, Z.;
   Freise, A.; Frey, R.; Frey, V.; Fries, E. M.; Fritschel, P.; Frolov,
   V. V.; Fulda, P.; Fyffe, M.; Gabbard, H.; Gadre, B. U.; Gaebel,
   S. M.; Gair, J. R.; Gammaitoni, L.; Ganija, M. R.; Gaonkar, S. G.;
   Garcia-Quiros, C.; Garufi, F.; Gateley, B.; Gaudio, S.; Gaur, G.;
   Gayathri, V.; Gehrels, N.; Gemme, G.; Genin, E.; Gennai, A.; George,
   D.; George, J.; Gergely, L.; Germain, V.; Ghonge, S.; Ghosh, Abhirup;
   Ghosh, Archisman; Ghosh, S.; Giaime, J. A.; Giardina, K. D.; Giazotto,
   A.; Gill, K.; Glover, L.; Goetz, E.; Goetz, R.; Gomes, S.; Goncharov,
   B.; González, G.; Gonzalez Castro, J. M.; Gopakumar, A.; Gorodetsky,
   M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Grado, A.; Graef, C.;
   Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco, G.; Green, A. C.;
   Gretarsson, E. M.; Griswold, B.; Groot, P.; Grote, H.; Grunewald, S.;
   Gruning, P.; Guidi, G. M.; Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa,
   K. E.; Gustafson, E. K.; Gustafson, R.; Halim, O.; Hall, B. R.; Hall,
   E. D.; Hamilton, E. Z.; Hammond, G.; Haney, M.; Hanke, M. M.; Hanks,
   J.; Hanna, C.; Hannam, M. D.; Hannuksela, O. A.; Hanson, J.; Hardwick,
   T.; Harms, J.; Harry, G. M.; Harry, I. W.; Hart, M. J.; Haster, C. -J.;
   Haughian, K.; Healy, J.; Heidmann, A.; Heintze, M. C.; Heitmann,
   H.; Hello, P.; Hemming, G.; Hendry, M.; Heng, I. S.; Hennig, J.;
   Heptonstall, A. W.; Heurs, M.; Hild, S.; Hinderer, T.; Hoak, D.;
   Hofman, D.; Holt, K.; Holz, D. E.; Hopkins, P.; Horst, C.; Hough,
   J.; Houston, E. A.; Howell, E. J.; Hreibi, A.; Hu, Y. M.; Huerta,
   E. A.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh,
   T.; Indik, N.; Inta, R.; Intini, G.; Isa, H. N.; Isac, J. -M.; Isi,
   M.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jani, K.; Jaranowski,
   P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.; Jones,
   D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Junker, J.; Kalaghatgi,
   C. V.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner,
   J. B.; Kapadia, S. J.; Karki, S.; Karvinen, K. S.; Kasprzack, M.;
   Katolik, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kawabe, K.;
   Kéfélian, F.; Keitel, D.; Kemball, A. J.; Kennedy, R.; Kent, C.;
   Key, J. S.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov,
   E. A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J. C.; Kim, K.; Kim, W.;
   Kim, W. S.; Kim, Y. -M.; Kimbrell, S. J.; King, E. J.; King, P. J.;
   Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J. S.; Kleybolte, L.;
   Klimenko, S.; Knowles, T. D.; Koch, P.; Koehlenbeck, S. M.; Koley,
   S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kowalska,
   I.; Kozak, D. B.; Krämer, C.; Kringel, V.; Krishnan, B.; Królak,
   A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo, L.; Kutynia,
   A.; Kwang, S.; Lackey, B. D.; Lai, K. H.; Landry, M.; Lang, R. N.;
   Lange, J.; Lantz, B.; Lanza, R. K.; Larson, S. L.; Lartaux-Vollard,
   A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.;
   Leavey, S.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Lee, K.;
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   B.; Wei, L. -W.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.;
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   Burns, E.; Cleveland, W. H.; Connaughton, V.; Gibby, M. H.; Giles,
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   K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida,
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   G. C.; Rao, A. R.; Vadawale, S. V.; AstroSat Cadmium Zinc Telluride
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   Zhao, H. S.; Zhao, J. L.; Zhao, X. F.; Zheng, S. J.; Zhu, Y.; Zhu,
   Y. X.; Zou, C. L.; Insight-HXMT Collaboration; Albert, A.; André,
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   T.; Baret, B.; Barrios-Martí, J.; Basa, S.; Belhorma, B.; Bertin, V.;
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   Van Elewyck, V.; Versari, F.; Vivolo, D.; Vizzoca, A.; Wilms, J.;
   Zornoza, J. D.; Zúñiga, J.; ANTARES Collaboration; Beardmore, A. P.;
   Breeveld, A. A.; Burrows, D. N.; Cenko, S. B.; Cusumano, G.; D'Aì, A.;
   de Pasquale, M.; Emery, S. W. K.; Evans, P. A.; Giommi, P.; Gronwall,
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   F. E.; Melandri, A.; Nousek, J. A.; Oates, S. R.; Osborne, J. P.;
   Pagani, C.; Page, K. L.; Palmer, D. M.; Perri, M.; Siegel, M. H.;
   Sbarufatti, B.; Tagliaferri, G.; Tohuvavohu, A.; Swift Collaboration;
   Tavani, M.; Verrecchia, F.; Bulgarelli, A.; Evangelista, Y.; Pacciani,
   L.; Feroci, M.; Pittori, C.; Giuliani, A.; Del Monte, E.; Donnarumma,
   I.; Argan, A.; Trois, A.; Ursi, A.; Cardillo, M.; Piano, G.; Longo,
   F.; Lucarelli, F.; Munar-Adrover, P.; Fuschino, F.; Labanti, C.;
   Marisaldi, M.; Minervini, G.; Fioretti, V.; Parmiggiani, N.; Gianotti,
   F.; Trifoglio, M.; Di Persio, G.; Antonelli, L. A.; Barbiellini, G.;
   Caraveo, P.; Cattaneo, P. W.; Costa, E.; Colafrancesco, S.; D'Amico,
   F.; Ferrari, A.; Morselli, A.; Paoletti, F.; Picozza, P.; Pilia,
   M.; Rappoldi, A.; Soffitta, P.; Vercellone, S.; AGILE Team; Foley,
   R. J.; Coulter, D. A.; Kilpatrick, C. D.; Drout, M. R.; Piro, A. L.;
   Shappee, B. J.; Siebert, M. R.; Simon, J. D.; Ulloa, N.; Kasen, D.;
   Madore, B. F.; Murguia-Berthier, A.; Pan, Y. -C.; Prochaska, J. X.;
   Ramirez-Ruiz, E.; Rest, A.; Rojas-Bravo, C.; 1M2H Team; Berger, E.;
   Soares-Santos, M.; Annis, J.; Alexander, K. D.; Allam, S.; Balbinot,
   E.; Blanchard, P.; Brout, D.; Butler, R. E.; Chornock, R.; Cook,
   E. R.; Cowperthwaite, P.; Diehl, H. T.; Drlica-Wagner, A.; Drout,
   M. R.; Durret, F.; Eftekhari, T.; Finley, D. A.; Fong, W.; Frieman,
   J. A.; Fryer, C. L.; García-Bellido, J.; Gruendl, R. A.; Hartley,
   W.; Herner, K.; Kessler, R.; Lin, H.; Lopes, P. A. A.; Lourenço,
   A. C. C.; Margutti, R.; Marshall, J. L.; Matheson, T.; Medina, G. E.;
   Metzger, B. D.; Muñoz, R. R.; Muir, J.; Nicholl, M.; Nugent, P.;
   Palmese, A.; Paz-Chinchón, F.; Quataert, E.; Sako, M.; Sauseda, M.;
   Schlegel, D. J.; Scolnic, D.; Secco, L. F.; Smith, N.; Sobreira, F.;
   Villar, V. A.; Vivas, A. K.; Wester, W.; Williams, P. K. G.; Yanny,
   B.; Zenteno, A.; Zhang, Y.; Abbott, T. M. C.; Banerji, M.; Bechtol,
   K.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke,
   D. L.; Capozzi, D.; Carnero Rosell, A.; Carrasco Kind, M.; Castander,
   F. J.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.;
   Davis, C.; DePoy, D. L.; Desai, S.; Dietrich, J. P.; Eifler, T. F.;
   Fernandez, E.; Flaugher, B.; Fosalba, P.; Gaztanaga, E.; Gerdes,
   D. W.; Giannantonio, T.; Goldstein, D. A.; Gruen, D.; Gschwend, J.;
   Gutierrez, G.; Honscheid, K.; James, D. J.; Jeltema, T.; Johnson,
   M. W. G.; Johnson, M. D.; Kent, S.; Krause, E.; Kron, R.; Kuehn, K.;
   Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Martini, P.; McMahon,
   R. G.; Menanteau, F.; Miller, C. J.; Miquel, R.; Mohr, J. J.; Nichol,
   R. C.; Ogando, R. L. C.; Plazas, A. A.; Romer, A. K.; Roodman, A.;
   Rykoff, E. S.; Sanchez, E.; Scarpine, V.; Schindler, R.; Schubnell,
   M.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, M.; Smith, R. C.; Stebbins,
   A.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, R. C.; Troxel,
   M. A.; Tucker, D. L.; Vikram, V.; Walker, A. R.; Wechsler, R. H.;
   Weller, J.; Carlin, J. L.; Gill, M. S. S.; Li, T. S.; Marriner, J.;
   Neilsen, E.; Dark Energy Camera GW-EM Collaboration; DES Collaboration;
   Haislip, J. B.; Kouprianov, V. V.; Reichart, D. E.; Sand, D. J.;
   Tartaglia, L.; Valenti, S.; Yang, S.; DLT40 Collaboration; Benetti,
   S.; Brocato, E.; Campana, S.; Cappellaro, E.; Covino, S.; D'Avanzo,
   P.; D'Elia, V.; Getman, F.; Ghirlanda, G.; Ghisellini, G.; Limatola,
   L.; Nicastro, L.; Palazzi, E.; Pian, E.; Piranomonte, S.; Possenti,
   A.; Rossi, A.; Salafia, O. S.; Tomasella, L.; Amati, L.; Antonelli,
   L. A.; Bernardini, M. G.; Bufano, F.; Capaccioli, M.; Casella, P.;
   Dadina, M.; De Cesare, G.; Di Paola, A.; Giuffrida, G.; Giunta,
   A.; Israel, G. L.; Lisi, M.; Maiorano, E.; Mapelli, M.; Masetti,
   N.; Pescalli, A.; Pulone, L.; Salvaterra, R.; Schipani, P.; Spera,
   M.; Stamerra, A.; Stella, L.; Testa, V.; Turatto, M.; Vergani, D.;
   Aresu, G.; Bachetti, M.; Buffa, F.; Burgay, M.; Buttu, M.; Caria,
   T.; Carretti, E.; Casasola, V.; Castangia, P.; Carboni, G.; Casu,
   S.; Concu, R.; Corongiu, A.; Deiana, G. L.; Egron, E.; Fara, A.;
   Gaudiomonte, F.; Gusai, V.; Ladu, A.; Loru, S.; Leurini, S.; Marongiu,
   L.; Melis, A.; Melis, G.; Migoni, Carlo; Milia, Sabrina; Navarrini,
   Alessandro; Orlati, A.; Ortu, P.; Palmas, S.; Pellizzoni, A.; Perrodin,
   D.; Pisanu, T.; Poppi, S.; Righini, S.; Saba, A.; Serra, G.; Serrau,
   M.; Stagni, M.; Surcis, G.; Vacca, V.; Vargiu, G. P.; Hunt, L. K.;
   Jin, Z. P.; Klose, S.; Kouveliotou, C.; Mazzali, P. A.; Møller, P.;
   Nava, L.; Piran, T.; Selsing, J.; Vergani, S. D.; Wiersema, K.; Toma,
   K.; Higgins, A. B.; Mundell, C. G.; di Serego Alighieri, S.; Gótz,
   D.; Gao, W.; Gomboc, A.; Kaper, L.; Kobayashi, S.; Kopac, D.; Mao,
J.; Starling, R. L. C.; Steele, I.; van der Horst, A. J.; GRAWITA:
   GRAvitational Wave Inaf TeAm; Acero, F.; Atwood, W. B.; Baldini,
   L.; Barbiellini, G.; Bastieri, D.; Berenji, B.; Bellazzini, R.;
   Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini,
   E.; Bregeon, J.; Buehler, R.; Buson, S.; Cameron, R. A.; Caputo, R.;
   Caraveo, P. A.; Cavazzuti, E.; Chekhtman, A.; Cheung, C. C.; Chiang,
   J.; Ciprini, S.; Cohen-Tanugi, J.; Cominsky, L. R.; Costantin, D.;
   Cuoco, A.; D'Ammando, F.; de Palma, F.; Digel, S. W.; Di Lalla,
   N.; Di Mauro, M.; Di Venere, L.; Dubois, R.; Fegan, S. J.; Focke,
   W. B.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano,
   F.; Gasparrini, D.; Giglietto, N.; Giordano, F.; Giroletti, M.;
   Glanzman, T.; Green, D.; Grondin, M. -H.; Guillemot, L.; Guiriec,
   S.; Harding, A. K.; Horan, D.; Jóhannesson, G.; Kamae, T.; Kensei,
   S.; Kuss, M.; La Mura, G.; Latronico, L.; Lemoine-Goumard, M.;
   Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill,
   J. D.; Maldera, S.; Manfreda, A.; Mazziotta, M. N.; McEnery, J. E.;
   Meyer, M.; Michelson, P. F.; Mirabal, N.; Monzani, M. E.; Moretti,
   E.; Morselli, A.; Moskalenko, I. V.; Negro, M.; Nuss, E.; Ojha, R.;
   Omodei, N.; Orienti, M.; Orlando, E.; Palatiello, M.; Paliya, V. S.;
   Paneque, D.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Principe, G.;
   Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer,
   O.; Reposeur, T.; Rochester, L. S.; Saz Parkinson, P. M.; Sgrò, C.;
   Siskind, E. J.; Spada, F.; Spandre, G.; Suson, D. J.; Takahashi, M.;
   Tanaka, Y.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo,
   L.; Torres, D. F.; Torresi, E.; Troja, E.; Venters, T. M.; Vianello,
   G.; Zaharijas, G.; Fermi Large Area Telescope Collaboration; Allison,
   J. R.; Bannister, K. W.; Dobie, D.; Kaplan, D. L.; Lenc, E.; Lynch,
   C.; Murphy, T.; Sadler, E. M.; Australia Telescope Compact Array,
ATCA:; Hotan, A.; James, C. W.; Oslowski, S.; Raja, W.; Shannon,
R. M.; Whiting, M.; Australian SKA Pathfinder, ASKAP:; Arcavi,
   I.; Howell, D. A.; McCully, C.; Hosseinzadeh, G.; Hiramatsu, D.;
   Poznanski, D.; Barnes, J.; Zaltzman, M.; Vasylyev, S.; Maoz, D.; Las
   Cumbres Observatory Group; Cooke, J.; Bailes, M.; Wolf, C.; Deller,
   A. T.; Lidman, C.; Wang, L.; Gendre, B.; Andreoni, I.; Ackley, K.;
   Pritchard, T. A.; Bessell, M. S.; Chang, S. -W.; Möller, A.; Onken,
   C. A.; Scalzo, R. A.; Ridden-Harper, R.; Sharp, R. G.; Tucker, B. E.;
   Farrell, T. J.; Elmer, E.; Johnston, S.; Venkatraman Krishnan, V.;
   Keane, E. F.; Green, J. A.; Jameson, A.; Hu, L.; Ma, B.; Sun, T.;
   Wu, X.; Wang, X.; Shang, Z.; Hu, Y.; Ashley, M. C. B.; Yuan, X.; Li,
   X.; Tao, C.; Zhu, Z.; Zhang, H.; Suntzeff, N. B.; Zhou, J.; Yang, J.;
   Orange, B.; Morris, D.; Cucchiara, A.; Giblin, T.; Klotz, A.; Staff,
   J.; Thierry, P.; Schmidt, B. P.; OzGrav; (Deeper, DWF; Wider; program,
   Faster; AST3; CAASTRO Collaborations; Tanvir, N. R.; Levan, A. J.;
   Cano, Z.; de Ugarte-Postigo, A.; González-Fernández, C.; Greiner,
   J.; Hjorth, J.; Irwin, M.; Krühler, T.; Mandel, I.; Milvang-Jensen,
   B.; O'Brien, P.; Rol, E.; Rosetti, S.; Rosswog, S.; Rowlinson, A.;
   Steeghs, D. T. H.; Thöne, C. C.; Ulaczyk, K.; Watson, D.; Bruun,
   S. H.; Cutter, R.; Figuera Jaimes, R.; Fujii, Y. I.; Fruchter, A. S.;
   Gompertz, B.; Jakobsson, P.; Hodosan, G.; Jèrgensen, U. G.; Kangas,
   T.; Kann, D. A.; Rabus, M.; Schrøder, S. L.; Stanway, E. R.; Wijers,
   R. A. M. J.; VINROUGE Collaboration; Lipunov, V. M.; Gorbovskoy, E. S.;
   Kornilov, V. G.; Tyurina, N. V.; Balanutsa, P. V.; Kuznetsov, A. S.;
   Vlasenko, D. M.; Podesta, R. C.; Lopez, C.; Podesta, F.; Levato,
   H. O.; Saffe, C.; Mallamaci, C. C.; Budnev, N. M.; Gress, O. A.;
   Kuvshinov, D. A.; Gorbunov, I. A.; Vladimirov, V. V.; Zimnukhov,
   D. S.; Gabovich, A. V.; Yurkov, V. V.; Sergienko, Yu. P.; Rebolo,
   R.; Serra-Ricart, M.; Tlatov, A. G.; Ishmuhametova, Yu. V.; MASTER
   Collaboration; Abe, F.; Aoki, K.; Aoki, W.; Asakura, Y.; Baar, S.;
   Barway, S.; Bond, I. A.; Doi, M.; Finet, F.; Fujiyoshi, T.; Furusawa,
   H.; Honda, S.; Itoh, R.; Kanda, N.; Kawabata, K. S.; Kawabata, M.; Kim,
   J. H.; Koshida, S.; Kuroda, D.; Lee, C. -H.; Liu, W.; Matsubayashi,
   K.; Miyazaki, S.; Morihana, K.; Morokuma, T.; Motohara, K.; Murata,
   K. L.; Nagai, H.; Nagashima, H.; Nagayama, T.; Nakaoka, T.; Nakata,
   F.; Ohsawa, R.; Ohshima, T.; Ohta, K.; Okita, H.; Saito, T.; Saito,
   Y.; Sako, S.; Sekiguchi, Y.; Sumi, T.; Tajitsu, A.; Takahashi,
   J.; Takayama, M.; Tamura, Y.; Tanaka, I.; Tanaka, M.; Terai, T.;
   Tominaga, N.; Tristram, P. J.; Uemura, M.; Utsumi, Y.; Yamaguchi,
   M. S.; Yasuda, N.; Yoshida, M.; Zenko, T.; J-GEM; Adams, S. M.;
   Anupama, G. C.; Bally, J.; Barway, S.; Bellm, E.; Blagorodnova, N.;
   Cannella, C.; Chandra, P.; Chatterjee, D.; Clarke, T. E.; Cobb, B. E.;
   Cook, D. O.; Copperwheat, C.; De, K.; Emery, S. W. K.; Feindt, U.;
   Foster, K.; Fox, O. D.; Frail, D. A.; Fremling, C.; Frohmaier, C.;
   Garcia, J. A.; Ghosh, S.; Giacintucci, S.; Goobar, A.; Gottlieb, O.;
   Grefenstette, B. W.; Hallinan, G.; Harrison, F.; Heida, M.; Helou,
   G.; Ho, A. Y. Q.; Horesh, A.; Hotokezaka, K.; Ip, W. -H.; Itoh, R.;
   Jacobs, Bob; Jencson, J. E.; Kasen, D.; Kasliwal, M. M.; Kassim,
   N. E.; Kim, H.; Kiran, B. S.; Kuin, N. P. M.; Kulkarni, S. R.;
   Kupfer, T.; Lau, R. M.; Madsen, K.; Mazzali, P. A.; Miller, A. A.;
   Miyasaka, H.; Mooley, K.; Myers, S. T.; Nakar, E.; Ngeow, C. -C.;
   Nugent, P.; Ofek, E. O.; Palliyaguru, N.; Pavana, M.; Perley, D. A.;
   Peters, W. M.; Pike, S.; Piran, T.; Qi, H.; Quimby, R. M.; Rana, J.;
   Rosswog, S.; Rusu, F.; Sadler, E. M.; Van Sistine, A.; Sollerman, J.;
   Xu, Y.; Yan, L.; Yatsu, Y.; Yu, P. -C.; Zhang, C.; Zhao, W.; GROWTH;
   JAGWAR; Caltech-NRAO; TTU-NRAO; NuSTAR Collaborations; Chambers,
   K. C.; Huber, M. E.; Schultz, A. S. B.; Bulger, J.; Flewelling, H.;
   Magnier, E. A.; Lowe, T. B.; Wainscoat, R. J.; Waters, C.; Willman,
   M.; Pan-STARRS; Ebisawa, K.; Hanyu, C.; Harita, S.; Hashimoto, T.;
   Hidaka, K.; Hori, T.; Ishikawa, M.; Isobe, N.; Iwakiri, W.; Kawai,
   H.; Kawai, N.; Kawamuro, T.; Kawase, T.; Kitaoka, Y.; Makishima,
   K.; Matsuoka, M.; Mihara, T.; Morita, T.; Morita, K.; Nakahira, S.;
   Nakajima, M.; Nakamura, Y.; Negoro, H.; Oda, S.; Sakamaki, A.; Sasaki,
   R.; Serino, M.; Shidatsu, M.; Shimomukai, R.; Sugawara, Y.; Sugita,
   S.; Sugizaki, M.; Tachibana, Y.; Takao, Y.; Tanimoto, A.; Tomida, H.;
   Tsuboi, Y.; Tsunemi, H.; Ueda, Y.; Ueno, S.; Yamada, S.; Yamaoka,
   K.; Yamauchi, M.; Yatabe, F.; Yoneyama, T.; Yoshii, T.; MAXI Team;
   Coward, D. M.; Crisp, H.; Macpherson, D.; Andreoni, I.; Laugier,
   R.; Noysena, K.; Klotz, A.; Gendre, B.; Thierry, P.; Turpin, D.;
   Consortium, TZAC; Im, M.; Choi, C.; Kim, J.; Yoon, Y.; Lim, G.; Lee,
   S. -K.; Lee, C. -U.; Kim, S. -L.; Ko, S. -W.; Joe, J.; Kwon, M. -K.;
   Kim, P. -J.; Lim, S. -K.; Choi, J. -S.; KU Collaboration; Fynbo,
   J. P. U.; Malesani, D.; Xu, D.; Optical Telescope, Nordic; Smartt,
   S. J.; Jerkstrand, A.; Kankare, E.; Sim, S. A.; Fraser, M.; Inserra,
   C.; Maguire, K.; Leloudas, G.; Magee, M.; Shingles, L. J.; Smith,
   K. W.; Young, D. R.; Kotak, R.; Gal-Yam, A.; Lyman, J. D.; Homan,
   D. S.; Agliozzo, C.; Anderson, J. P.; Angus, C. R.; Ashall, C.;
   Barbarino, C.; Bauer, F. E.; Berton, M.; Botticella, M. T.; Bulla,
   M.; Cannizzaro, G.; Cartier, R.; Cikota, A.; Clark, P.; De Cia,
   A.; Della Valle, M.; Dennefeld, M.; Dessart, L.; Dimitriadis, G.;
   Elias-Rosa, N.; Firth, R. E.; Flörs, A.; Frohmaier, C.; Galbany, L.;
   González-Gaitán, S.; Gromadzki, M.; Gutiérrez, C. P.; Hamanowicz,
   A.; Harmanen, J.; Heintz, K. E.; Hernandez, M. -S.; Hodgkin, S. T.;
   Hook, I. M.; Izzo, L.; James, P. A.; Jonker, P. G.; Kerzendorf, W. E.;
   Kostrzewa-Rutkowska, Z.; Kromer, M.; Kuncarayakti, H.; Lawrence,
   A.; Manulis, I.; Mattila, S.; McBrien, O.; Müller, A.; Nordin, J.;
   O'Neill, D.; Onori, F.; Palmerio, J. T.; Pastorello, A.; Patat, F.;
   Pignata, G.; Podsiadlowski, P.; Razza, A.; Reynolds, T.; Roy, R.;
   Ruiter, A. J.; Rybicki, K. A.; Salmon, L.; Pumo, M. L.; Prentice,
   S. J.; Seitenzahl, I. R.; Smith, M.; Sollerman, J.; Sullivan, M.;
   Szegedi, H.; Taddia, F.; Taubenberger, S.; Terreran, G.; Van Soelen,
   B.; Vos, J.; Walton, N. A.; Wright, D. E.; Wyrzykowski, Ł.; Yaron,
   O.; pre="(">ePESSTO, <author; Chen, T. -W.; Krühler, T.; Schady,
   P.; Wiseman, P.; Greiner, J.; Rau, A.; Schweyer, T.; Klose, S.;
   Nicuesa Guelbenzu, A.; GROND; Palliyaguru, N. T.; Tech University,
   Texas; Shara, M. M.; Williams, T.; Vaisanen, P.; Potter, S. B.; Romero
   Colmenero, E.; Crawford, S.; Buckley, D. A. H.; Mao, J.; SALT Group;
   Díaz, M. C.; Macri, L. M.; García Lambas, D.; Mendes de Oliveira,
   C.; Nilo Castellón, J. L.; Ribeiro, T.; Sánchez, B.; Schoenell,
   W.; Abramo, L. R.; Akras, S.; Alcaniz, J. S.; Artola, R.; Beroiz,
   M.; Bonoli, S.; Cabral, J.; Camuccio, R.; Chavushyan, V.; Coelho,
   P.; Colazo, C.; Costa-Duarte, M. V.; Cuevas Larenas, H.; Domínguez
   Romero, M.; Dultzin, D.; Fernández, D.; García, J.; Girardini, C.;
   Gonçalves, D. R.; Gonçalves, T. S.; Gurovich, S.; Jiménez-Teja, Y.;
   Kanaan, A.; Lares, M.; Lopes de Oliveira, R.; López-Cruz, O.; Melia,
   R.; Molino, A.; Padilla, N.; Peñuela, T.; Placco, V. M.; Quiñones,
   C.; Ramírez Rivera, A.; Renzi, V.; Riguccini, L.; Ríos-López, E.;
   Rodriguez, H.; Sampedro, L.; Schneiter, M.; Sodré, L.; Starck, M.;
Torres-Flores, S.; Tornatore, M.; Zadrożny, A.; Castillo, M.; TOROS:
   Transient Robotic Observatory of South Collaboration; Castro-Tirado,
   A. J.; Tello, J. C.; Hu, Y. -D.; Zhang, B. -B.; Cunniffe, R.;
   Castellón, A.; Hiriart, D.; Caballero-García, M. D.; Jelínek,
   M.; Kubánek, P.; Pérez del Pulgar, C.; Park, I. H.; Jeong, S.;
   Castro Cerón, J. M.; Pandey, S. B.; Yock, P. C.; Querel, R.; Fan,
   Y.; Wang, C.; BOOTES Collaboration; Beardsley, A.; Brown, I. S.;
   Crosse, B.; Emrich, D.; Franzen, T.; Gaensler, B. M.; Horsley,
   L.; Johnston-Hollitt, M.; Kenney, D.; Morales, M. F.; Pallot, D.;
   Sokolowski, M.; Steele, K.; Tingay, S. J.; Trott, C. M.; Walker, M.;
Wayth, R.; Williams, A.; Wu, C.; Murchison Widefield Array, MWA:;
   Yoshida, A.; Sakamoto, T.; Kawakubo, Y.; Yamaoka, K.; Takahashi,
   I.; Asaoka, Y.; Ozawa, S.; Torii, S.; Shimizu, Y.; Tamura, T.;
   Ishizaki, W.; Cherry, M. L.; Ricciarini, S.; Penacchioni, A. V.;
   Marrocchesi, P. S.; CALET Collaboration; Pozanenko, A. S.; Volnova,
   A. A.; Mazaeva, E. D.; Minaev, P. Yu.; Krugov, M. A.; Kusakin, A. V.;
   Reva, I. V.; Moskvitin, A. S.; Rumyantsev, V. V.; Inasaridze, R.;
   Klunko, E. V.; Tungalag, N.; Schmalz, S. E.; Burhonov, O.; IKI-GW
   Follow-up Collaboration; Abdalla, H.; Abramowski, A.; Aharonian, F.;
   Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arrieta, M.; Aubert,
   P.; Backes, M.; Balzer, A.; Barnard, M.; Becherini, Y.; Becker Tjus,
   J.; Berge, D.; Bernhard, S.; Bernlöhr, K.; Blackwell, R.; Böttcher,
   M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bordas, P.; Bregeon, J.;
   Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Capasso, M.;
   Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chakraborty, N.;
   Chaves, R. C. G.; Chen, A.; Chevalier, J.; Colafrancesco, S.; Condon,
   B.; Conrad, J.; Davids, I. D.; Decock, J.; Deil, C.; Devin, J.; deWilt,
   P.; Dirson, L.; Djannati-Ataï, A.; Donath, A.; O'C. Drury, L.; Dutson,
   K.; Dyks, J.; Edwards, T.; Egberts, K.; Emery, G.; Ernenwein, J. -P.;
   Eschbach, S.; Farnier, C.; Fegan, S.; Fernandes, M. V.; Fiasson, A.;
   Fontaine, G.; Funk, S.; Füssling, M.; Gabici, S.; Gallant, Y. A.;
   Garrigoux, T.; Gaté, F.; Giavitto, G.; Giebels, B.; Glawion, D.;
   Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.;
   Haupt, M.; Hawkes, J.; Heinzelmann, G.; Henri, G.; Hermann, G.;
   Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.;
   Horns, D.; Ivascenko, A.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.;
   Jankowsky, D.; Jankowsky, F.; Jingo, M.; Jouvin, L.; Jung-Richardt,
   I.; Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Kerszberg,
   D.; Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Klochkov,
   D.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Krakau, S.; Kraus, M.;
   Krüger, P. P.; Laffon, H.; Lamanna, G.; Lau, J.; Lees, J. -P.;
   Lefaucheur, J.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.;
   Leser, E.; Lohse, T.; Lorentz, M.; Liu, R.; Lypova, I.; Malyshev,
   D.; Marandon, V.; Marcowith, A.; Mariaud, C.; Marx, R.; Maurin, G.;
   Maxted, N.; Mayer, M.; Meintjes, P. J.; Meyer, M.; Mitchell, A. M. W.;
   Moderski, R.; Mohamed, M.; Mohrmann, L.; Morå, K.; Moulin, E.; Murach,
   T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.;
   Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; Ostrowski,
   M.; Oya, I.; Padovani, M.; Panter, M.; Parsons, R. D.; Pekeur,
   N. W.; Pelletier, G.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.;
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2017ApJ...848L..12A    Altcode: 2017arXiv171005833L
  On 2017 August 17 a binary neutron star coalescence candidate (later
  designated GW170817) with merger time 12:41:04 UTC was observed
  through gravitational waves by the Advanced LIGO and Advanced Virgo
  detectors. The Fermi Gamma-ray Burst Monitor independently detected a
  gamma-ray burst (GRB 170817A) with a time delay of ∼ 1.7 {{s}} with
  respect to the merger time. From the gravitational-wave signal, the
  source was initially localized to a sky region of 31 deg<SUP>2</SUP>
  at a luminosity distance of {40}<SUB>-8</SUB><SUP>+8</SUP> Mpc and
  with component masses consistent with neutron stars. The component
  masses were later measured to be in the range 0.86 to 2.26 {M}<SUB>⊙
  </SUB>. An extensive observing campaign was launched across the
  electromagnetic spectrum leading to the discovery of a bright optical
  transient (SSS17a, now with the IAU identification of AT 2017gfo) in
  NGC 4993 (at ∼ 40 {{Mpc}}) less than 11 hours after the merger by the
  One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The
  optical transient was independently detected by multiple teams
  within an hour. Subsequent observations targeted the object and its
  environment. Early ultraviolet observations revealed a blue transient
  that faded within 48 hours. Optical and infrared observations showed
  a redward evolution over ∼10 days. Following early non-detections,
  X-ray and radio emission were discovered at the transient's position ∼
  9 and ∼ 16 days, respectively, after the merger. Both the X-ray and
  radio emission likely arise from a physical process that is distinct
  from the one that generates the UV/optical/near-infrared emission. No
  ultra-high-energy gamma-rays and no neutrino candidates consistent with
  the source were found in follow-up searches. These observations support
  the hypothesis that GW170817 was produced by the merger of two neutron
  stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A)
  and a kilonova/macronova powered by the radioactive decay of r-process
  nuclei synthesized in the ejecta. <P />Any correspondence should be
  addressed to .

---------------------------------------------------------
Title: All-sky search for periodic gravitational waves in the O1
    LIGO data
Authors: Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.;
   Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya,
   V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agatsuma, K.; Aggarwal,
   N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.; Allen, B.; Allen,
   G.; Allocca, A.; Altin, P. A.; Amato, A.; Ananyeva, A.; Anderson,
   S. B.; Anderson, W. G.; Antier, S.; Appert, S.; Arai, K.; Araya,
   M. C.; Areeda, J. S.; Arnaud, N.; Ascenzi, S.; Ashton, G.; Ast, M.;
   Aston, S. M.; Astone, P.; Aufmuth, P.; Aulbert, C.; AultONeal, K.;
   Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.; Bae, S.;
   Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.; Banagiri,
   S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker, D.; Barone,
   F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Bartlett, J.;
   Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Baune, C.; Bawaj,
   M.; Bazzan, M.; Bécsy, B.; Beer, C.; Bejger, M.; Belahcene, I.; Bell,
   A. S.; Berger, B. K.; Bergmann, G.; Berry, C. P. L.; Bersanetti, D.;
   Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko,
   I. A.; Billingsley, G.; Billman, C. R.; Birch, J.; Birney, R.;
   Birnholtz, O.; Biscans, S.; Bisht, A.; Bitossi, M.; Biwer, C.;
   Bizouard, M. A.; Blackburn, J. K.; Blackman, J.; Blair, C. D.;
   Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bode, N.; Boer,
   M.; Bogaert, G.; Bohe, A.; Bondu, F.; Bonnand, R.; Boom, B. A.; Bork,
   R.; Boschi, V.; Bose, S.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.;
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   Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill, P.; Broida, J. E.;
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   Fisher, R. P.; Flaminio, R.; Fletcher, M.; Fong, H.; Forsyth, P. W. F.;
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   S.; Giaime, J. A.; Giardina, K. D.; Giazotto, A.; Gill, K.; Glover,
   L.; Goetz, E.; Goetz, R.; Gomes, S.; González, G.; Gonzalez Castro,
   J. M.; Gopakumar, A.; Gorodetsky, M. L.; Gossan, S. E.; Gosselin, M.;
   Gouaty, R.; Grado, A.; Graef, C.; Granata, M.; Grant, A.; Gras, S.;
   Gray, C.; Greco, G.; Green, A. C.; Groot, P.; Grote, H.; Grunewald,
   S.; Gruning, P.; Guidi, G. M.; Guo, X.; Gupta, A.; Gupta, M. K.;
   Gushwa, K. E.; Gustafson, E. K.; Gustafson, R.; Hall, B. R.; Hall,
   E. D.; Hammond, G.; Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.;
   Hannuksela, O. A.; Hanson, J.; Hardwick, T.; Harms, J.; Harry, G. M.;
   Harry, I. W.; Hart, M. J.; Haster, C. -J.; Haughian, K.; Healy, J.;
   Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.;
   Hendry, M.; Heng, I. S.; Hennig, J.; Henry, J.; Heptonstall, A. W.;
   Heurs, M.; Hild, S.; Hoak, D.; Hofman, D.; Holt, K.; Holz, D. E.;
   Hopkins, P.; Horst, C.; Hough, J.; Houston, E. A.; Howell, E. J.;
   Hu, Y. M.; Huerta, E. A.; Huet, D.; Hughey, B.; Husa, S.; Huttner,
   S. H.; Huynh-Dinh, T.; Indik, N.; Ingram, D. R.; Inta, R.; Intini, G.;
   Isa, H. N.; Isac, J. -M.; Isi, M.; Iyer, B. R.; Izumi, K.; Jacqmin,
   T.; Jani, K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.;
   Johnson, W. W.; Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju,
   L.; Junker, J.; Kalaghatgi, C. V.; Kalogera, V.; Kandhasamy, S.;
   Kang, G.; Kanner, J. B.; Karki, S.; Karvinen, K. S.; Kasprzack, M.;
   Katolik, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kawabe, K.;
   Kéfélian, F.; Keitel, D.; Kemball, A. J.; Kennedy, R.; Kent, C.;
   Key, J. S.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov,
   E. A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J. C.; Kim, W.; Kim, W. S.;
   Kim, Y. -M.; Kimbrell, S. J.; King, E. J.; King, P. J.; Kirchhoff, R.;
   Kissel, J. S.; Kleybolte, L.; Klimenko, S.; Koch, P.; Koehlenbeck,
   S. M.; Koley, S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth,
   W. Z.; Kowalska, I.; Kozak, D. B.; Krämer, C.; Kringel, V.; Krishnan,
   B.; Królak, A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo,
   L.; Kutynia, A.; Kwang, S.; Lackey, B. D.; Lai, K. H.; Landry, M.;
   Lang, R. N.; Lange, J.; Lantz, B.; Lanza, R. K.; Lartaux-Vollard,
   A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.;
   Leavey, S.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Lee, K.;
   Lehmann, J.; Lenon, A.; Leonardi, M.; Leroy, N.; Letendre, N.; Levin,
   Y.; Li, T. G. F.; Libson, A.; Littenberg, T. B.; Liu, J.; Liu, W.; Lo,
   R. K. L.; Lockerbie, N. A.; London, L. T.; Lord, J. E.; Lorenzini,
   M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lovelace,
   G.; Lück, H.; Lumaca, D.; Lundgren, A. P.; Lynch, R.; Ma, Y.; Macfoy,
   S.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Magaña Hernandez,
   I.; Magaña-Sandoval, F.; Magaña Zertuche, L.; Magee, R. M.; Majorana,
   E.; Maksimovic, I.; Man, N.; Mandic, V.; Mangano, V.; Mansell, G. L.;
   Manske, M.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.;
   Márka, Z.; Markakis, C.; Markosyan, A. S.; Maros, E.; Martelli, F.;
   Martellini, L.; Martin, I. W.; Martynov, D. V.; Marx, J. N.; Mason,
   K.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Mastrogiovanni,
   S.; Matas, A.; Matichard, F.; Matone, L.; Mavalvala, N.; Mayani,
   R.; Mazumder, N.; McCarthy, R.; McClelland, D. E.; McCormick, S.;
   McCuller, L.; McGuire, S. C.; McIntyre, G.; McIver, J.; McManus,
   D. J.; McRae, T.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.;
   Meidam, J.; Mejuto-Villa, E.; Melatos, A.; Mendell, G.; Mercer, R. A.;
   Merilh, E. L.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick,
   C.; Metzdorff, R.; Meyers, P. M.; Mezzani, F.; Miao, H.; Michel,
   C.; Middleton, H.; Mikhailov, E. E.; Milano, L.; Miller, A. L.;
   Miller, A.; Miller, B. B.; Miller, J.; Millhouse, M.; Minazzoli, O.;
   Minenkov, Y.; Ming, J.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.;
   Mitselmakher, G.; Mittleman, R.; Moggi, A.; Mohan, M.; Mohapatra,
   S. R. P.; Montani, M.; Moore, B. C.; Moore, C. J.; Moraru, D.;
   Moreno, G.; Morriss, S. R.; Mours, B.; Mow-Lowry, C. M.; Mueller,
   G.; Muir, A. W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, S.;
   Mukund, N.; Mullavey, A.; Munch, J.; Muniz, E. A. M.; Murray, P. G.;
   Napier, K.; Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Nelemans,
   G.; Nelson, T. J. N.; Neri, M.; Nery, M.; Neunzert, A.; Newport,
   J. M.; Newton, G.; Ng, K. K. Y.; Nguyen, T. T.; Nichols, D.; Nielsen,
   A. B.; Nissanke, S.; Nitz, A.; Noack, A.; Nocera, F.; Nolting, D.;
   Normandin, M. E. N.; Nuttall, L. K.; Oberling, J.; Ochsner, E.;
   Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, S. H.; Ohme, F.; Oliver, M.;
   Oppermann, P.; Oram, Richard J.; O'Reilly, B.; Ormiston, R.; Ortega,
   L. F.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.;
   Pace, A. E.; Page, J.; Page, M. A.; Pai, A.; Pai, S. A.; Palamos,
   J. R.; Palashov, O.; Palomba, C.; Pal-Singh, A.; Pan, H.; Pang, B.;
   Pang, P. T. H.; Pankow, C.; Pannarale, F.; Pant, B. C.; Paoletti,
   F.; Paoli, A.; Papa, M. A.; Paris, H. R.; Parker, W.; Pascucci, D.;
   Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patricelli, B.;
   Pearlstone, B. L.; Pedraza, M.; Pedurand, R.; Pekowsky, L.; Pele, A.;
   Penn, S.; Perez, C. J.; Perreca, A.; Perri, L. M.; Pfeiffer, H. P.;
   Phelps, M.; Piccinni, O. J.; Pichot, M.; Piergiovanni, F.; Pierro,
   V.; Pillant, G.; Pinard, L.; Pinto, I. M.; Pisarski, A.; Pitkin, M.;
   Poggiani, R.; Popolizio, P.; Porter, E. K.; Post, A.; Powell, J.;
   Prasad, J.; Pratt, J. W. W.; Predoi, V.; Prestegard, T.; Prijatelj,
   M.; Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov,
   L. G.; Puncken, O.; Punturo, M.; Puppo, P.; Pürrer, M.; Qi, H.; Qin,
   J.; Qiu, S.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab,
   F. J.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raja, S.; Rajan, C.;
   Rakhmanov, M.; Ramirez, K. E.; Rapagnani, P.; Raymond, V.; Razzano,
   M.; Read, J.; Regimbau, T.; Rei, L.; Reid, S.; Reitze, D. H.; Rew,
   H.; Reyes, S. D.; Ricci, F.; Ricker, P. M.; Rieger, S.; Riles, K.;
   Rizzo, M.; Robertson, N. A.; Robie, R.; Robinet, F.; Rocchi, A.;
   Rolland, L.; Rollins, J. G.; Roma, V. J.; Romano, R.; Romel, C. L.;
   Romie, J. H.; Rosińska, D.; Ross, M. P.; Rowan, S.; Rüdiger, A.;
   Ruggi, P.; Ryan, K.; Rynge, M.; Sachdev, S.; Sadecki, T.; Sadeghian,
   L.; Sakellariadou, M.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar,
   A.; Sammut, L.; Sampson, L. M.; Sanchez, E. J.; Sandberg, V.; Sandeen,
   B.; Sanders, J. R.; Sassolas, B.; Saulson, P. R.; Sauter, O.; Savage,
   R. L.; Sawadsky, A.; Schale, P.; Scheuer, J.; Schmidt, E.; Schmidt,
   J.; Schmidt, P.; Schnabel, R.; Schofield, R. M. S.; Schönbeck, A.;
   Schreiber, E.; Schuette, D.; Schulte, B. W.; Schutz, B. F.; Schwalbe,
   S. G.; Scott, J.; Scott, S. M.; Seidel, E.; Sellers, D.; Sengupta,
   A. S.; Sentenac, D.; Sequino, V.; Sergeev, A.; Shaddock, D. A.;
   Shaffer, T. J.; Shah, A. A.; Shahriar, M. S.; Shao, L.; Shapiro,
   B.; Shawhan, P.; Sheperd, A.; Shoemaker, D. H.; Shoemaker, D. M.;
   Siellez, K.; Siemens, X.; Sieniawska, M.; Sigg, D.; Silva, A. D.;
   Singer, A.; Singer, L. P.; Singh, A.; Singh, R.; Singhal, A.; Sintes,
   A. M.; Slagmolen, B. J. J.; Smith, B.; Smith, J. R.; Smith, R. J. E.;
   Son, E. J.; Sonnenberg, J. A.; Sorazu, B.; Sorrentino, F.; Souradeep,
   T.; Spencer, A. P.; Srivastava, A. K.; Staley, A.; Steinke, M.;
   Steinlechner, J.; Steinlechner, S.; Steinmeyer, D.; Stephens, B. C.;
   Stone, R.; Strain, K. A.; Stratta, G.; Strigin, S. E.; Sturani,
   R.; Stuver, A. L.; Summerscales, T. Z.; Sun, L.; Sunil, S.; Sutton,
   P. J.; Swinkels, B. L.; Szczepańczyk, M. J.; Tacca, M.; Talukder,
   D.; Tanner, D. B.; Tao, D.; Tápai, M.; Taracchini, A.; Taylor, J. A.;
   Taylor, R.; Theeg, T.; Thomas, E. G.; Thomas, M.; Thomas, P.; Thorne,
   K. A.; Thorne, K. S.; Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov,
   K. V.; Toland, K.; Tonelli, M.; Tornasi, Z.; Torrie, C. I.; Töyrä,
   D.; Travasso, F.; Traylor, G.; Trembath-Reichert, S.; Trifirò, D.;
   Trinastic, J.; Tringali, M. C.; Trozzo, L.; Tsang, K. W.; Tse, M.; Tso,
   R.; Tuyenbayev, D.; Ueno, K.; Ugolini, D.; Unnikrishnan, C. S.; Urban,
   A. L.; Usman, S. A.; Vahi, K.; Vahlbruch, H.; Vajente, G.; Valdes,
   G.; Vallisneri, M.; van Bakel, N.; van Beuzekom, M.; van den Brand,
   J. F. J.; Van Den Broeck, C.; Vander-Hyde, D. C.; van der Schaaf,
   L.; van Heijningen, J. V.; van Veggel, A. A.; Vardaro, M.; Varma, V.;
   Vass, S.; Vasúth, M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch,
   P. J.; Venkateswara, K.; Venugopalan, G.; Verkindt, D.; Vetrano,
   F.; Viceré, A.; Viets, A. D.; Vinciguerra, S.; Vine, D. J.; Vinet,
   J. -Y.; Vitale, S.; Vo, T.; Vocca, H.; Vorvick, C.; Voss, D. V.;
   Vousden, W. D.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade,
   M.; Walet, R.; Walker, M.; Wallace, L.; Walsh, S.; Wang, G.; Wang, H.;
   Wang, J. Z.; Wang, M.; Wang, Y. -F.; Wang, Y.; Ward, R. L.; Warner, J.;
   Was, M.; Watchi, J.; Weaver, B.; Wei, L. -W.; Weinert, M.; Weinstein,
   A. J.; Weiss, R.; Wen, L.; Wessel, E. K.; Weßels, P.; Westphal, T.;
   Wette, K.; Whelan, J. T.; Whiting, B. F.; Whittle, C.; Williams, D.;
   Williams, R. D.; Williamson, A. R.; Willis, J. L.; Willke, B.; Wimmer,
   M. H.; Winkler, W.; Wipf, C. C.; Wittel, H.; Woan, G.; Woehler, J.;
   Wofford, J.; Wong, K. W. K.; Worden, J.; Wright, J. L.; Wu, D. S.;
   Wu, G.; Yam, W.; Yamamoto, H.; Yancey, C. C.; Yap, M. J.; Yu, Hang;
   Yu, Haocun; Yvert, M.; ZadroŻny, A.; Zanolin, M.; Zelenova, T.;
   Zendri, J. -P.; Zevin, M.; Zhang, L.; Zhang, M.; Zhang, T.; Zhang,
   Y. -H.; Zhao, C.; Zhou, M.; Zhou, Z.; Zhu, S.; Zhu, X. J.; Zucker,
   M. E.; Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration
2017PhRvD..96f2002A    Altcode: 2017arXiv170702667L
  We report on an all-sky search for periodic gravitational waves in
  the frequency band 20-475 Hz and with a frequency time derivative in
  the range of [-1.0 ,+0.1 ] ×10<SUP>-8</SUP> Hz /s . Such a signal
  could be produced by a nearby spinning and slightly nonaxisymmetric
  isolated neutron star in our galaxy. This search uses the data from
  Advanced LIGO's first observational run, O1. No periodic gravitational
  wave signals were observed, and upper limits were placed on their
  strengths. The lowest upper limits on worst-case (linearly polarized)
  strain amplitude h<SUB>0</SUB> are ∼4 ×10<SUP>-25</SUP> near 170
  Hz. For a circularly polarized source (most favorable orientation), the
  smallest upper limits obtained are ∼1.5 ×10<SUP>-25</SUP>. These
  upper limits refer to all sky locations and the entire range of
  frequency derivative values. For a population-averaged ensemble of sky
  locations and stellar orientations, the lowest upper limits obtained
  for the strain amplitude are ∼2.5 ×10<SUP>-25</SUP>.

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Title: The Fate of Cool Material in the Hot Corona: Solar Prominences
    and Coronal Rain
Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Vial, Jean-Claude;
   Berger, Thomas
2017SPD....4810501L    Altcode:
  As an important chain of the chromosphere-corona mass cycle,
  some of the million-degree hot coronal mass undergoes a radiative
  cooling instability and condenses into material at chromospheric or
  transition-region temperatures in two distinct forms - prominences
  and coronal rain (some of which eventually falls back to the
  chromosphere). A quiescent prominence usually consists of numerous
  long-lasting, filamentary downflow threads, while coronal rain consists
  of transient mass blobs falling at comparably higher speeds along
  well-defined paths. It remains puzzling why such material of similar
  temperatures exhibit contrasting morphologies and behaviors. We report
  recent SDO/AIA and IRIS observations that suggest different magnetic
  environments being responsible for such distinctions. Specifically,
  in a hybrid prominence-coronal rain complex structure, we found that
  the prominence material is formed and resides near magnetic null points
  that favor the radiative cooling process and provide possibly a high
  plasma-beta environment suitable for the existence of meandering
  prominence threads. As the cool material descends, it turns into
  coronal rain tied onto low-lying coronal loops in a likely low-beta
  environment. Such structures resemble to certain extent the so-called
  coronal spiders or cloud prominences, but the observations reported
  here provide critical new insights. We will discuss the broad physical
  implications of these observations for fundamental questions, such as
  coronal heating and beyond (e.g., in astrophysical and/or laboratory
  plasma environments).

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Title: Structure and Dynamics of Cool Flare Loops Observed by the
    Interface Region Imaging Spectrograph
Authors: Mikuła, K.; Heinzel, P.; Liu, W.; Berlicki, A.
2017ApJ...845...30M    Altcode:
  Flare loops were well observed with the Interface Region Imaging
  Spectrograph (IRIS) during the gradual phase of two solar flares
  on 2014 March 29 and 2015 June 22. Cool flare loops are visible in
  various spectral lines formed at chromospheric and transition-region
  temperatures and exhibit large downflows which correspond to the
  standard scenario. The principal aim of this work is to analyze
  the structure and dynamics of cool flare loops observed in Mg II
  lines. Synthetic profiles of the Mg II h line are computed using the
  classical cloud model and assuming a uniform background intensity. In
  this paper, we study novel IRIS NUV observations of such loops in Mg II
  h and k lines and also show the behavior of hotter lines detected in
  the FUV channel. We obtained the spatial evolution of the velocities:
  near the loop top, the flow velocities are small and they are increasing
  toward the loop legs. Moreover, from slit-jaw image (SJI) movies, we
  observe some plasma upflows into the loops, which are also detectable
  in Mg II spectra. The brightness of the loops systematically decreases
  with increasing flow velocity, and we ascribe this to the effect of
  Doppler dimming, which works for Mg II lines. Emission profiles of Mg
  II were found to be extremely broad, and we explain this through the
  large unresolved non-thermal motions.

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Title: Data-driven Simulations of Magnetic Connectivity in
    Behind-the-Limb Gamma-ray Flares and Associated Coronal Mass Ejections
Authors: Jin, Meng; Petrosian, Vahe; Liu, Wei; Omodei, Nicola
2017SPD....48.0303J    Altcode:
  Recent Fermi detection of high-energy gamma-ray emission from the
  behind-the-limb (BTL) solar flares pose a puzzle on the particle
  acceleration and transport mechanisms in such events. Due to
  the large separation between the flare site and the location of
  gamma-ray emission, it is believed that the associated coronal
  mass ejections (CMEs) play an important role in accelerating and
  subsequently transporting particles back to the Sun to produce obseved
  gamma-rays. We explore this scenario by simulating the CME associated
  with a well-observed flare on 2014 September 1 about 40 degrees behind
  the east solar limb and by comparing the simulation and observational
  results. We utilize a data-driven global magnetohydrodynamics model
  (AWSoM: Alfven-wave Solar Model) to track the dynamical evolution of
  the global magnetic field during the event and investigate the magnetic
  connectivity between the CME/CME-driven shock and the Fermi emission
  region. Moreover, we derive the time-varying shock parameters (e.g.,
  compression ratio, Alfven Mach number, and ThetaBN) over the area
  that is magnetically connected to the visible solar disk where Fermi
  gamma-ray emission originates. Our simulation shows that the visible
  solar disk develops connections both to the flare region and to the
  CME-driven shock during the eruption, which indicate that the CME’s
  interaction with the global solar corona is critical for understanding
  such Fermi BTL events and gamma-ray flares in general. We discuss
  the causes and implications of Fermi BTL events, in the framework
  of a potential shift of paradigm on particle acceleration in solar
  flares/CMEs.

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Title: Fast-mode Coronal EUV Wave Trains Associated with Solar Flares
    and CMEs
Authors: Liu, Wei; Ofman, Leon; Downs, Cooper; Karlicky, Marian;
   Chen, Bin
2017SPD....48.0401L    Altcode:
  As a new observational phenomenon, Quasi-periodic, Fast Propagating EUV
  wave trains (QFPs) are fast-mode magnetosonic waves closely related
  to quasi-periodic pulsations commonly detected in solar flares
  (traditionally with non-imaging observations). They can provide
  critical clues to flare energy release and serve as new tools for
  coronal seismology. We report recent advances in observing and modeling
  QFPs, including evidence of heating and cooling cycles revealed with
  differential emission measure (DEM) analysis that are consistent
  with alternating compression and rarefaction expected for magnetosonic
  waves. Through a statistical survey, we found a preferential association
  of QFPs with eruptive flares (with CMEs) rather than confined flares
  (without CMEs). We also identified some correlation with quasi-periodic
  radio bursts observed at JVLA and Ondrejov observatories. We will
  discuss the implications of these results and the potential roles of
  QFPs in coronal heating and energy transport.

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Title: Ten years of SLR production in Argentina
Authors: Pacheco, A.; Podestá, R.; Yin, Z.; Liu, W.; Actis, E.;
   Adarvez, S.; Quinteros, J.; Podestá, F.
2017RMxAC..49..143P    Altcode:
  SLR technique is a proved astro-geodetic art with a significant power
  to contribute to Earth and Space Sciences. Therefore, scientific
  applications of SLR System are able to perform multiple tasks in
  the fields of Astrometry, Geodesy and Geophysics. The results we
  show here were obtained from satellite observations made at SLR 7406
  Station of Observatorio Astronómico Félix Aguilar (OAFA) in San Juan,
  Argentina. The telescope was installed early on 2006, in concordance
  with an International Cooperation Agreement between Universidad
  Nacional de San Juan, Argentina and Chinese Academy of Sciences. In this
  abstract we show the current research being done with ILRS 7406 station:
  Length of day (LOD) and Angular velocity of Earth Rotation, calculated
  weekly; Pole Motion. ILRS7406 is daily surveying Pole coordinates x
  and y; Tracking SLR to GNSS constellations. SLR System contributes
  to the adjustment and validation of satellite GALILEO, GPS, GLONASS,
  and BEIDOU orbits. Our station is nowadays member of the new ITRF 2014
  frame, and these past years has been one of the 3 highest producing SLR
  Stations on the ILRS net, composed of about 40 stations distributed all
  around the world. The obtained results during this first 10 years of
  experience are useful to enhance the traditional collaboration between
  OAFA and international services such as ILRS, IERS and NASA.

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Title: A Model-free CAF Fringe Search Algorithm with Wavelet Boosting
    for VLBI Observation
Authors: Zhang, Tianyi; Meng, Qiao; Chen, Congyan; Zheng, Weimin;
   Liu, Wei; Yu, Quantao; Tong, Li
2017PASP..129g4501Z    Altcode:
  Very-Long-Baseline interferometry (VLBI) is a powerful tool in radio
  astronomy, geodesy, and deep space exploration. Priori predicted delay
  models are needed to make interferometry fringes, but in some cases they
  would be difficult to get. This paper proposes an effective algorithm
  named CAF-W algorithm to search fringes from the raw data in a large
  search range without priori predicted delay models. The cross-ambiguity
  function (CAF) is used to make a time-frequency correlation in the
  delay-delay rate plane. The wavelet boosting algorithm is used to
  eliminate interference and enhance the CAF peak, whose position would
  give the delay and delay rate estimations. Incoherent averaging and
  sliding search window techniques are used to overcome the wide search
  range and the poor signal-to-noise ratio in VLBI observations. The CAF-W
  algorithm could be performed with fast algorithms so the computation
  burden is affordable. This algorithm has successfully achieved VLBI
  fringes from the raw data without priori predicted delay models in
  VLBI observations.

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Title: Double-coronal X-Ray and Microwave Sources Associated with
    a Magnetic Breakout Solar Eruption
Authors: Chen, Yao; Wu, Zhao; Liu, Wei; Schwartz, Richard A.; Zhao,
   Di; Wang, Bing; Du, Guohui
2017ApJ...843....8C    Altcode: 2017arXiv170506074C
  Double-coronal hard X-ray (HXR) sources are believed to be critical
  observational evidence of bi-directional energy release through magnetic
  reconnection in large-scale current sheets in solar flares. Here,
  we present a study on double-coronal sources observed in both HXR
  and microwave regimes, revealing new characteristics distinct from
  earlier reports. This event is associated with a footpoint-occulted
  X1.3-class flare (2014 April 25, starting at 00:17 UT) and a coronal
  mass ejection that were likely triggered by the magnetic breakout
  process, with the lower source extending upward from the top of the
  partially occulted flare loops and the upper source co-incident with
  rapidly squeezing-in side lobes (at a speed of ∼250 km s<SUP>-1</SUP>
  on both sides). The upper source can be identified at energies as high
  as 70-100 keV. The X-ray upper source is characterized by flux curves
  that differ from those of the lower source, a weak energy dependence
  of projected centroid altitude above 20 keV, a shorter duration,
  and an HXR photon spectrum slightly harder than those of the lower
  source. In addition, the microwave emission at 34 GHz also exhibits
  a similar double-source structure and the microwave spectra at both
  sources are in line with gyrosynchrotron emission given by non-thermal
  energetic electrons. These observations, especially the co-incidence of
  the very-fast squeezing-in motion of side lobes and the upper source,
  indicate that the upper source is associated with (and possibly caused
  by) this fast motion of arcades. This sheds new light on the origin of
  the corona double-source structure observed in both HXRs and microwaves.

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Title: Excesses of cosmic ray spectra from a single nearby source
Authors: Liu, Wei; Bi, Xiao-Jun; Lin, Su-Jie; Wang, Bing-Bing; Yin,
   Peng-Fei
2017PhRvD..96b3006L    Altcode: 2016arXiv161109118L
  Growing evidence reveals universal hardening on various cosmic ray
  spectra, e.g., proton, positron, as well as antiproton fractions. Such
  universality may indicate they have a common origin. In this paper, we
  argue that these widespread excesses can be accounted for by a nearby
  supernova remnant surrounded by a giant molecular cloud. Secondary
  cosmic rays (p , e<SUP>+</SUP> ) are produced through the collisions
  between the primary cosmic-ray nuclei from this supernova remnant and
  the molecular gas. Different from the background, which is produced
  by the ensemble of a large number of sources in the Milky Way, the
  local injected spectrum can be harder. The time-dependent transport
  of particles would make the propagated spectrum even harder. Under
  this scenario, the anomalies of both primary (p , e<SUP>-</SUP>)
  and secondary (e<SUP>+</SUP>, p ¯ /p ) cosmic rays can be properly
  interpreted. We further show that the TeV to sub-PeV anisotropy of
  the proton is consistent with the observations if the local source is
  relatively young and lying at the anti-Galactic center direction.

---------------------------------------------------------
Title: Explaining the rolling-pin distribution of suprathermal
    electrons behind dipolarization fronts
Authors: Liu, C. M.; Fu, H. S.; Xu, Y.; Cao, J. B.; Liu, W. L.
2017GeoRL..44.6492L    Altcode:
  The rolling-pin distribution of suprathermal electrons (40-200 keV),
  showing electron pitch angles primarily at 0°, 90°, and 180°,
  has recently been reported behind dipolarization fronts (DFs)
  both in observations and simulations. The formation of such type
  of distribution, however, has been unclear so far. In this study,
  we present an observation of such type of distribution by Cluster
  in the magnetotail behind a DF. We interpret the formation of such
  distribution using the global-scale Fermi acceleration together with
  local-scale betatron acceleration. We quantitatively reproduce these two
  processes and therefore the rolling-pin distribution of suprathermal
  electrons using an analytical model. We further reveal that only at
  energies higher than 26 keV can such distribution be formed. This study,
  quantitatively explaining the formation of rolling-pin distribution,
  can improve the understanding of electron dynamics behind DFs.

---------------------------------------------------------
Title: Constraints on dark matter annihilation and decay from the
    isotropic gamma-ray background
Authors: Liu, Wei; Bi, Xiao-Jun; Lin, Su-Jie; Yin, Peng-Fei
2017ChPhC..41d5104L    Altcode: 2016arXiv160201012L
  We study the constraints on dark matter (DM) annihilation/decay from
  the Fermi-LAT Isotropic Gamma-Ray Background (IGRB) observation. We
  consider the contributions from both extragalactic and galactic
  DM components. For DM annihilation, the evolution of extragalactic
  DM halos is taken into account. We find that the IGRB annihilation
  constraints under some DM subhalo models can be comparable to those
  derived from the observations of dwarf spheroidal galaxies and
  CMB. We also use the IGRB results to constrain the parameter regions
  accounting for the latest AMS-02 electron-positron anomaly. We find
  that the majority of DM annihilation/decay channels are strongly
  disfavored by the latest Fermi-LAT IGRB observation; only DM decays
  to μ<SUP>+</SUP>μ<SUP>-</SUP> and 4μ channels may be valid. <P
  />Supported by National Natural Science Foundation of China (11475189,
  11475191, 11135009), 973 Program of China (2013CB837000), Strategic
  Priority Research Program “The Emergence of Cosmological Structures”
  of the Chinese Academy of Sciences (XDB09000000)

---------------------------------------------------------
Title: Broadband high-frequency waves detected at dipolarization
    fronts
Authors: Yang, J.; Cao, J. B.; Fu, H. S.; Wang, T. Y.; Liu, W. L.;
   Yao, Z. H.
2017JGRA..122.4299Y    Altcode:
  Dipolarization front (DF) is a sharp boundary most probably separating
  the reconnection jet from the background plasma sheet. So far at this
  boundary, the observed waves are mainly in low-frequency range (e.g.,
  magnetosonic waves and lower hybrid waves). Few high-frequency waves
  are observed in this region. In this paper, we report the broadband
  high-frequency wave emissions at the DF. These waves, having frequencies
  extending from the electron cyclotron frequency f<SUB>ce</SUB>, up to
  the electron plasma frequency f<SUB>pe</SUB>, could contribute 10%
  to the in situ measurement of intermittent energy conversion at the
  DF layer. Their generation may be attributed to electron beams, which
  are simultaneously observed at the DF as well.

---------------------------------------------------------
Title: Lunar Water Spatial Distribution and Its Temporal Variations
Authors: Wang, H. Z.; Zhang, J.; Shi, Q. Q.; Tian, A. M.; Chen, J.;
   Liu, J.; Ling, Z. C.; Fu, X. H.; Wei, Y.; Zhang, H.; Liu, W. L.; Fu,
   S. Y.; Zong, Q. G.; Pu, Z. Y.
2017LPI....48.1831W    Altcode:
  We studied spatial distribution and temporal variations of lunar water
  to investigate the influence of the Earth's magnetosphere in the lunar
  surface hydration.

---------------------------------------------------------
Title: Oxidative Alteration of Ferrous Smectites: A Formation Pathway
    for Martian Nontronite?
Authors: Chemtob, S. M.; Catalano, J. G.; Nickerson, R. D.; Morris,
   R. V.; Agresti, D. G.; Rivera-Banuchi, V.; Liu, W.; Yee, N.
2017LPI....48.2520C    Altcode:
  We show experimentally that martian ferric smectites can form by
  oxidation of ferrous smectite precursors, suggesting reducing conditions
  during the Noachian.

---------------------------------------------------------
Title: Hard X-Ray Emission from Partially Occulted Solar Flares:
    RHESSI Observations in Two Solar Cycles
Authors: Effenberger, Frederic; Rubio da Costa, Fatima; Oka, Mitsuo;
   Saint-Hilaire, Pascal; Liu, Wei; Petrosian, Vahé; Glesener, Lindsay;
   Krucker, Säm
2017ApJ...835..124E    Altcode: 2016arXiv161202856E
  Flares close to the solar limb, where the footpoints are occulted,
  can reveal the spectrum and structure of the coronal looptop source
  in X-rays. We aim at studying the properties of the corresponding
  energetic electrons near their acceleration site, without footpoint
  contamination. To this end, a statistical study of partially occulted
  flares observed with Reuven Ramaty High-Energy Solar Spectroscopic
  Imager is presented here, covering a large part of solar cycles
  23 and 24. We perform detailed spectra, imaging, and light curve
  analyses for 116 flares and include contextual observations from
  SDO and STEREO when available, providing further insights into flare
  emission that were previously not accessible. We find that most spectra
  are fitted well with a thermal component plus a broken power-law,
  non-thermal component. A thin-target kappa distribution model gives
  satisfactory fits after the addition of a thermal component. X-ray
  imaging reveals small spatial separation between the thermal and
  non-thermal components, except for a few flares with a richer coronal
  source structure. A comprehensive light curve analysis shows a very good
  correlation between the derivative of the soft X-ray flux (from GOES)
  and the hard X-rays for a substantial number of flares, indicative of
  the Neupert effect. The results confirm that non-thermal particles
  are accelerated in the corona and estimated timescales support the
  validity of a thin-target scenario with similar magnitudes of thermal
  and non-thermal energy fluxes.

---------------------------------------------------------
Title: Fermi-LAT Observations of High-energy Behind-the-limb Solar
    Flares
Authors: Ackermann, M.; Allafort, A.; Baldini, L.; Barbiellini, G.;
   Bastieri, D.; Bellazzini, R.; Bissaldi, E.; Bonino, R.; Bottacini, E.;
   Bregeon, J.; Bruel, P.; Buehler, R.; Cameron, R. A.; Caragiulo, M.;
   Caraveo, P. A.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Ciprini, S.;
   Costanza, F.; Cutini, S.; D'Ammando, F.; de Palma, F.; Desiante, R.;
   Digel, S. W.; Di Lalla, N.; Di Mauro, M.; Di Venere, L.; Drell, P. S.;
   Favuzzi, C.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Giglietto, N.;
   Giordano, F.; Giroletti, M.; Grenier, I. A.; Guillemot, L.; Guiriec,
   S.; Jogler, T.; Jóhannesson, G.; Kashapova, L.; Krucker, S.; Kuss,
   M.; La Mura, G.; Larsson, S.; Latronico, L.; Li, J.; Liu, W.; Longo,
   F.; Loparco, F.; Lubrano, P.; Magill, J. D.; Maldera, S.; Manfreda,
   A.; Mazziotta, M. N.; Mitthumsiri, W.; Mizuno, T.; Monzani, M. E.;
   Morselli, A.; Moskalenko, I. V.; Negro, M.; Nuss, E.; Ohsugi, T.;
   Omodei, N.; Orlando, E.; Pal'shin, V.; Paneque, D.; Perkins, J. S.;
   Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Principe, G.; Rainò,
   S.; Rando, R.; Razzano, M.; Reimer, O.; Rubio da Costa, F.; Sgrò,
   C.; Simone, D.; Siskind, E. J.; Spada, F.; Spandre, G.; Spinelli,
   P.; Tajima, H.; Thayer, J. B.; Torres, D. F.; Troja, E.; Vianello, G.
2017ApJ...835..219A    Altcode: 2017arXiv170200577A
  We report on the Fermi-LAT detection of high-energy emission from the
  behind-the-limb (BTL) solar flares that occurred on 2013 October 11,
  and 2014 January 6 and September 1. The Fermi-LAT observations are
  associated with flares from active regions originating behind both
  the eastern and western limbs, as determined by STEREO. All three
  flares are associated with very fast coronal mass ejections (CMEs)
  and strong solar energetic particle events. We present updated
  localizations of the &gt;100 MeV photon emission, hard X-ray (HXR)
  and EUV images, and broadband spectra from 10 keV to 10 GeV, as well
  as microwave spectra. We also provide a comparison of the BTL flares
  detected by Fermi-LAT with three on-disk flares and present a study
  of some of the significant quantities of these flares as an attempt
  to better understand the acceleration mechanisms at work during these
  occulted flares. We interpret the HXR emission to be due to electron
  bremsstrahlung from a coronal thin-target loop top with the accelerated
  electron spectra steepening at semirelativistic energies. The &gt;100
  MeV gamma-rays are best described by a pion-decay model resulting
  from the interaction of protons (and other ions) in a thick-target
  photospheric source. The protons are believed to have been accelerated
  (to energies &gt;10 GeV) in the CME environment and precipitate down to
  the photosphere from the downstream side of the CME shock and landed
  on the front side of the Sun, away from the original flare site and
  the HXR emission.

---------------------------------------------------------
Title: Enhancement of oxygen in the magnetic island associated with
    dipolarization fronts
Authors: Wang, J.; Cao, J. B.; Fu, H. S.; Liu, W. L.; Lu, S.
2017JGRA..122..185W    Altcode:
  A significant enhancement of O<SUP>+</SUP> is observed by Cluster inside
  an earthward propagating magnetic island behind a dipolarization front
  (DF). Such enhancement, from 0.005 to 0.03 cm<SUP>-3</SUP>, makes the
  O<SUP>+</SUP> flux inside the magnetic island 20 times larger than that
  outside the magnetic island. In the meantime, the H<SUP>+</SUP> density
  is nearly a constant, 0.1 cm<SUP>-3</SUP>, during the magnetic-island
  encounter. This results in a dramatic increase of the density ratio,
  nO&lt;mo form="prefix"&gt;+&gt;/nH&lt;mo form="prefix"&gt;+, from
  0.05 to 0.3 (about 10 times as large as the average value in the
  plasma sheet) and a dramatic decrease of the local Alfvén speed from
  V<SUB>A</SUB> ≈ 770 km/s to V<SUB>A</SUB> ≈ 430 km/s inside the
  magnetic island. The decrease of Alfvén speed indicates an asymmetric
  reconnection and a slow magnetic reconnection rate near the secondary X
  line. Since the reconnection rates at the primary X line and secondary
  X line are imbalanced, the DFs and magnetic islands are pushed to
  propagate earthward by the outflow of the primary reconnection, as
  demonstrated in recent simulations.

---------------------------------------------------------
Title: Fermi Large Area Telescope Observations of High-Energy
    Gamma-ray Emission From Behind-the-limb Solar Flares
Authors: Omodei, Nicola; Pesce-Rollins, Melissa; Petrosian, Vahe;
   Liu, Wei; Rubio da Costa, Fatima; Golenetskii, Sergei; Kashapova,
   Larisa; Krucker, Sam; Palshin, Valentin; Fermi Large Area Telescope
   Collaboration
2017APS..APR.Y3005O    Altcode:
  Fermi LAT &gt;30 MeV observations of the active Sun have increased
  the number of detected solar flares by almost a factor of 10 with
  respect to previous space observations. Of particular interest are the
  recent detections of three solar flares whose position behind the limb
  was confirmed by the STEREO-B spacecraft. These observations sample
  flares from active regions originating from behind both the eastern
  and western limbs and include an event associated with the second
  ground level enhancement event (GLE) of the 24th Solar Cycle. While
  gamma-ray emission up to tens of MeV resulting from proton interactions
  has been detected before from occulted solar flares, the significance
  of these particular events lies in the fact that these are the first
  detections of &gt;100 MeV gamma-ray emission from footpoint-occulted
  flares. These detections present an unique opportunity to diagnose
  the mechanisms of high-energy emission and particle acceleration and
  transport in solar flares. We will present the Fermi-LAT, RHESSI and
  STEREO observations of these flares and discuss the various emission
  scenarios for these sources.

---------------------------------------------------------
Title: The Structure of the Local Hot Bubble
Authors: Liu, W.; Chiao, M.; Collier, M. R.; Cravens, T.; Galeazzi, M.;
   Koutroumpa, D.; Kuntz, K. D.; Lallement, R.; Lepri, S. T.; McCammon,
   D.; Morgan, K.; Porter, F. S.; Snowden, S. L.; Thomas, N. E.; Uprety,
   Y.; Ursino, E.; Walsh, B. M.
2017ApJ...834...33L    Altcode: 2016arXiv161105133L
  Diffuse X-rays from the Local Galaxy (DXL) is a sounding rocket mission
  designed to quantify and characterize the contribution of Solar Wind
  Charge eXchange (SWCX) to the Diffuse X-ray Background and study the
  properties of the Local Hot Bubble (LHB). Based on the results from
  the DXL mission, we quantified and removed the contribution of SWCX to
  the diffuse X-ray background measured by the ROSAT All Sky Survey. The
  “cleaned” maps were used to investigate the physical properties of
  the LHB. Assuming thermal ionization equilibrium, we measured a highly
  uniform temperature distributed around kT = 0.097 keV ± 0.013 keV
  (FWHM) ± 0.006 keV (systematic). We also generated a thermal emission
  measure map and used it to characterize the three-dimensional (3D)
  structure of the LHB, which we found to be in good agreement with the
  structure of the local cavity measured from dust and gas.

---------------------------------------------------------
Title: Underground Nuclear Astrophysics Experiment JUNA in China
Authors: Liu, W. P.
2017nuco.confa1101L    Altcode:
  Underground Nuclear Astrophysics Experiment in China (JUNA) will take
  the advantage of the ultra-low background in Jinping underground
  lab. A 400 kV high current accelerator with an ECR source and γ ,
  neutron and charged particle detectors will be set up. We plan to study
  directly a number of nuclear reactions important to hydrostatic stellar
  evolution near their Gamow window energies such as <SUP>25</SUP>Mg(p,
  γ )<SUP>26</SUP>Al, <SUP>19</SUP>F(p, α )<SUP>16</SUP>O,
  <SUP>13</SUP>C(α , n)<SUP>16</SUP>O, and <SUP>12</SUP>C(α , γ
  )<SUP>16</SUP>O, by the end of 2019.

---------------------------------------------------------
Title: Hard X-Ray Observations of Coronal Sources: Implications for
    Particle Acceleration
Authors: Effenberger, F.; Rubio da Costa, F.; Oka, M.; Saint-Hilaire,
   P.; Liu, W.; Krucker, S.; Glesener, L.; Petrosian, V.
2016AGUFMSH51E2634E    Altcode:
  The properties of hard X-ray emission from solar flares can provide
  insight into particle acceleration and transport processes. Commonly,
  at higher energies the bright footpoint emission from the flare loop
  prevents a detailed analysis of the weaker loop-top source due to
  the limited dynamic range. Thus, flares close to the solar limb,
  where the footpoints are occulted, are interesting events to study
  because they can reveal the coronal loop-top emission and thus the
  electron properties at their acceleration site. We present results of
  a survey study of partially occulted flares observed with the Reuven
  Ramaty High-Energy Solar Spectroscopic Imager (RHESSI). We found that
  most of the flare spectra allow a fit to a thermal plus non-thermal
  component, either with a broken power-law or a kappa function. The
  spatial separation between the thermal and non-thermal component,
  as derived from imaging, is usually small. The light curve analysis
  shows for many flares a very good correlation between the derivative
  of the soft X-ray flux and the hard X-rays. We discuss implications
  for particle acceleration models that result from our study.

---------------------------------------------------------
Title: High resolution observations of prominence rotation by Hinode
    and IRIS
Authors: Okamoto, J.; Liu, W.; Tsuneta, S.
2016AGUFMSH41E..05O    Altcode:
  Fine structures of prominences, especially threads, and their dynamics
  provide physical information about the magnetic configuration and
  property in the corona. Here we report two events of prominence rotation
  observed by the Hinode and IRIS satellites. In the first event, we found
  transverse motions of brightening threads at speeds up to 55 km/s seen
  in the plane of the sky. Such motions appeared as sinusoidal space-time
  trajectories with a typical period of 390 s, which is consistent
  with plane-of-sky projections of rotational motions. At least 15
  episodes of such motions occurred in two days, none associated with
  any eruption. For these episodes, the plane-of-sky speed is linearly
  correlated with the vertical travel distance, suggestive of a constant
  angular speed. In the second event, spectral data taken by IRIS showed
  strong blueshifts in the top portion of the prominence with a speed
  of 30-40 km/s, while redshifts of similar speeds were detected at the
  bottom. Line width of the bright threads were significantly larger
  than those of stationary threads. These behaviors indicate rotations of
  helical prominence threads. We interpreted the activations as evidence
  of unwinding motions caused by magnetic reconnection between twisted
  prominence fields and ambient coronal fields.

---------------------------------------------------------
Title: Particle Acceleration in High-Energy Solar Flares Detected
    by the Fermi Large Area Telescope
Authors: Omodei, N.; Pesce-Rollins, M.; Petrosian, V.; Liu, W.;
   Rubio da Costa, F.
2016AGUFMSH41D..02O    Altcode:
  The Fermi Large Area Telescope (LAT) is the most sensitive instrument
  ever deployed in space for observing gamma-ray emission above 100
  MeV. LAT observations of the active Sun have increased the number of
  detected solar flares by almost a factor of 10 with respect to previous
  space observations. We will present an overview of these observations,
  which include detections of impulsive and sustained emission, extending
  up to 20 hours in the case of the X-class flare occurred on 2012
  March 7. Of particular interest is the first detection of &gt;100 MeV
  gamma-ray emission from three solar flares whose positions behind the
  limb were confirmed by the STEREO spacecrafts. These observations sample
  flares from active regions originating from behind both the eastern
  and western limbs and present a unique opportunity to diagnose the
  mechanisms of high-energy emission and particle acceleration in solar
  flares. We will present the Fermi-LAT, RHESSI and STEREO observations
  of these flares and discuss how these observations provide constrains
  on different emission mechanisms.

---------------------------------------------------------
Title: Observations and Modeling of Plasma Waves in the Solar
    Atmosphere
Authors: Liu, W.; Ofman, L.; Downs, C.
2016AGUFMSH14B..01L    Altcode:
  The solar atmosphere, especially the extended corona, provides rich
  observations of magnetohydrodynamic (MHD) waves and plasma waves in
  general. Such waves can be used as seismological tools to probe the
  physical conditions of the medium in which they travel, such as the
  coronal magnetic field and plasma parameters. Recent high-resolution
  imaging and spectroscopic observations in extreme ultraviolet (EUV)
  by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics
  Observatory (SDO) and in UV by the Interface Region Imaging Spectrograph
  (IRIS) have opened a new chapter in understanding these waves and
  in utilizing them for coronal seismology. We will review such new
  observations of two intimately related phenomena - global EUV waves
  (so-called "EIT waves") associated with coronal mass ejections (CMEs)
  and quasi-periodic, fast-mode magnetosonic wave trains associated with
  flares. We will focus on the generation and propagation of global
  EUV waves and their interaction with coronal structures, as well
  as the correlation of AIA-detected fast-mode wave trains with flare
  pulsations seen from radio to hard X-ray wavelengths. We will also
  present recent MHD modeling efforts in reproducing these waves using
  realistic, observationally-driven simulations. We will discuss the
  roles of such waves in energy transport within the solar atmosphere
  and in their associated CME/flare eruptions.

---------------------------------------------------------
Title: Prompt GPS TEC Response to Magnetospheric Compression by
    Interplanetary Shock
Authors: Hao, Y.; Liu, W. L.; Huang, J.; Zhang, D.; Xiao, Z.
2016AGUFMSM13B2201H    Altcode:
  A new type of total electron content (TEC) variation was observed in
  prompt response to an interplanetary shock (IS) impact on the Earth's
  magnetosphere. With hundreds of ground-based global positioning system
  (GPS) receivers, simultaneous TEC impulses with amplitudes as large
  as 0.3 TECU were detected in the signals of GPS satellites which were
  cruising in the dayside equatorial magnetosphere. We suggest that the
  TEC impulses result from shock-induced magnetospheric compression,
  which drives plasma to move earthward via perturbed electric field
  in the dayside magnetosphere. The observed TEC increase reflects the
  radial motion of plasma from outside of the GPS orbit (4.2 RE) to
  inside, showing an unprecedented ability of the GPS TEC technique to
  capture small tremor of the magnetosphere and, with the dense receiver
  network it can be a useful tool for investigating the plasma dynamics
  around 4.2 RE.

---------------------------------------------------------
Title: Curvature of the spectral energy distribution, the inverse
    Compton component and the jet in Fermi 2LAC blazars
Authors: Xue, R.; Luo, D.; Du, L. M.; Wang, Z. R.; Xie, Z. H.; Yi,
   T. F.; Xiong, D. R.; Xu, Y. B.; Liu, W. G.; Yu, X. L.
2016MNRAS.463.3038X    Altcode: 2016arXiv160905697X
  We fitted the spectral energy distributions (SEDs) of members of a
  large sample of Fermi 2LAC blazars to synchrotron and inverse Compton
  (IC) models. Our main results are as follows. (I) As suggested
  by previous works, the correlation between the peak frequency and
  curvature can be explained by statistical or stochastic particle
  acceleration mechanisms. For BL Lacs, we found a linear correlation
  between the synchrotron peak frequency and its curvature. The slope of
  the correlation is consistent with stochastic acceleration mechanisms
  and confirms the results of previous studies. For flat-spectrum radio
  quasars (FSRQs), we also found a linear correlation, but in this case
  the slope cannot be explained by previous theoretical models. (II) We
  found a significant correlation between IC luminosity and synchrotron
  luminosity. The slope of the correlation for FSRQs is consistent
  with the external Compton (EC) process. The slope of the correlation
  for BL Lacs is consistent with the synchrotron self-Compton (SSC)
  process. (III) We found several significant correlations between IC
  curvature and various basic parameters of blazars (black hole mass,
  broad-line luminosity, the Lorentz factor of the jet). We also found
  significant correlations between the bolometric luminosity and these
  basic parameters of blazars, which suggests that the origin of jets
  is a mixture of the mechanisms proposed by Blandford &amp; Znajek and
  by Blandford &amp; Payne.

---------------------------------------------------------
Title: The Contribution of Geomagnetic Activities to Polar Ozone
    Changes in Upper Atmosphere
Authors: Huang, C.; Huang, F.; Zhang, X.; Liu, D.; Hao, Y.; Liu, W. L.
2016AGUFMSM22A..08H    Altcode:
  Energetic particle precipitation (EPP) plays an important role in
  the catalytic process of ozone depletion due to the odd nitrogen and
  odd hydrogen species produced by EPP in the polar middle atmosphere
  during the geomagnetic activities. It is known that solar UV emission
  variations have significant effects on ozone generation. So it
  is interesting to compare the contributions of EPP and solar UV
  emission to ozone change in the polar upper atmosphere. In this work,
  we applied annual average Ap index to denote the annual mean magnitude
  of geomagnetic activity which has good relationship with EPP flux and
  annual average F10.7 index to denote annual mean magnitude of solar
  radiation which has certain relevancy with solar UV emission. We adopted
  latitude-average dataset of ozone measurements from SBUV instruments
  on the POES satellites and studied the statistics characters between
  ozone dataset and Ap,F10.7 index. The multiple regression analysis shows
  that the contributions of geomagnetic activities are not negligible and
  have the similar order of magnitude compared with solar UV emission
  in polar upper atmosphere (above 30 km). The results also show that
  HSSWS-Induced (HSSWS, High-Speed Solar Wind Stream) geomagnetic
  activities and that of CME-Induced (CME, Coronal Mass Ejection) are
  of the same order of magnitude. There exists differences between two
  hemispheres according to the multiple regression analysis and we made
  a discussion to interpret the causes of these differences.

---------------------------------------------------------
Title: Calculation of electric radial diffusion coefficient of
    radiation belt electrons with in situ electric field measurements
    by THEMIS
Authors: Liu, W.; Tu, W.; Li, X.; Sarris, T. E.; Khotyaintsev, Y. V.;
   Fu, H.; Zhang, H.; Shi, Q.
2016AGUFMSM22B..03L    Altcode:
  Based on seven years' observations from THEMIS, we investigate the
  statistical distribution of electric field Pc5 ULF wave power under
  different geomagnetic activities and calculate the radial diffusion
  coefficient due to electric field, DLLE, for outer radiation belt
  electrons. A simple empirical expression of DLLE[THEMIS] is also
  derived. Subsequently we compare DLLE[THEMIS] to previous DLL models,
  and find similar Kp dependence with the DLLE[CRRES] model, which is
  also based on in-situ electric field measurements. The absolute value of
  DLLE[THEMIS] is constantly higher than DLLE[CRRES], probably due to the
  limited orbital coverage of CRRES. The differences between DLLE[THEMIS]
  and the commonly-used DLLM[B-A] and DLLE[Ozeke] models are significant,
  especially in Kp dependence and energy dependence. Possible reasons for
  these differences and their implications are discussed. The diffusion
  coefficient provided in this paper, which also has energy dependence,
  will be an important contributor to quantify the radial diffusion
  process of radiation belt electrons.

---------------------------------------------------------
Title: Probing the Physical Connection between Solar Prominences
    and Coronal Rain
Authors: Liu, W.; Antolin, P.; Sun, X.; Vial, J. C.; Guo, L.; Gibson,
   S. E.; Berger, T. E.; Okamoto, J.; De Pontieu, B.
2016AGUFMSH43C2587L    Altcode:
  Solar prominences and coronal rain are intimately related phenomena,
  both involving cool material at chromospheric temperatures within the
  hot corona and both playing important roles as part of the return flow
  of the chromosphere-corona mass cycle. At the same time, they exhibit
  distinct morphologies and dynamics not yet well understood. Quiescent
  prominences consist of numerous long-lasting, filamentary downflow
  threads, while coronal rain is more transient and falls comparably
  faster along well-defined curved paths. We report here a novel, hybrid
  prominence-coronal rain complex in an arcade-fan geometry observed
  by SDO/AIA and IRIS, which provides new insights to the underlying
  physics of such contrasting behaviors. We found that the supra-arcade
  fan region hosts a prominence sheet consisting of meandering threads
  with broad line widths. As the prominence material descends to the
  arcade, it turns into coronal rain sliding down coronal loops with
  line widths 2-3 times narrower. This contrast suggests that distinct
  local plasma and magnetic conditions determine the fate of the cool
  material, a scenario supported by our magnetic field extrapolations
  from SDO/HMI. Specifically, the supra-arcade fan (similar to those
  in solar flares) is likely situated in a current sheet, where the
  magnetic field is weak and the plasma-beta could be close to unity, thus
  favoring turbulent flows like those prominence threads. In contrast,
  the underlying arcade has a stronger magnetic field and most likely a
  low-beta environment, such that the material is guided along magnetic
  field lines to appear as coronal rain. We will discuss the physical
  implications of these observations beyond the phenomena of prominences
  and coronal rain.

---------------------------------------------------------
Title: Observations of the Motion of X Line on the Dayside
    Magnetopause
Authors: Zhu, C.; Zhang, H.; Ge, Y.; Pu, Z.; Liu, L.; Wan, W.; Liu,
   W. L.; Chen, Y.; Le, H.
2016AGUFMSM21A2425Z    Altcode:
  Various observations from satellites have shown that reconnection X line
  should be stable at a fixed position at low latitude of magnetosphere
  during stable southward IMF conditions. On the contrary, there are also
  events demonstrated that reconnection X line can move, which is rare
  but particular important. The direction of the motion of X line has
  been presumed along the electron diamagnetic drift direction on the
  dayside magnetopause. However, we discovered a case that the X line
  moved in the ion diamagnetic drift direction, which is opposite to
  electron diamagnetic direction. The result is reasonable because the
  fluid velocity that convect field lines is mainly determined by ions'
  velocity instead of electrons' velocity, thus the direction of the
  motion of X line is decided by ions. We analyzed the event of single
  X line crossing Cluster 1 and Cluster 3 satellites sequentially on
  the magnetopause, and found that the direction of the moving X line
  is in the ion diamagnetic drift and the magnitude of that is the sum
  of the ion and electron diamagnetic drift in the electron rest frame.

---------------------------------------------------------
Title: Slipping reconnection in a solar flare observed in high
    resolution with the GREGOR solar telescope
Authors: Sobotka, M.; Dudík, J.; Denker, C.; Balthasar, H.; Jurčák,
   J.; Liu, W.; Berkefeld, T.; Collados Vera, M.; Feller, A.; Hofmann,
   A.; Kneer, F.; Kuckein, C.; Lagg, A.; Louis, R. E.; von der Lühe, O.;
   Nicklas, H.; Schlichenmaier, R.; Schmidt, D.; Schmidt, W.; Sigwarth,
   M.; Solanki, S. K.; Soltau, D.; Staude, J.; Strassmeier, K. G.;
   Volkmer, R.; Waldmann, T.
2016A&A...596A...1S    Altcode: 2016arXiv160500464S
  A small flare ribbon above a sunspot umbra in active region 12205 was
  observed on November 7, 2014, at 12:00 UT in the blue imaging channel
  of the 1.5 m GREGOR telescope, using a 1 Å Ca II H interference
  filter. Context observations from the Atmospheric Imaging Assembly
  (AIA) onboard the Solar Dynamics Observatory (SDO), the Solar Optical
  Telescope (SOT) onboard Hinode, and the Interface Region Imaging
  Spectrograph (IRIS) show that this ribbon is part of a larger one
  that extends through the neighboring positive polarities and also
  participates in several other flares within the active region. We
  reconstructed a time series of 140 s of Ca II H images by means of the
  multiframe blind deconvolution method, which resulted in spatial and
  temporal resolutions of 0.1″ and 1 s. Light curves and horizontal
  velocities of small-scale bright knots in the observed flare ribbon
  were measured. Some knots are stationary, but three move along the
  ribbon with speeds of 7-11 km s<SUP>-1</SUP>. Two of them move in the
  opposite direction and exhibit highly correlated intensity changes,
  which provides evidence of a slipping reconnection at small spatial
  scales. <P />Movies associated to Figs. 1 and 2 are available at <A
  href="http://www.aanda.org/10.1051/0004-6361/201527966/olm">http://www.aanda.org</A>

---------------------------------------------------------
Title: Physics of higher orbital bands in optical lattices: a review
Authors: Li, Xiaopeng; Liu, W. Vincent
2016RPPh...79k6401L    Altcode: 2015arXiv150806285L
  The orbital degree of freedom plays a fundamental role in understanding
  the unconventional properties in solid state materials. Experimental
  progress in quantum atomic gases has demonstrated that high orbitals
  in optical lattices can be used to construct quantum emulators of
  exotic models beyond natural crystals, where novel many-body states
  such as complex Bose-Einstein condensates and topological semimetals
  emerge. A brief introduction of orbital degrees of freedom in optical
  lattices is given and a summary of exotic orbital models and resulting
  many-body phases is provided. Experimental consequences of the novel
  phases are also discussed.

---------------------------------------------------------
Title: Helical Motions of Fine-structure Prominence Threads Observed
    by Hinode and IRIS
Authors: Okamoto, Takenori J.; Liu, Wei; Tsuneta, Saku
2016ApJ...831..126O    Altcode: 2016arXiv160800123O
  Fine-structure dynamics in solar prominences holds critical clues
  to understanding their physical nature of significant space-weather
  implications. We report evidence of rotational motions of horizontal
  helical threads in two active-region prominences observed by the
  Hinode and/or Interface Region Imaging Spectrograph satellites at
  high resolution. In the first event, we found transverse motions
  of brightening threads at speeds up to 55 km s<SUP>-1</SUP> seen in
  the plane of the sky. Such motions appeared as sinusoidal space-time
  trajectories with a typical period of ∼390 s, which is consistent
  with plane-of-sky projections of rotational motions. Phase delays at
  different locations suggest the propagation of twists along the threads
  at phase speeds of 90-270 km s<SUP>-1</SUP>. At least 15 episodes of
  such motions occurred in two days, none associated with an eruption. For
  these episodes, the plane-of-sky speed is linearly correlated with the
  vertical travel distance, suggestive of a constant angular speed. In the
  second event, we found Doppler velocities of 30-40 km s<SUP>-1</SUP> in
  opposite directions in the top and bottom portions of the prominence,
  comparable to the plane-of-sky speed. The moving threads have about
  twice broader line widths than stationary threads. These observations,
  when taken together, provide strong evidence for rotations of helical
  prominence threads, which were likely driven by unwinding twists
  triggered by magnetic reconnection between twisted prominence magnetic
  fields and ambient coronal fields.

---------------------------------------------------------
Title: Alfvén wings in the lunar wake: The role of pressure gradients
Authors: Zhang, H.; Khurana, K. K.; Kivelson, M. G.; Fatemi, S.;
   Holmström, M.; Angelopoulos, V.; Jia, Y. D.; Wan, W. X.; Liu, L. B.;
   Chen, Y. D.; Le, H. J.; Shi, Q. Q.; Liu, W. L.
2016JGRA..12110698Z    Altcode:
  Strongly conducting or magnetized obstacles in a flowing plasma generate
  structures called Alfvén wings, which mediate momentum transfer between
  the obstacle and the plasma. Nonconducting obstacles such as airless
  planetary bodies can generate such structures, which, however, have so
  far been seen only in sub-Alfvénic regime. A novel statistical analysis
  of simultaneous measurements made by two ARTEMIS satellites, one in
  the solar wind upstream of the Moon and one in the downstream wake, and
  comparison of the data with results of a three-dimensional hybrid model
  of the interaction reveal that the perturbed plasma downstream of the
  Moon generates Alfvén wings in super-Alfvénic solar wind. In the wake
  region, magnetic field lines bulge toward the Moon and the plasma flows
  are significantly perturbed. We use the simulation to show that some of
  the observed bends of the field result from field-aligned currents. The
  perturbations in the wake thus arise from a combination of compressional
  and Alfvénic perturbations. Because of the super-Alfvénic background
  flow of the solar wind, the two Alfvén wings fold back to form a small
  intersection angle. The currents that form the Alfvén wing in the wake
  are driven by both plasma flow deceleration and a gradient of plasma
  pressure, positive down the wake from the region just downstream of
  the Moon. Such Alfvén wing structures, caused by pressure gradients
  in the wake and the resulting plasma slowdown, should exist downstream
  of any nonconducting body in a super-Alfvénic plasma flow.

---------------------------------------------------------
Title: On the White Dwarf Mass Problem of Cataclysmic Variables
Authors: Liu, Wei-Min; Li, Xiang-Dong
2016ApJ...832...80L    Altcode: 2016arXiv160906940L
  Recent observations show that white dwarfs (WDs) in cataclysmic
  variables (CVs) have an average mass significantly higher than
  isolated WDs and WDs in post-common envelope binaries (PCEBs),
  which are thought to be the progenitors of CVs. This suggests that
  either the WDs have grown in mass during the PCEB/CV evolution or
  the binaries with low-mass WDs are unable to evolve to be CVs. In
  this paper, we calculate the evolution of accreting WD binaries with
  updated hydrogen accumulation efficiency and angular momentum loss
  (AML) prescriptions. We show that thermal-timescale mass transfer is
  not effective in changing the average WD mass distribution. The WD
  mass discrepancy is most likely related to unstable mass transfer in
  WD binaries, in which an efficient mechanism of AML is required.

---------------------------------------------------------
Title: Optical design study of the Wide Field Survey Telescope (WFST)
Authors: Lou, Zheng; Liang, Ming; Yao, Dazhi; Zheng, Xianzhong; Cheng,
   Jingquan; Wang, Hairen; Liu, Wei; Qian, Yuan; Zhao, Haibin; Yang, Ji
2016SPIE10154E..2AL    Altcode:
  WFST is a proposed 2.5m wide field survey telescope intended for
  dedicated wide field sciences. The telescope is to operate at
  six wavelength bands (u, g, r, i, z, and w), spanning from 320
  to 1028 nm. Designed with a field of view diameter of 3 degree
  and an effective aperture diameter of 2.29 m, the WFST acquires a
  total optical throughput over 29.3 m2deg<SUP>2</SUP>. With such a
  large throughput, WFST will survey up to 6000deg<SUP>2</SUP> of the
  northern sky in multiple colors each night, reaching 23th magnitude
  for high-precision photometry and astrometry. The optical design is
  based on an advanced primary-focus system made up of a 2.5 m f/2.48
  concave primary mirror and a primary-focus assembly (PFA) consisting of
  five corrector lenses, atmospheric dispersion corrector (ADC), filters,
  and the focal-plane instrument. For zenith angles from 0 to 60 degrees,
  80% of the polychromatic diffracted energy falls within a 0.35 arcsec
  diameter. The optical design also highlights an enhanced transmission in
  the UV bands. The total optical transmission reaches 23.5% at 320 nm,
  allowing unique science goals in the U band. Other features include
  low distortion and ease of baffling against stray lights, etc. The
  focal-plane instrument is a 0.9 gigapixel mosaic CCD camera comprising
  9 pieces of 10K×10K CCD chips. An active optics system (AOS) is used
  to maintain runtime image quality. Various design aspects of the WFST
  including the optical design, active optics, mirror supports, and the
  focal-plane instrument are discussed in detail.

---------------------------------------------------------
Title: Flare-associated Fast-mode Coronal Wave Trains Detected by
SDO/AIA: Recent Observational Advances
Authors: Liu, Wei; Ofman, Leon; Downs, Cooper; Cheung, Mark; De
   Pontieu, Bart
2016usc..confE.107L    Altcode:
  Quasi-periodic Fast Propagating wave trains (QFPs) are new observational
  phenomena discovered by SDO/AIA in extreme ultraviolet (EUV). They
  were interpreted as fast-mode magnetosonic waves using MHD modeling,
  and also found to be closely related to quasi-periodic pulsations
  in solar flare emission ranging from radio to X-ray wavelengths. The
  significance of QFPs lies in their diagnostic potential (and possibly
  in flare energy transport), because they can provide critical clues to
  flare energy release and serve as new tools for coronal seismology. In
  this presentation, we report recent advances in observing QFPs. In
  particular, using differential emission measure (DEM) inversion,
  we found clear evidence of heating and cooling cycles that are
  consistent with alternating compression and rarefaction expected for
  magnetosonic wave pulses. We also found that different local magnetic
  and plasma environments can lead to two distinct types of QFPs located
  in different spatial domains with respect to their accompanying coronal
  mass ejections (CMEs). More interestingly, from a statistical survey of
  over 100 QFP events, we found a preferential association with eruptive
  flares rather than confined flares. We will discuss the implications
  of these results and the potential roles of QFPs in coronal heating,
  energy transport, and solar eruptions.

---------------------------------------------------------
Title: Joint SDO and IRIS Observations of a Novel, Hybrid
    Prominence-Coronal Rain Complex
Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Gao, Lijia; Vial,
   Jean-Claude; Gibson, Sarah; Okamoto, Takenori; Berger, Thomas;
   Uitenbroek, Han; De Pontieu, Bart
2016usc..confE..99L    Altcode:
  Solar prominences and coronal rain are intimately related phenomena,
  both involving cool material at chromospheric temperatures within the
  hot corona and both playing important roles as part of the return flow
  of the chromosphere-corona mass cycle. At the same time, they exhibit
  distinct morphologies and dynamics not yet well understood. Quiescent
  prominences consist of numerous long-lasting, filamentary downflow
  threads, while coronal rain is more transient and falls comparably
  faster along well-defined curved paths. We report here a novel, hybrid
  prominence-coronal rain complex in an arcade-fan geometry observed
  by SDO/AIA and IRIS, which provides new insights to the underlying
  physics of such contrasting behaviors. We found that the supra-arcade
  fan region hosts a prominence sheet consisting of meandering threads
  with broad line widths. As the prominence material descends to the
  arcade, it turns into coronal rain sliding down coronal loops with
  line widths 2-3 times narrower. This contrast suggests that distinct
  local plasma and magnetic conditions determine the fate of the cool
  material, a scenario supported by our magnetic field extrapolations
  from SDO/HMI. Specifically, the supra-arcade fan (similar to those
  in solar flares; e.g., McKenzie 2013) is likely situated in a current
  sheet, where the magnetic field is weak and the plasma-beta could be
  close to unity, thus favoring turbulent flows like those prominence
  threads. In contrast, the underlying arcade has a stronger magnetic
  field and most likely a low-beta environment, such that the material
  is guided along magnetic field lines to appear as coronal rain. We
  will discuss the physical implications of these observations beyond
  prominence and coronal rain.

---------------------------------------------------------
Title: Solar Wind Charge Exchange Contribution to the ROSAT All Sky
    Survey Maps
Authors: Uprety, Y.; Chiao, M.; Collier, M. R.; Cravens, T.; Galeazzi,
   M.; Koutroumpa, D.; Kuntz, K. D.; Lallement, R.; Lepri, S. T.; Liu,
   W.; McCammon, D.; Morgan, K.; Porter, F. S.; Prasai, K.; Snowden,
   S. L.; Thomas, N. E.; Ursino, E.; Walsh, B. M.
2016ApJ...829...83U    Altcode: 2016arXiv160303447U
  DXL (Diffuse X-ray emission from the Local Galaxy) is a sounding
  rocket mission designed to estimate the contribution of solar wind
  charge eXchange (SWCX) to the diffuse X-ray background and to help
  determine the properties of the Local Hot Bubble. The detectors are
  large area thin-window proportional counters with a spectral response
  that is similar to that of the PSPC used in the ROSAT All Sky Survey
  (RASS). A direct comparison of DXL and RASS data for the same part of
  the sky viewed from quite different vantage points in the solar system,
  and the assumption of approximate isotropy for the solar wind, allowed
  us to quantify the SWCX contribution to all six RASS bands (R1-R7,
  excluding R3). We find that the SWCX contribution at l=140^\circ
  ,b=0^\circ , where the DXL path crosses the Galactic plane, is 33 %
  +/- 6 % ({statistical})+/- 12 % ({systematic}) for R1, 44 % +/- 6 %
  +/- 5 % for R2, 18 % +/- 12 % +/- 11 % for R4, 14 % +/- 11 % +/-
  9 % for R5, and negligible for the R6 and R7 bands. Reliable models
  for the distribution of neutral H and He in the solar system permit
  estimation of the contribution of interplanetary SWCX emission over
  the the whole sky and correction of the RASS maps. We find that the
  average SWCX contribution in the whole sky is 26 % +/- 6 % +/- 13 %
  for R1, 30 % +/- 4 % +/- 4 % for R2, 8 % +/- 5 % +/- 5 % for R4, 6 %
  +/- 4 % +/- 4 % for R5, and negligible for R6 and R7.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Photometry and spectroscopy of
    LS V+44 17 (Yan+, 2016)
Authors: Yan, J.; Zhang, P.; Liu, W.; Liu, Q.
2016yCat..51510104Y    Altcode:
  Most of our spectra of RX J0440.9+4431 were obtained with the
  2.16m telescope at Xinglong Station of National Astronomical
  Observatories. The optical spectroscopy with an intermediate resolution
  was made with a CCD grating spectrograph at the Cassegrain focus
  of the telescope. We took the red spectra covering from 5500 to
  6700Å. Sometimes low-resolution spectra (covering from 4300 to
  6700Å) were also obtained. In 2012 March and 2013 November, we also
  carried out the spectroscopic observations with the Yunnan Faint
  Object Spectrograph and Camera (YFOSC) instrument of the Lijiang
  2.4m telescope in the Yunnan Astronomical Observatory. The Grism #8
  was used with a resolution of 1.47Å/pixel, with a spectral range
  from 5050 to 9750Å. The journal of our observations is summarized
  in Table1. <P />Since 2007, we performed systematic photometric
  observations on a sample of X-ray binaries with the 100cm Education
  and Science Telescope (EST) and the 80cm Tsinghua-NAOC Telescope (TNT)
  at Xinglong Station of NAOC. The EST, manufactured by EOS Technologies,
  is an altazimuth-mounted reflector with Nasmyth foci at a focal ratio
  of f/8. TNT is an equatorial-mounted Cassegrain system with a focal
  of f/10, made by AstroOptik, funded by Tsinghua University in 2002 and
  jointly operated with NAOC. Both telescopes are equipped with the same
  type of Princeton Instrument 1340*1300 thin back-illuminated CCD. The
  CCD cameras use standard Johnson-Cousins UBVRI filters made by Custom
  Scientific. The BVRI differential magnitudes and their errors are
  listed in Table2. <P />(2 data files).

---------------------------------------------------------
Title: Coronal and Flare Diagnostic with SDO/AIA-discovered Fast
    MHD Wave Trains in Active Regions
Authors: Ofman, Leon; Liu, Wei
2016usc..confE.106O    Altcode:
  Recently, SDO/AIA discovered quasi-periodic, fast-mode propagating
  MHD wave trains (QFPs) that propagate at high speeds of more than 1000
  km/s. The waves provide a new diagnostic tool for coronal seismology
  that includes information on the flare energy release and the magnetic
  structure of the active regions. Many events are now available in a
  statistical study. However, for improved accuracy of coronal seismology,
  3D MHD modeling is required and simple wave-mode analysis may be
  insufficient. We present new results of observationally constrained
  models of QFPs using our recently upgraded radiative, thermally
  conductive, visco-resistive 3D MHD code. The waves are excited by
  time-depended boundary conditions constrained by the spatial (localized)
  and quasi-periodic temporal evolution of a C-class flare typically
  associated with QFPs, and produce observable density and temperature
  fluctuations. We investigate parametrically the excitation, propagation,
  and damping of the waves for a range of key model parameters, such
  as the background temperature, density, magnetic field structure,
  and the location of the flaring site within the active region. We
  synthesize EUV intensities in multiple AIA channels and then obtain the
  model parameters that best reproduce the properties of observed QFPs,
  such as the recent DEM analysis. We discuss the implications of our
  modeling results for the seismological application of QFPs for the
  diagnostic of the active region field and flare pulsations.

---------------------------------------------------------
Title: Comparison and Analysis of BeiDou Satellite Single-system
    Precise Orbit Determination
Authors: Liu, W. P.; Hao, J. M.; Deng, K.; Chen, Y. L.
2016AcASn..57..534L    Altcode:
  The method of double-difference dynamic precise orbit determination for
  BeiDou satellites by using both carrier phase and smoothed pseudo-range
  is presented. The data processing flows of zero-difference and
  double-difference dynamic precise orbit determination for BeiDou
  satellites are presented. And the two methods are analyzed. The
  precision of two methods is compared based on the real data. The results
  show that in the condition of stations layout and by using the two
  methods, the three-dimension precision of GEO (Geostationary Earth
  Orbit Satellite) can reach about 1 m, and those of IGSO (Inclined
  Geosynchronous Earth Orbit Satellite) and MEO (Medium Earth Orbit
  Satellite) can be better than 0.5 m. And the radial precision of the
  three kinds of orbit satellites can be all better than 10 cm. Compared
  with the zero-difference dynamic method, the orbit precision of GEO
  is better with the double-difference dynamic method, and that of IGSO
  is comparable, but that of MEO is worse.

---------------------------------------------------------
Title: Data-driven Radiative Hydrodynamic Modeling of the 2014 March
    29 X1.0 Solar Flare
Authors: Rubio da Costa, Fatima; Kleint, Lucia; Petrosian, Vahé;
   Liu, Wei; Allred, Joel C.
2016ApJ...827...38R    Altcode: 2016arXiv160304951R; 2016ApJ...827...38D
  Spectroscopic observations of solar flares provide critical diagnostics
  of the physical conditions in the flaring atmosphere. Some key
  features in observed spectra have not yet been accounted for in
  existing flare models. Here we report a data-driven simulation of
  the well-observed X1.0 flare on 2014 March 29 that can reconcile some
  well-known spectral discrepancies. We analyzed spectra of the flaring
  region from the Interface Region Imaging Spectrograph (IRIS) in Mg
  II h&amp;k, the Interferometric BIdimensional Spectropolarimeter at
  the Dunn Solar Telescope (DST/IBIS) in Hα 6563 Å and Ca II 8542 Å,
  and the Reuven Ramaty High Energy Solar Spectroscope Imager (RHESSI)
  in hard X-rays. We constructed a multithreaded flare loop model and
  used the electron flux inferred from RHESSI data as the input to
  the radiative hydrodynamic code RADYN to simulate the atmospheric
  response. We then synthesized various chromospheric emission lines
  and compared them with the IRIS and IBIS observations. In general, the
  synthetic intensities agree with the observed ones, especially near the
  northern footpoint of the flare. The simulated Mg II line profile has
  narrower wings than the observed one. This discrepancy can be reduced
  by using a higher microturbulent velocity (27 km s<SUP>-1</SUP>) in a
  narrow chromospheric layer. In addition, we found that an increase of
  electron density in the upper chromosphere within a narrow height range
  of ≈800 km below the transition region can turn the simulated Mg II
  line core into emission and thus reproduce the single peaked profile,
  which is a common feature in all IRIS flares.

---------------------------------------------------------
Title: Dynamics of a Prominence-horn Structure during Its Evaporation
    in the Solar Corona
Authors: Wang, Bing; Chen, Yao; Fu, Jie; Li, Bo; Li, Xing; Liu, Wei
2016ApJ...827L..33W    Altcode: 2016arXiv160804095W
  The physical connections among and formation mechanisms of various
  components of the prominence-horn cavity system remain elusive. Here
  we present observations of such a system, focusing on a section
  of the prominence that rises and separates gradually from the main
  body. This forms a configuration sufficiently simple to yield clues
  regarding the above issues. It is characterized by embedding horns,
  oscillations, and a gradual disappearance of the separated material. The
  prominence-horn structure exhibits a large-amplitude longitudinal
  oscillation with a period of ∼150 minutes and an amplitude of ∼30
  Mm along the trajectory defined by the concave horn structure. The
  horns also experience a simultaneous transverse oscillation with a much
  smaller amplitude (∼3 Mm) and a shorter period (∼10-15 minutes),
  likely representative of a global mode of the large-scale magnetic
  structure. The gradual disappearance of the structure indicates that the
  horn, an observational manifestation of the field-aligned transition
  region separating the cool and dense prominence from the hot and
  tenuous corona, is formed due to the heating and diluting process of
  the central prominence mass; most previous studies suggested that it
  is the opposite process, I.e., the cooling and condensation of coronal
  plasmas, that formed the horn. This study also demonstrates how the
  prominence transports magnetic flux to the upper corona, a process
  essential for the gradual build-up of pre-eruption magnetic energy.

---------------------------------------------------------
Title: Measuring wind and stress under tropical cyclones with
    scatterometer
Authors: Liu, W. Timothy
2016cosp...41E1178L    Altcode:
  Ocean surface stress, the turbulent transport of momentum, is largely
  derived from wind through a drag coefficient. In tropical cyclones
  (TC), scatterometers have difficulty in measuring strong wind and
  there is large uncertainty in the drag coefficient. We postulate that
  the microwave backscatter from ocean surface roughness, which is in
  equilibrium with local stress, does not distinguish weather systems. The
  reduced sensitivity of scatterometer wind retrieval algorithm under the
  strong wind is an air-sea interaction problem that is caused by a change
  in the behavior of the drag coefficient and not a sensor problem. Under
  this assumption, we applied a stress retrieval algorithm developed
  over a moderate wind range to retrieve stress under the strong winds
  of TCs. Over a moderate wind range, the abundant wind measurements and
  more established drag coefficient value allow sufficient stress data to
  be computed from wind to develop a stress retrieval algorithm for the
  scatterometer. Using unprecedented large amount of stress retrieved from
  the scatterometer coincident with strong winds in TC, we showed that the
  drag coefficient decreases with wind speed at a much steeper rate than
  previously revealed, for wind speeds over 25 m/s. The result implies
  that the ocean applies less drag to inhibit TC intensification and the
  TC causes less ocean mixing and surface cooling than previous studies
  indicated. With continuous and extensive coverage from constellations
  of scatterometers for several decades, the impact of tropical cyclones
  on the ocean and the feedback from the ocean are examined.

---------------------------------------------------------
Title: The disk-jet connection of Fermi 2LAC blazars
Authors: Du, L. M.; Xie, Zh. H.; Yi, T. F.; Xue, R.; Xu, Y. B.; Liu,
   W. G.; Wang, X. H.
2016NewA...46....9D    Altcode:
  In this article, an estimator of the radiative power for blazars is
  proposed and is used in the study of the link between the accretion
  disk power and jet power. The results lend support to the disk-jet
  symbiosis. Since the blazars are strongly beamed sources, our results
  suggest that the Doppler enhancement of the sources needs to be removed
  to obtain physically reasonable results in the disk-jet connection
  study. The results after de-beaming suggest that FSRQs are accreting in
  the radiatively efficient regime, while the BL Lac population shows a
  flatter dependence between jet power and disk power, possibly due to
  a mixture of sources in the radiatively efficient (the broad lined BL
  Lacs) and inefficient (the bulk of the BL Lac population) regimes.

---------------------------------------------------------
Title: Propagation of small size magnetic holes in the magnetospheric
    plasma sheet
Authors: Yao, S. T.; Shi, Q. Q.; Li, Z. Y.; Wang, X. G.; Tian, A. M.;
   Sun, W. J.; Hamrin, M.; Wang, M. M.; Pitkänen, T.; Bai, S. C.; Shen,
   X. C.; Ji, X. F.; Pokhotelov, D.; Yao, Z. H.; Xiao, T.; Pu, Z. Y.; Fu,
   S. Y.; Zong, Q. G.; De Spiegeleer, A.; Liu, W.; Zhang, H.; Rème, H.
2016JGRA..121.5510Y    Altcode:
  Magnetic holes (MHs), characteristic structures where the magnetic
  field magnitude decreases significantly, have been frequently observed
  in space plasmas. Particularly, small size magnetic holes (SSMHs) which
  the scale is less than or close to the proton gyroradius are recently
  detected in the magnetospheric plasma sheet. In this study of Cluster
  observations, by the timing method, the minimum directional difference
  (MDD) method, and the spatiotemporal difference (STD) method, we obtain
  the propagation velocity of SSMHs in the plasma flow frame. Furthermore,
  based on electron magnetohydrodynamics (EMHD) theory we calculate the
  velocity, width, and depth of the electron solitary wave and compare
  it to SSMH observations. The result shows a good accord between the
  theory and the observation.

---------------------------------------------------------
Title: Understanding the formation of the Mg II h&amp;k lines during
    solar flares
Authors: Rubio Da Costa, Fatima; Kleint, Lucia; Petrosian, Vahe';
   Liu, Wei; Allred, Joel C.
2016SPD....4740304R    Altcode:
  The Mg II h&amp;k lines are useful diagnostics for physical processes
  in the solar chromosphere. Understanding the line formation is
  crucial for the correct interpretation of spectral observations
  and characteristics such as line asymmetries or how their central
  reversals in the line cores disappear and turn into emission during
  flares are manifestations of various physical processes.Focusing on
  the well-observed X1.0 flare on 2014 March 29, we carried out a joint
  observational and modeling study to analyze the Mg II h&amp;k spectra
  observed by IRIS. We constructed a multi-threaded flare loop model and
  used the time-dependent electron flux inferred from the RHESSI hard
  X-ray data as the input to the radiative hydrodynamic code RADYN to
  simulate the atmospheric response. Using the RH code we conducted a
  detailed modeling on line shape and evolution to derive how different
  atmospheric parameters may affect the MgII line emission.We successfully
  simulated the single-peaked Mg II h&amp;k line profiles by increasing
  electron density in the upper chromosphere within a narrow height range
  of ≈ 800 km below the transition region. To our knowledge, this is the
  first successful attempt in reproducing such line-profile shapes under
  flaring conditions. We will discuss the implications of this result for
  diagnosing atmospheric dynamics and energy transport in solar flares.

---------------------------------------------------------
Title: Fast-mode Coronal Wave Trains Detected by SDO/AIA: Recent
    Observational Progress
Authors: Liu, Wei; Downs, Cooper; Ofman, Leon
2016SPD....4730802L    Altcode:
  Quasi-periodic Fast Propagating wave trains (QFPs) are a new
  observational phenomenon discovered by SDO/AIA in extreme ultraviolet
  (EUV). They are fast-mode magnetosonic waves, closely related to
  quasi-periodic pulsations in solar flare emission ranging from
  radio to X-ray wavelengths. The significance of QFPs lies in their
  diagnostic potential, because they can provide critical clues to flare
  energy release and serve as new tools for coronal seismology. In
  this presentation, we report recent advances in observing QFPs. In
  particular, using differential emission measure (DEM) inversion,
  we found clear evidence of heating and cooling cycles that are
  consistent with alternating compression and rarefaction expected for
  magnetosonic wave pulses. We also found that different local magnetic
  and plasma environments can lead to two distinct types of QFPs located
  in different spatial domains with respect to their accompanying
  coronal mass ejections (CMEs). Moreover, recent IRIS observations
  of QFP source regions revealed sawtooth-like flare ribbon motions,
  indicative of pulsed magnetic reconnection, that are correlated with
  QFP excitation. More interestingly, from a statistical survey of over
  100 QFP events, we found a preferential association with eruptive
  flares rather than confined flares. We will discuss the implications
  of these results and the potential roles of QFPs in coronal heating,
  energy transport, and solar eruptions.

---------------------------------------------------------
Title: IRIS Observations of a Novel, Hybrid Prominence-Coronal
    Rain Complex
Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong
2016SPD....47.0402L    Altcode:
  Solar prominences and coronal rain are intimately related phenomena,
  both involving cool material at chromospheric temperatures within the
  hot corona and both playing important roles as part of the return flow
  of the chromosphere-corona mass cycle. At the same time, they exhibit
  distinct morphologies and dynamics not yet well understood. Quiescent
  prominences consist of numerous long-lasting, filamentary downflow
  threads, while coronal rain is more transient and falls comparably
  faster along well-defined curved paths. We report here a novel, hybrid
  prominence-coronal rain complex in an arcade-fan geometry observed
  by IRIS and SDO/AIA, which provides new insights to the underlying
  physics of such contrasting behaviors. We found that the supra-arcade
  fan region hosts a prominence sheet consisting of meandering threads
  with broad Mg II k/h line widths. As the prominence material descends to
  the arcade, it turns into coronal rain sliding down coronal loops with
  line widths 2-3 times narrower. This contrast suggests that distinct
  local plasma and magnetic conditions determine the fate of the cool
  material, a scenario supported by our magnetic field extrapolations from
  SDO/HMI. Specifically, the supra-arcade fan (similar to those in solar
  flares; e.g., McKenzie 2013) is likely situated in a current sheet,
  where the magnetic field is weak and the plasma-beta could be close to
  unity, thus favoring turbulent flows like those prominence threads. In
  contrast, the underlying arcade has a stronger magnetic field and
  most likely a low-beta environment, such that the material is guided
  along magnetic field lines to appear as coronal rain. We will discuss
  the implications of these novel results for future observations e.g.,
  with DKIST.

---------------------------------------------------------
Title: Realistic Modeling of SDO/AIA-discovered Coronal Fast MHD
    Wave Trains in Active Regions
Authors: Ofman, Leon; Liu, Wei
2016SPD....47.0621O    Altcode:
  High-resolution EUV observations by space telescopes have provided
  plenty of evidence for coronal MHD waves in active regions. In
  particular, SDO/AIA discovered quasi-periodic, fast-mode propagating
  MHD wave trains (QFPs), which can propagate at speeds of ~1000 km/s
  perpendicular to the magnetic field. Such waves can provide information
  on the energy release of their associated flares and the magnetized
  plasma structure of the active regions. Before we can use these waves
  as tools for coronal seismology, 3D MHD modeling is required for
  disentangling observational ambiguities and improving the diagnostic
  accuracy. We present new results of observationally contained models
  of QFPs using our recently upgraded radiative, thermally conductive,
  visco-resistive 3D MHD code. The waves are excited by time-depended
  boundary conditions constrained by the spatial (localized) and
  quasi-periodic temporal evolution of a C-class flare typically
  associated with QFPs. We investigate the excitation, propagation,
  and damping of the waves for a range of key model parameters, such as
  the background temperature, density, magnetic field structure, and the
  location of the flaring site within the active region. We synthesize
  EUV intensities in multiple AIA channels and then obtain the model
  parameters that best reproduce the properties of observed QFPs. We
  discuss the implications of our model results for the seismological
  application of QFPs and for understanding the dynamics of their
  associated flares.

---------------------------------------------------------
Title: Microwave Imaging of a Hot Flux Rope Structure during the
    Pre-impulsive Stage of an Eruptive M7.7 Solar Flare
Authors: Wu, Zhao; Chen, Yao; Huang, Guangli; Nakajima, Hiroshi;
   Song, Hongqiang; Melnikov, Victor; Liu, Wei; Li, Gang; Chandrashekhar,
   Kalugodu; Jiao, Fangran
2016ApJ...820L..29W    Altcode: 2016arXiv160302777W
  Corona structures and processes during the pre-impulsive stage of
  solar eruption are crucial to understanding the physics leading
  to the subsequent explosive energy release. Here we present the
  first microwave imaging study of a hot flux rope structure during
  the pre-impulsive stage of an eruptive M7.7 solar flare, with the
  Nobeyama Radioheliograph at 17 GHz. The flux rope is also observed by
  the SDO/AIA in its hot passbands of 94 and 131 Å. In the microwave
  data, it is revealed as an overall arcade-like structure consisting of
  several intensity enhancements bridged by generally weak emissions,
  with brightness temperatures (T <SUB>B</SUB>) varying from ∼10,000
  K to ∼20,000 K. Locations of microwave intensity enhancements along
  the structure remain relatively fixed at certain specific parts of
  the flux rope, indicating that the distribution of emitting electrons
  is affected by the large-scale magnetic configuration of the twisted
  flux rope. Wavelet analysis shows a pronounced 2 minute period of
  the microwave T <SUB>B</SUB> variation during the pre-impulsive
  stage of interest. The period agrees well with that reported for AIA
  sunward-contracting loops and upward ejective plasmoids (suggested
  to be reconnection outflows). This suggests that both periodicities
  are controlled by the same reconnection process that takes place
  intermittently at a 2 minute timescale. We infer that at least a part
  of the emission is excited by non-thermal energetic electrons via the
  gyro-synchrotron mechanism. The study demonstrates the potential of
  microwave imaging in exploring the flux rope magnetic geometry and
  relevant reconnection process during the onset of solar eruption.

---------------------------------------------------------
Title: Analysis of a Limb Eruptive Event
Authors: Kotrč, P. Kupryakov, Yu. A.; Bárta, M.; Kashapova, K.,
   L.; Liu, W.
2016ASPC..504...51K    Altcode:
  We present the analysis of an eruptive event that took place on the
  eastern limb on April 21, 2015, which was observed by the Ondřejov
  horizontal telescope and spectrograph. The eruption of the highly
  twisted prominence was followed by the onset of soft X-ray sources. We
  identified the structures observed in Hα spectra with the details on
  the Hα filtergrams and analyzed the evolution of Doppler component
  velocities. The timing and observed characteristics of the eruption
  were compared with the prediction of the model based on the twisting
  of the flux ropes and the kink/torus instability.

---------------------------------------------------------
Title: The potential of crowdsourcing and mobile technology to
    support flood disaster risk reduction
Authors: See, Linda; McCallum, Ian; Liu, Wei; Mechler, Reinhard;
   Keating, Adriana; Hochrainer-Stigler, Stefan; Mochizuki, Junko;
   Fritz, Steffen; Dugar, Sumit; Arestegui, Michael; Szoenyi, Michael;
   Laso-Bayas, Juan-Carlos; Burek, Peter; French, Adam; Moorthy, Inian
2016EGUGA..1811261S    Altcode:
  The last decade has seen a rise in citizen science and crowdsourcing for
  carrying out a variety of tasks across a number of different fields,
  most notably the collection of data such as the identification of
  species (e.g. eBird and iNaturalist) and the classification of images
  (e.g. Galaxy Zoo and Geo-Wiki). Combining human computing with the
  proliferation of mobile technology has resulted in vast amounts of
  geo-located data that have considerable value across multiple domains
  including flood disaster risk reduction. Crowdsourcing technologies,
  in the form of online mapping, are now being utilized to great effect
  in post-disaster mapping and relief efforts, e.g. the activities of
  Humanitarian OpenStreetMap, complementing official channels of relief
  (e.g. Haiti, Nepal and New York). Disaster event monitoring efforts have
  been further complemented with the use of social media (e.g. twitter
  for earthquakes, flood monitoring, and fire detection). Much of the
  activity in this area has focused on ex-post emergency management while
  there is considerable potential for utilizing crowdsourcing and mobile
  technology for vulnerability assessment, early warning and to bolster
  resilience to flood events. This paper examines the use of crowdsourcing
  and mobile technology for measuring and monitoring flood hazards,
  exposure to floods, and vulnerability, drawing upon examples from the
  literature and ongoing projects on flooding and food security at IIASA.

---------------------------------------------------------
Title: Long-term Optical Studies of the Be/X-Ray Binary RX
    J0440.9+4431/LS V+44 17
Authors: Yan, Jingzhi; Zhang, Peng; Liu, Wei; Liu, Qingzhong
2016AJ....151..104Y    Altcode: 2016arXiv160207778Y
  We present the spectroscopic and photometric observations on the
  Be/X-ray binary RX J0440.9+4431 from 2001 to 2014. The short-term and
  long-term variability of the Hα line profile indicates that one-armed
  global oscillations existed in the circumstellar disk. Several
  positive and negative correlations between the V-band brightness
  and the Hα intensity were found from the long-term photometric and
  spectroscopic observations. We suggest that the monotonic increase
  of the V-band brightness and the Hα brightness between our 2005 and
  2007 observations might be the result of a continuous mass ejection
  from the central Be star, while the negative correlation in 2007-2010
  should be caused by the cessation of mass loss from the Be star
  just before the decline in V-band brightness began (around our 2007
  observations). With the extension of the ejection material, the largest
  circumstellar disk during the last two decades has been observed in our
  2010 observations with an equivalent width of approximately -12.88 Å,
  which corresponds to a circumstellar disk with a size of 12.9 times
  the radius of the central Be star. Three consecutive X-ray outbursts
  peaking around MJD 55293, 55444, and 55591 might be connected with the
  largest circumstellar disk around the Be star. We also use the orbital
  motion of the neutron star as a probe to constrain the structure of
  the circumstellar disk and estimate the eccentricity of the binary
  system to be ≥0.4. After three years of the Hα intensity decline
  after the X-ray outbursts, a new circumstellar disk was being formed
  around the Be star after our 2013 observations.

---------------------------------------------------------
Title: The composition and tail activity of Sun-grazing comets
Authors: Jia, Ying-Dong; Russell, Cristopher; Liu, Wei
2016EGUGA..1810155J    Altcode:
  Sun-grazing comets dive into the low corona to reveal the ambient
  plasma and field conditions with its very active EUV and X-ray radiation
  patterns. In this study we model the charging-balanced cometary plasma,
  and its transportation in the solar magnetic field. We study the
  comet C/2011 W3 (Lovejoy) event seen by SDO, Stereo and SOHO. Our model
  provides line-of-sight integrated emission intensity calculated via each
  emission lines of each charge state of O, and Fe ions. Such intensity is
  then compared with the observed EUV and X-ray images. Typical structures
  of the coronal magnetic field are studied to investigate their effects
  on the comet tail, and to model the observed tail activity.

---------------------------------------------------------
Title: Imaging a Magnetic-breakout Solar Eruption
Authors: Chen, Yao; Du, Guohui; Zhao, Di; Wu, Zhao; Liu, Wei; Wang,
   Bing; Ruan, Guiping; Feng, Shiwei; Song, Hongqiang
2016ApJ...820L..37C    Altcode:
  The fundamental mechanism initiating coronal mass ejections (CMEs)
  remains controversial. One of the leading theories is magnetic breakout,
  in which magnetic reconnection occurring high in the corona removes the
  confinement on an energized low-corona structure from the overlying
  magnetic field, thus allowing it to erupt. Here, we report critical
  observational evidence of this elusive breakout reconnection in a
  multi-polar magnetic configuration that leads to a CME and an X-class,
  long-duration flare. Its occurrence is supported by the presence of
  pairs of heated cusp-shaped loops around an X-type null point and
  signatures of reconnection inflows. Other peculiar features new to
  the breakout picture include sequential loop brightening, coronal hard
  X-rays at energies up to ∼100 keV, and extended high-corona X-rays
  above the later restored multi-polar structure. These observations, from
  a novel perspective with clarity never achieved before, present crucial
  clues to understanding the initiation mechanism of solar eruptions.

---------------------------------------------------------
Title: Quasi-periodic fast-mode magnetosonic wave trains within
    coronal waveguides associated with flares and CMEs
Authors: Liu, Wei; Ofman, Leon; Broder, Brittany; Karlický, Marian;
   Downs, Cooper
2016AIPC.1720d0010L    Altcode: 2015arXiv151207930L
  Quasi-periodic, fast-mode, propagating wave trains (QFPs) are a new
  observational phenomenon recently discovered in the solar corona by
  the Solar Dynamics Observatory with extreme ultraviolet (EUV) imaging
  observations. They originate from flares and propagate at speeds up to
  ∼2000 km s<SUP>-1</SUP> within funnel-shaped waveguides in the wakes
  of coronal mass ejections (CMEs). QFPs can carry suffcient energy fluxes
  required for coronal heating during their occurr ences. They can provide
  new diagnostics for the solar corona and their associated flares. We
  present recent observations of QFPs focusing on their spatio-temporal
  properties, temperature dependence, and statistical correlation
  with flares and CMEs. Of particular interest is the 2010-Aug-01 C3.2
  flare with correlated QFPs and drifting zebra and fiber radio bursts,
  which might be different manifestations of the same fast-mode wave
  trains. We also discuss the potential roles of QFPs in accelerating
  and/or modulating the solar wind.

---------------------------------------------------------
Title: Reduced interdecadal variability of Atlantic Meridional
    Overturning Circulation under global warming
Authors: Cheng, Jun; Liu, Zhengyu; Zhang, Shaoqing; Liu, Wei; Dong,
   Lina; Liu, Peng; Li, Hongli
2016PNAS..113.3175C    Altcode:
  Interdecadal variability of the Atlantic Meridional Overturning
  Circulation (AMOC-IV) plays an important role in climate variation and
  has significant societal impacts. Past climate reconstruction indicates
  that AMOC-IV has likely undergone significant changes. Despite some
  previous studies, responses of AMOC-IV to global warming remain unclear,
  in particular regarding its amplitude and time scale. In this study,
  we analyze the responses of AMOC-IV under various scenarios of future
  global warming in multiple models and find that AMOC-IV becomes weaker
  and shorter with enhanced global warming. From the present climate
  condition to the strongest future warming scenario, on average,
  the major period of AMOC-IV is shortened from ∼50 y to ∼20 y,
  and the amplitude is reduced by ∼60%. These reductions in period
  and amplitude of AMOC-IV are suggested to be associated with increased
  oceanic stratification under global warming and, in turn, the speedup
  of oceanic baroclinic Rossby waves.

---------------------------------------------------------
Title: Preface
Authors: Liu, W. -P.; Li, Z. -H.; Wang, Y. -B.; Guo, B.; Shen, Y. -P.
2016EPJWC.10900001L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Astrophysical S<SUB>E2</SUB> factor of the <SUP>12</SUP>C(α,
    γ)<SUP>16</SUP>O reaction through the <SUP>12</SUP>C(<SUP>11</SUP>B,
    <SUP>7</SUP>Li)<SUP>16</SUP>O transfer reaction
Authors: Guo, B.; Du, X. C.; Li, Z. H.; Li, Y. J.; Pang, D. Y.; Su,
   J.; Yan, S. Q.; Fan, Q. W.; Gan, L.; Han, Z. Y.; Li, E. T.; Li, X. Y.;
   Lian, G.; Liu, J. C.; Pei, C. J.; Qiao, L. H.; Shen, Y. P.; Su, Y.;
   Wang, Y. B.; Zeng, S.; Zhou, Y.; Liu, W. P.
2016EPJWC.10904003G    Altcode:
  The <SUP>12</SUP>C(α, γ)<SUP>16</SUP>O reaction plays a key role in
  the evolution of stars with masses of M &gt; 0.55 M<SUB>⊙</SUB>. At
  the Gamow peak (E<SUB>c.m.</SUB> = 300 ke V, T<SUB>9</SUB> = 0.2),
  the cross section of the <SUP>12</SUP>C(α, γ)<SUP>16</SUP>O reaction
  is so small (about 10<SUP>-17</SUP> barn) that the direct measurement
  in ground laboratory is not feasible with the existing technology. Up
  to now, the cross sections at lower energies can only be extrapolated
  from the data at higher energies. However, two subthreshold resonances,
  locating at E<SUB>x</SUB> = 7.117 MeV and E<SUB>x</SUB> = 6.917 MeV,
  make this extrapolation more complicated. In this work the 6.917 MeV
  subthreshold resonance in the <SUP>12</SUP>C(α, γ)<SUP>16</SUP>O
  reaction was investigated via the <SUP>12</SUP>C(<SUP>11</SUP>B,
  <SUP>7</SUP>Li)<SUP>16</SUP>O reaction. The experiment was performed
  using the Q3D magnetic spectrograph at HI-13 tandem accelerator. We
  measured the angular distribution of the <SUP>12</SUP>C(<SUP>11</SUP>B,
  <SUP>7</SUP>Li)<SUP>16</SUP>O transfer reaction leading to the
  6.917 MeV state. Based on DWBA analysis, we derived the square of
  ANC of the 6.917 MeV level in <SUP>16</SUP>O to be (2.45± 0.28)
  ×10<SUP>10</SUP> fm<SUP>-1</SUP>, with which the reduced-α width can
  be computed. Finally, we calculated the astrophysical S<SUB>E2</SUB>
  factor of the 6.917 MeV resonance to be 67.6 ± 7.7 ke V b.

---------------------------------------------------------
Title: Two measurements of the <SUP>22</SUP>Na+p resonant scattering
    via thick-target inverse-kinematics method
Authors: Wang, Y. B.; Jin, S. J.; Jing, L.; Han, Z. Y.; Bai, X. X.;
   Guo, B.; Li, Y. J.; Li, Z. H.; Lian, G.; Su, J.; Sun, L. J.; Yan,
   S. Q.; Zeng, S.; Liu, W. P.; Yamaguchi, H.; Kubono, S.; Hu, J.; Kahl,
   D.; He, J. J.; Wang, J. S.; Tang, X. D.; Xu, S. W.; Ma, P.; Zhang,
   N. T.; Bai, Z.; Huang, M. R.; Jia, B. L.; Jin, S. L.; Ma, J. B.;
   Ma, S. B.; Ma, W. H.; Yang, Y. Y.; Zhang, L. Y.; Jung, H. S.; Moon,
   J. Y.; Lee, C. S.; Teranishi, T.; Wang, H. W.; Ishiyama, H.; Iwasa,
   N.; Komatsubara, T.; Brown, B. A.
2016EPJWC.10904010W    Altcode:
  <SUP>22</SUP>Na is an important isotope for the study of extinct
  radioactivity, meanwhile its sufficiently long half life provides
  the possibility to observe live <SUP>22</SUP>Na in nearby nova
  explosions. The <SUP>22</SUP>Na(p,γ) <SUP>23</SUP>Mg is one of
  the key reactions that influence the <SUP>22</SUP>Na abundance in
  nova ejecta. To study the proton resonant states in <SUP>23</SUP>Mg
  relevant to the astrophysical <SUP>22</SUP>Na(p,γ) <SUP>23</SUP>Mg
  reaction rates, two measurements have been carried out at the CRIB
  separator of University of Tokyo, and the RIBLL secondary beamline
  in Lanzhou, respectively. The <SUP>22</SUP>Na secondary beam was
  produced via the <SUP>1</SUP>H(<SUP>22</SUP>Ne, <SUP>22</SUP>Na)n
  charge exchange reaction. Thick-target inverse-kinematics method
  is applied to obtain the excitation function of <SUP>22</SUP>Na+p
  elastic scattering. Extended gas target and solid state polyethylene
  foil were used in the two measurements, respectively, to map
  the different excitation energy region of the compound nucleus
  <SUP>23</SUP>Mg. Several new resonant levels are observed and their
  contribution to the <SUP>22</SUP>Na(p,γ) <SUP>23</SUP>Mg reaction
  rate is evaluated.

---------------------------------------------------------
Title: Optical potential parameters from <SUP>12</SUP>C + Zr elastic
    scattering
Authors: Gan, L.; Li, Z. H.; Sun, H. B.; Su, J.; Li, Y. J.; Yan,
   S. Q.; Wang, Y. B.; Zeng, S.; Bai, X. X.; Du, X. C.; Wu, Z. D.; Jin,
   S. J.; Zhang, W. J.; Liu, W. P.; Li, E. T.
2016EPJWC.10904002G    Altcode:
  The angular distributions of <SUP>12</SUP>C + <SUP>90,92,94,96</SUP>Zr
  elastic scattering were measured with the Q3D magnetic spectrometer
  at the HI-13 tandem accelerator, Beijing. The real part of
  optical potential were extracted by analysing these angular
  distributions. The analysis enable us to avoid the influence of
  Coulomb effect and to observe the dependence of optical potential
  on the nuclear properties. With the deduced potential parameters,
  the experimental elastic scattering angular distributions can be
  reproduced very well. Formulas to infer global heavy-ion potential
  parameters were obtained then by analyzing the extracted optical
  potential parameters. The formulas can be used widely in heavy-ion
  nuclear reactions.

---------------------------------------------------------
Title: Identifying magnetic reconnection events using the FOTE method
Authors: Fu, H. S.; Cao, J. B.; Vaivads, A.; Khotyaintsev, Y. V.;
   Andre, M.; Dunlop, M.; Liu, W. L.; Lu, H. Y.; Huang, S. Y.; Ma, Y. D.;
   Eriksson, E.
2016JGRA..121.1263F    Altcode:
  A magnetic reconnection event detected by Cluster is analyzed using
  three methods: Single-spacecraft Inference based on Flow-reversal
  Sequence (SIFS), Multispacecraft Inference based on Timing a Structure
  (MITS), and the First-Order Taylor Expansion (FOTE). Using the SIFS
  method, we find that the reconnection structure is an X line; while
  using the MITS and FOTE methods, we find it is a magnetic island (O
  line). We compare the efficiency and accuracy of these three methods
  and find that the most efficient and accurate approach to identify
  a reconnection event is FOTE. In both the guide and nonguide field
  reconnection regimes, the FOTE method is equally applicable. This study
  for the first time demonstrates the capability of FOTE in identifying
  magnetic reconnection events; it would be useful to the forthcoming
  Magnetospheric Multiscale (MMS) mission.

---------------------------------------------------------
Title: Fermi Large Area Telescope observation of high-energy solar
flares: constraining emission scenarios
Authors: Omodei, Nicola; Pesce-Rollins, Melissa; Petrosian, Vahè;
   Liu, Wei; da Costa, Fatima Rubio; Allafort, Alice
2016IAUS..320...51O    Altcode:
  The Fermi Large Area Telescope (LAT) is the most sensitive instrument
  ever deployed in space for observing gamma-ray emission &gt;100
  MeV. This has also been demonstrated by its detection of quiescent
  gamma-ray emission from pions produced by cosmic-ray protons
  interacting in the solar atmosphere, and from cosmic-ray electron
  interactions with solar optical photons. The Fermi-LAT has also
  detected high-energy gamma-ray emission associated with GOES M-class
  and X-class solar flares, each accompanied by a coronal mass ejection
  and a solar energetic particle event, increasing the number of detected
  solar flares by almost a factor of 10 with respect to previous space
  observations. During the impulsive phase, gamma rays with energies up
  to several hundreds of MeV have been recorded by the LAT. Emission up
  to GeV energies lasting several hours after the flare has also been
  detected by the LAT. Of particular interest are the recent detections
  of three solar flares whose position behind the limb was confirmed
  by the STEREO satellites. While gamma-ray emission up to tens of
  MeV resulting from proton interactions has been detected before from
  occulted solar flares, the significance of these particular events
  lies in the fact that these are the first detections of &gt;100 MeV
  gamma-ray emission from footpoint-occulted flares. We will present the
  Fermi-LAT, RHESSI and STEREO observations of these flares and discuss
  the various emission scenarios for these sources.

---------------------------------------------------------
Title: GREGOR observations of a small flare above a sunspot
Authors: Sobotka, M.; Dudík, J.; Denker, C.; Balthasar, H.; Jurčák,
   J.; Liu, W.
2016IAUS..320...68S    Altcode:
  A small flare ribbon above a sunspot umbra in active region 12205 was
  observed on November 7, 2014, at 12:00 UT in the blue imaging channel
  of the 1.5-m GREGOR telescope, using a 0.1 nm Ca II H interference
  filter. Context observations from SDO/AIA, Hinode/SOT, and IRIS show
  that the ribbon is a part of a larger one that extends through the
  neighboring positive polarities and also participates in several
  other flares within the active region. A 140 second long time series
  of Ca II H images was reconstructed by means of the Multi-Frame
  Blind Deconvolution method, giving the respective spatial and
  temporal resolutions of 0”.1 and 1 s. Light curves and horizontal
  velocities of small-scale bright knots in the observed flare ribbon
  were measured. Some knots are stationary but three move along the
  ribbon with speeds of 7-11 km s<SUP>-1</SUP>. Two of them move in the
  opposite direction and exhibit highly correlated intensity changes,
  providing evidence for the presence of slipping reconnection at small
  spatial scales.

---------------------------------------------------------
Title: Evidence for a Very Low-column Density Hole in the Galactic
    Halo in the Direction of the High Latitude Molecular Cloud MBM 16
Authors: Liu, W.; Galeazzi, M.; Ursino, E.
2016ApJ...816...82L    Altcode: 2015arXiv151200043L
  Shadow observations are the only way to observe emission from the
  galactic halo (GH) and/or the circumgalactic medium (CGM) free of any
  foreground contamination from local hot bubble (LHB) and solar wind
  charge exchange (SWCX). We analyzed data from a shadow observation in
  the direction of the high latitude, neutral hydrogen cloud MBM 16 with
  Suzaku. We found that all emission can be accounted for by foreground
  emission from LHB and SWCX, plus power-law emission associated with
  unresolved point sources. The GH/CGM in the direction of MBM 16 is
  negligible or inexistent in our observation, with upper limits on
  the emission measure of 9× {10}<SUP>-4</SUP> pc cm<SUP>-6</SUP>
  (90% C.L.-solar metallicity), at the lowest end of current estimates.

---------------------------------------------------------
Title: Studying the Interstellar Medium and the Inner Region of
    NPS/LOOP 1 with Shadow Observations toward MBM36
Authors: Ursino, E.; Galeazzi, M.; Liu, W.
2016ApJ...816...33U    Altcode: 2015arXiv151200024U
  We analyzed data from a shadow observation of the high density
  molecular cloud MBM36 (l ∼ 4°, b ∼ 35°) with Suzaku. MBM36 is
  located in a region that emits relatively weakly in the 3/4 keV band
  compared to the surrounding North Polar Spur (NPS)/Loop 1 structure
  and the Galactic Bulge (GB). The contrast between high and low density
  targets in the MBM36 area allows one to separate the local and distant
  contributors to the soft diffuse X-ray background, providing a much
  better characterization of the individual components compared to single
  pointing observations. We identify two non-local thermal components,
  one at kT ≈ 0.12 keV and one at kT ≈ 0.29 keV. The colder component
  matches well with models of emission from the higher latitude region
  of the GB. The emission of the warmer component is in agreement with
  models predicting that the NPS is due to a hypershell from the center
  of the Milky Way. Geometrical and pressure calculations rule out a
  nearby bubble as responsible for the emission associated with the
  NPS. Any Galactic Halo/circumgalactic halo emission, if present, is
  outshined by the other components. We also report an excess emission
  around 0.9 keV, likely due to an overabundance of Ne ix.

---------------------------------------------------------
Title: Flare-associated Fast-mode Coronal Wave Trains Discovered by
SDO/AIA: Physical Properties and Implications
Authors: Liu, W.; Ofman, L.; Downs, C.; Cheung, C. M. M.; Broder,
   B.; De Pontieu, B.
2015AGUFMSH54B..02L    Altcode:
  Quasi-periodic Fast Propagating wave trains (QFPs) are a new
  observational phenomenon discovered in extreme ultraviolet (EUV) by
  the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics
  Observatory (SDO). They are fast-mode magnetosonic waves, closely
  related to quasi-periodic pulsations in solar flare emission ranging
  from radio to X-ray wavelengths. The significance of QFPs lies in their
  diagnostic potential, because they can provide critical clues to flare
  energy release and serve as new tools for coronal seismology. In
  this presentation, we report recent advances in observing and
  modeling QFPs. For example, using differential emission measure (DEM)
  inversion, we found clear evidence of heating and cooling cycles that
  are consistent with alternating compression and rarefaction expected
  for magnetosonic wave pulses. Moreover, recent IRIS observations
  of QFP source regions revealed sawtooth-like flare ribbon motions,
  indicative of pulsed magnetic reconnection, that are correlated with QFP
  excitation. More interestingly, from a survey of over 100 QFP events,
  we found a preferential association with eruptive flares rather than
  confined flares. We will discuss the implications of these results
  and the potential roles of QFPs in coronal heating, energy transport,
  and solar eruptions.

---------------------------------------------------------
Title: Fast Wave Trains Associated with Solar Eruptions: Insights
    from 3D Thermodynamic MHD Simulations
Authors: Downs, C.; Liu, W.; Torok, T.; Linker, J.; Mikic, Z.;
   Ofman, L.
2015AGUFMSH22A..06D    Altcode:
  EUV imaging observations during the SDO/AIA era have provided new
  insights into a variety of wave phenomena occurring in the low
  solar corona. One example is the observation of quasi-periodic,
  fast-propagating wave trains that are associated with solar eruptions,
  including flares and CMEs. While there has been considerable
  progress in understanding such waves from both an observational
  and theoretical perspective, it remains a challenge to pin down
  their physical origin. In this work, we detail our results from
  a case-study 3D thermodynamic MHD simulation of a coronal mass
  ejection where quasi-periodic wave trains are generated during the
  simulated eruption. We find a direct correlation between the onset of
  non-steady reconnection in the flare current sheet and the generation
  of quasi-periodic wave train signatures when patchy, collimated
  downflows interact with the flare arcade. Via forward modeling of
  SDO/AIA observables, we explore how the appearance of the wave trains
  is affected by line-of-sight integration and the multi-thermal nature
  of the coronal medium. We also examine how the wave trains themselves
  are channeled by natural waveguides formed in 3D by the non-uniform
  background magnetic field. While the physical association of the
  reconnection dynamics to the generation of quasi-periodic wave trains
  appears to be a compelling result, unanswered questions posed from
  recent observations as well as future prospects will be discussed.

---------------------------------------------------------
Title: Dynamic plasmapause model based on THEMIS measurements
Authors: Liu, X.; Liu, W.; Cao, J. B.; Fu, H. S.; Yu, J.; Li, X.
2015JGRA..12010543L    Altcode:
  This paper presents a dynamic plasmapause location model established
  based on 5 years of Time History of Events and Macroscale Interactions
  during Substorms (THEMIS) measurements from 2009 to 2013. In total,
  5878 plasmapause crossing events are identified, sufficiently covering
  all 24 magnetic local time (MLT) sectors. Based on this plasmapause
  crossing database, we investigate the correlations between plasmapause
  locations with solar wind parameters and geomagnetic indices. Input
  parameters for the best fits are obtained for different MLT sectors,
  and finally, we choose five input parameters to build a plasmapause
  location model, including 5 min-averaged SYM-H, AL, and AU indices
  as well as hourly-averaged AE and Kp indices. two out-of-sample
  comparisons on the evolution of the plasmapause is shown during two
  magnetic storms, demonstrating good agreement between model results and
  observations. Two major advantages are achieved by this model. First,
  this model provides plasmapause locations at 24 MLT sectors, still
  providing good consistency with observations. Second, this model is
  able to reproduce dynamic variations of the plasmapause on timescales
  as short as 5 min.

---------------------------------------------------------
Title: Mg II Lines Observed During the X-class Flare on 29 March
    2014 by the Interface Region Imaging Spectrograph
Authors: Liu, W.; Heinzel, P.; Kleint, L.; Kašparová, J.
2015SoPh..290.3525L    Altcode: 2015SoPh..tmp..166L; 2015arXiv151100480L
  Mg II lines represent one of the strongest emissions from the
  chromospheric plasma during solar flares. In this article, we
  studied the Mg II lines observed during the X1 flare on 29 March 2014
  (SOL2014-03-29T17:48) by the Interface Region Imaging Spectrograph
  (IRIS). IRIS detected large intensity enhancements of the Mg II h and
  k lines, subordinate triplet lines, and several other metallic lines
  at the flare footpoints during this flare. We have used the advantage
  of the slit-scanning mode (rastering) of IRIS and performed, for the
  first time, a detailed analysis of spatial and temporal variations
  of the spectra. Moreover, we were also able to identify positions
  of strongest hard X-ray (HXR) emissions using the Reuven Ramaty
  High Energy Solar Spectroscopic Imager (RHESSI) observations and to
  correlate them with the spatial and temporal evolution of IRIS Mg
  II spectra. The light curves of the Mg II lines increase and peak
  contemporarily with the HXR emissions but decay more gradually. There
  are large red asymmetries in the Mg IIh and k lines after the flare
  peak. We see two spatially well-separated groups of Mg II line profiles,
  non-reversed and reversed. In some cases, the Mg II footpoints with
  reversed profiles are correlated with HXR sources. We show the spatial
  and temporal behavior of several other line parameters (line metrics)
  and briefly discuss them. Finally, we have synthesized the Mg IIk line
  using our non-LTE code with the Multilevel Accelerated Lambda Iteration
  (MALI) technique. Two kinds of models are considered, the flare model
  F2 of Machado et al. (Astrophys. J.242, 336, 1980) and the models of
  Ricchiazzi and Canfield (Astrophys. J.272, 739, 1983, RC models). Model
  F2 reproduces the peak intensity of the non-reversed Mg IIk profile
  at flare maximum, but does not account for high wing intensities. On
  the other hand, the RC models show the sensitivity of Mg II line
  intensities to various electron-beam parameters. Our simulations also
  show that the microturbulence produces a broader line core, while the
  intense line wings are caused by an enhanced line source function.

---------------------------------------------------------
Title: A self-consistent combined radiative transfer hydrodynamic and
    particle acceleration model for the X1.0 class flare on March 29, 2014
Authors: Rubio da Costa, F.; Kleint, L.; Sainz Dalda, A.; Petrosian,
   V.; Liu, W.
2015AGUFMSH31B2419R    Altcode:
  The X1.0 flare on March 29, 2014 was well observed, covering its
  emission at several wavelengths from the photosphere to the corona. The
  RHESSI spectra images allow us to estimate the temporal variation of
  the electron spectra using regularized inversion techniques. Using
  this as input for a combined particle acceleration and transport
  (Stanford-Flare) and radiative transfer hydrodynamic (Radyn) code, we
  calculate the response of the atmosphere to the electron heating. We
  will present the evolution of the thermal continuum and several line
  emissions. Comparing them with GOES soft X-ray and high resolution
  observations from IRIS, SDO and DST/IBIS allows us to test the basic
  mechanism(s) of acceleration and to constrain its characteristics. We
  will also present perspectives on how to apply this methodology and
  related diagnostics to other flares.

---------------------------------------------------------
Title: Controls of Earth's dipole tilt angle and background
    magnetosheath flow to the locations of reconnection sites on the
    magnetopasue
Authors: Zhu, C.; Zhang, H.; Ge, Y.; Pu, Z.; Liu, W. L.; Liu, L.;
   Wan, W.; Le, H.; Chen, Y.; Wang, Y. F.
2015AGUFMSM13C2523Z    Altcode:
  Plasma energy-dispersion properties inside reconnection jet flows
  observed in the low latitude boundary layer are used to determine
  the distances of the observing satellites to reconnection sites. The
  locations of the reconnection sites are then retrieved by tracing the
  modeled field lines by those distances. The controlling effects of
  the dipole tilt angle to the location of X-lines or reconnection sites
  are investigated. Our results show that the Earth's dipole tilt angles
  strongly modify the location of X-lines predicted by Cooling et al's
  model, which is thought to be the result of magnetopause reshaping due
  to finite dipole tilt angles. By investigating the magnetosheath flow
  outside the reconnection sites, we found that besides the dipole tilt
  angle the magnetosheath background flows also play a significant role
  in determining the locations of the reconnection sites.

---------------------------------------------------------
Title: Dynamic plasmapause model based on THEMIS measurements
Authors: Liu, W.; Liu, X.
2015AGUFMSM41G2565L    Altcode:
  We will present a dynamic plasmapause location model established based
  on five years of THEMIS measurements from 2009 to 2013. In total,
  5878 plasmapause crossing events are identified, sufficiently covering
  all 24 Magnetic Local Time (MLT) sectors. Based on this plasmapause
  crossing database, we investigate the correlations between plasmapause
  locations with solar wind parameters and geomagnetic indices. Input
  parameters for the best fits are obtained for different MLT sectors
  and finally we choose five input parameters to build a plasmapause
  location model, including five-minute-averaged SYM-H, AL and AU
  indices as well as hourly-averaged AE and Kp indices. An out-of-sample
  comparison on the evolution of the plasmapause is shown during April
  2001 magnetic storm, demonstrating good agreement between model
  results and observations. Two major advantages are achieved by this
  model. First, this model provides plasmapause locations at 24 MLT
  sectors, still providing good consistency with observations. Second,
  this model is able to reproduce dynamic variations of plasmapause in
  the time scale as short as five minutes.

---------------------------------------------------------
Title: Flexible Filter Bank Based on an Improved Weighted Overlap-Add
    Algorithm for Processing Wide Bandwidth Radio Astronomy Signals
Authors: Wang, Xianhai; Meng, Qiao; Han, J. L.; Liu, Wei; Zhang,
   Jianwei
2015PASP..127.1263W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Combined Modeling of Acceleration, Transport, and Hydrodynamic
    Response in Solar Flares. II. Inclusion of Radiative Transfer
    with RADYN
Authors: Rubio da Costa, Fatima; Liu, Wei; Petrosian, Vahé; Carlsson,
   Mats
2015ApJ...813..133R    Altcode: 2015arXiv150501549R
  Solar flares involve complex processes that are coupled and span a
  wide range of temporal, spatial, and energy scales. Modeling such
  processes self-consistently has been a challenge in the past. Here we
  present results from simulations that couple particle kinetics with
  hydrodynamics (HD) of the atmospheric plasma. We combine the Stanford
  unified Fokker-Planck code that models particle acceleration and
  transport with the RADYN HD code that models the atmospheric response
  to collisional heating by accelerated electrons through detailed
  radiative transfer calculations. We perform simulations using two
  different electron spectra, one an ad hoc power law and the other
  predicted by the model of stochastic acceleration by turbulence or
  plasma waves. Surprisingly, the later model, even with energy flux \ll
  {10}<SUP>10</SUP> {erg} {{{s}}}<SUP>-1</SUP> {{cm}}<SUP>-2</SUP>, can
  cause “explosive” chromospheric evaporation and drive stronger
  up- and downflows (and HD shocks). This is partly because our
  acceleration model, like many others, produces a spectrum consisting
  of a quasi-thermal component plus a power-law tail. We synthesize
  emission-line profiles covering different heights in the lower
  atmosphere, including Hα 6563 Å, He ii 304 Å, Ca ii K 3934 Å, and
  Si iv 1393 Å. One interesting result is the unusual high temperature
  (up to a few times 10<SUP>5</SUP> K) of the formation site of He ii
  304 Å, which is expected owing to photoionization-recombination under
  flare conditions, compared to those in the quiet Sun dominated by
  collisional excitation. When compared with observations, our results
  can constrain the properties of nonthermal electrons and thus the
  poorly understood particle acceleration mechanism.

---------------------------------------------------------
Title: Temporal Evolution of Chromospheric Evaporation: Case
    Studies of the M1.1 Flare on 2014 September 6 and X1.6 Flare on 2014
    September 10
Authors: Tian, Hui; Young, Peter R.; Reeves, Katharine K.; Chen, Bin;
   Liu, Wei; McKillop, Sean
2015ApJ...811..139T    Altcode: 2015arXiv150502736T
  With observations from the Interface Region Imaging Spectrograph, we
  track the complete evolution of ∼11 MK evaporation flows in an M1.1
  flare on 2014 September 6 and an X1.6 flare on 2014 September 10. These
  hot flows, as indicated by the blueshifted Fe xxi 1354.08 Å line,
  evolve smoothly with a velocity decreasing exponentially from ∼200
  km s<SUP>-1</SUP> to almost stationary within a few minutes. We find a
  good correlation between the flow velocity and energy deposition rate
  as represented by the hard X-ray flux observed with the Reuven Ramaty
  High Energy Solar Spectroscopic Imager, or time derivative of the soft
  X-ray flux observed with the Geostationary Operational Environmental
  Satellites and the HINODE X-ray Telescope, which is in general agreement
  with models of nonthermal electron heating. The maximum blueshift of
  Fe xxi appears approximately at the same time as or slightly after
  the impulsive enhancement of the ultraviolet continuum and the Mg ii
  2798.8 Å line emission, demonstrating that the evaporation flow is
  closely related to heating of the lower chromosphere. Finally, while
  the hot Fe xxi 1354.08 Å line is entirely blueshifted with no obvious
  rest component, cool chromospheric and transition region lines like
  Si iv 1402.77 Å are often not entirely redshifted but just reveal an
  obvious red wing enhancement at the ribbons, suggesting that the speed
  of chromospheric condensation might be larger than previously thought.

---------------------------------------------------------
Title: LOD First Estimates In 7406 SLR San Juan Argentina Station
Authors: Pacheco, A.; Podestá, R.; Yin, Z.; Adarvez, S.; Liu, W.;
   Zhao, L.; Alvis Rojas, H.; Actis, E.; Quinteros, J.; Alacoria, J.
2015RMxAC..46...29P    Altcode:
  In this paper we show results derived from satellite observations at
  the San Juan SLR station of Felix Aguilar Astronomical Observatory
  (OAFA). The Satellite Laser Ranging (SLR) telescope was installed in
  early 2006, in accordance with an international cooperation agreement
  between the San Juan National University (UNSJ) and the Chinese Academy
  of Sciences (CAS). The SLR has been in successful operation since
  2011 using NAOC SLR software for the data processing. This program
  was designed to calculate satellite orbits and station coordinates,
  however it was used in this work for the determination of LOD (Length
  Of Day) time series and Earth Rotation speed.

---------------------------------------------------------
Title: Measurement of the <SUP>14</SUP>O(α ,p ) <SUP>17</SUP>F
    cross section at E<SUB>c .m .</SUB>≈2.1 -5.3 MeV
Authors: Kim, A.; Lee, N. H.; Han, M. H.; Yoo, J. S.; Hahn, K. I.;
   Yamaguchi, H.; Binh, D. N.; Hashimoto, T.; Hayakawa, S.; Kahl, D.;
   Kawabata, T.; Kurihara, Y.; Wakabayashi, Y.; Kubono, S.; Choi, S.;
   Kwon, Y. K.; Moon, J. Y.; Jung, H. S.; Lee, C. S.; Teranishi, T.;
   Kato, S.; Komatsubara, T.; Guo, B.; Liu, W. P.; Wang, B.; Wang, Y.
2015PhRvC..92c5801K    Altcode:
  Background: The <SUP>14</SUP>O(α ,p ) <SUP>17</SUP>F reaction
  plays an important role as the trigger reaction for the x-ray
  burst. <P />Purpose: The direct measurement of <SUP>14</SUP>O(α
  ,p ) <SUP>17</SUP>F was made for studying the resonant states in
  <SUP>18</SUP>Ne and determining the reaction rate of <SUP>14</SUP>O(α
  ,p ) <SUP>17</SUP>F at astrophysical temperatures. <P />Methods: The
  differential cross section of the <SUP>14</SUP>O(α ,p ) <SUP>17</SUP>F
  reaction was measured using a 2.5-MeV/u <SUP>14</SUP>O radioactive
  beam and the thick target method in inverse kinematics. Three sets
  of Δ E -E Si telescopes were installed and coincidence measurements
  were performed. We analyzed single-proton decay events using the
  time-of-flight (TOF) information of the recoiling protons. <P />Results:
  The excitation function of <SUP>14</SUP>O(α ,p ) <SUP>17</SUP>F
  was acquired for excitation energies between 7.2 and 10.4 MeV in
  <SUP>18</SUP>Ne by considering the two channels which decay to the
  ground state and first excited state of <SUP>17</SUP>F . Several new,
  as well as previously known, states in <SUP>18</SUP>Ne were observed and
  their resonance parameters were extracted from R -matrix analysis. The
  contributions of four resonances over the excitation energy range,
  7 &lt;E<SUB>x</SUB>&lt;8.2 MeV , to the <SUP>14</SUP>O(α ,p )
  <SUP>17</SUP>F reaction rate were calculated. <P />Conclusions:
  We observed very strong single-proton decay events, but did not
  observe strong double-proton decay events as in a previous study
  by Fu et al. The reaction rates contributed by the 7.35-, 7.58-,
  and 7.72-MeV states were estimated to be dominant at temperatures
  T<SUB>9</SUB>&gt;2 . Among these three states, the 7.35-MeV state was
  found to enhance the reaction rate by a factor of 10 greater than the
  other two resonance states.

---------------------------------------------------------
Title: Rapid Large Scale Reprocessing of the ODI Archive using the
    QuickReduce Pipeline
Authors: Gopu, A.; Kotulla, R.; Young, M. D.; Hayashi, S.; Harbeck,
   D.; Liu, W.; Henschel, R.
2015ASPC..495...53G    Altcode: 2015adass..24...53G
  The traditional model of astronomers collecting their observations
  as raw instrument data is being increasingly replaced by astronomical
  observatories serving standard calibrated data products to observers and
  to the public at large once proprietary restrictions are lifted. For
  this model to be effective, observatories need the ability to
  periodically re-calibrate archival data products as improved master
  calibration products or pipeline improvements become available, and also
  to allow users to rapidly calibrate their data on-the-fly. Traditional
  astronomy pipelines are heavily I/O dependent and do not scale with
  increasing data volumes. In this paper, we present the One Degree Imager
  - Portal, Pipeline and Archive (ODI-PPA) calibration pipeline framework
  which integrates the efficient and parallelized QuickReduce pipeline
  to enable a large number of simultaneous, parallel data reduction jobs
  - initiated by operators AND/OR users - while also ensuring rapid
  processing times and full data provenance. Our integrated pipeline
  system allows re-processing of the entire ODI archive (∼15,000 raw
  science frames, ∼3.0 TB compressed) within ∼18 hours using twelve
  32-core compute nodes on the Big Red II supercomputer. Our flexible,
  fast, easy to operate, and highly scalable framework improves access to
  ODI data, in particular when data rates double with an upgraded focal
  plane (scheduled for 2015), and also serve as a template for future data
  processing infrastructure across the astronomical community and beyond.

---------------------------------------------------------
Title: Operational Support for Instrument Stability through ODI-PPA
    Metadata Visualization and Analysis
Authors: Young, M. D.; Hayashi, S.; Gopu, A.; Kotulla, R.; Harbeck,
   D.; Liu, W.
2015ASPC..495..181Y    Altcode: 2015adass..24..181Y
  Over long time scales, quality assurance metrics taken from calibration
  and calibrated data products can aid observatory operations in
  quantifying the performance and stability of the instrument, and
  identify potential areas of concern or guide troubleshooting and
  engineering efforts. Such methods traditionally require manual SQL
  entries, assuming the requisite metadata has even been ingested
  into a database. With the ODI-PPA system, QA metadata has been
  harvested and indexed for all data products produced over the life
  of the instrument. In this paper we will describe how, utilizing
  the industry standard Highcharts Javascript charting package with a
  customized AngularJS-driven user interface, we have made the process
  of visualizing the long-term behavior of these QA metadata simple and
  easily replicated. Operators can easily craft a custom query using
  the powerful and flexible ODI-PPA search interface and visualize
  the associated metadata in a variety of ways. These customized
  visualizations can be bookmarked, shared, or embedded externally,
  and will be dynamically updated as new data products enter the system,
  enabling operators to monitor the long-term health of their instrument
  with ease.

---------------------------------------------------------
Title: Fermi Large Area Telescope observation of high-energy solar
flares: constraining emission scenarios
Authors: Omodei, Nicola; Pesce-Rollins, Melissa; Petrosian, Vahe;
   Liu, Wei; Rubio da Costa, Fatima
2015IAUGA..2255415O    Altcode:
  The Fermi Large Area Telescope (LAT) is the most sensitive instrument
  ever deployed in space for observing gamma-ray emission &gt;100
  MeV. This has also been demonstrated by its detection of quiescent
  gamma-ray emission from pions produced by cosmic-ray protons
  interacting in the solar atmosphere, and from cosmic-ray electron
  interactions with solar optical photons. The Fermi LAT has also
  detected high-energy gamma-ray emission associated with GOES M-class
  and X-class X-ray flares, each accompanied by a coronal mass ejection
  and a solar energetic particle event increasing the number of detected
  solar flares by almost a factor of 10 with respect to previous space
  observations. During the impulsive phase, gamma rays with energies up
  to several hundreds of MeV have been recorded by the LAT. Emission up
  to GeV energies lasting several hours after the flare has also been
  recorded by the LAT. Of particular interest are the recent detections
  of two solar flares whose position behind the limb was confirmed by
  the STEREO-B satellite. While gamma-ray emission up to tens of MeV
  resulting from proton interactions has been detected before from
  occulted solar flares, the significance of these particular events
  lies in the fact that these are the first detections of &gt;100 MeV
  gamma-ray emission from footpoint-occulted flares. We will present the
  Fermi-LAT, RHESSI and STEREO observations of these flares and discuss
  the various emission scenarios for these sources.

---------------------------------------------------------
Title: Dipole tilt angle effect on magnetic reconnection locations
    on the magnetopause
Authors: Zhu, C. B.; Zhang, H.; Ge, Y. S.; Pu, Z. Y.; Liu, W. L.;
   Wan, W. X.; Liu, L. B.; Chen, Y. D.; Le, H. J.; Wang, Y. F.
2015JGRA..120.5344Z    Altcode:
  Plasma energy dispersion properties inside reconnection jet flows
  observed inside the low-latitude boundary layer are used to determine
  the distances of observing satellites to reconnection sites. The
  locations of the reconnection sites are then retrieved by tracing
  the modeled field lines by those distances. The controlling effects
  of the dipole tilt angle to the location of X lines or reconnection
  sites are investigated. Our results show that the Earth's dipole tilt
  angles strongly modify the location of X lines predicted by Cooling et
  al's model, which is thought to be the result of magnetopause reshaping
  due to finite dipole tilt angles.

---------------------------------------------------------
Title: Fermi Large Area Telescope observations of high-energy
    gamma-ray emission from behind-the-limb solar flares
Authors: Pesce-Rollins, M.; Omodei, N.; Petrosian, V.; Liu, W.;
   Rubio da Costa, F.; Allafort, A.; Fermi-LAT Collaboration
2015ICRC...34..128P    Altcode: 2015arXiv150704303P; 2015PoS...236..128P
  Fermi-LAT &gt;30 MeV observations have increased the number of detected
  solar flares by almost a factor of 10 with respect to previous space
  observations. These sample both the impulsive and long duration phases
  of GOES M and X class flares. Of particular interest is the recent
  detections of three solar flares whose position behind the limb was
  confirmed by the STEREO-B spacecraft. While gamma-ray emission up to
  tens of MeV resulting from proton interactions has been detected before
  from occulted solar flares, the significance of these particular events
  lies in the fact that these are the first detections of &gt;100 MeV
  gamma-ray emission from footpoint-occulted flares. We will present the
  Fermi-LAT, RHESSI and STEREO observations of these flares and discuss
  the various emission scenarios for these sources and implications for
  the particle acceleration mechanisms.

---------------------------------------------------------
Title: First Detection of &amp;gt100 MeV Gamma Rays Associated with
    a Behind-the-limb Solar Flare
Authors: Pesce-Rollins, M.; Omodei, N.; Petrosian, V.; Liu, Wei;
   Rubio da Costa, Fatima; Allafort, A.; Chen, Qingrong
2015ApJ...805L..15P    Altcode: 2015arXiv150503480P
  We report the first detection of &gt;100 MeV gamma-rays associated with
  a behind-the-limb solar flare, which presents a unique opportunity to
  probe the underlying physics of high-energy flare emission and particle
  acceleration. On 2013 October 11 a GOES M1.5 class solar flare occurred
  ∼9.°9 behind the solar limb as observed by STEREO-B. RHESSI observed
  hard X-ray (HXR) emission above the limb, most likely from the flare
  loop-top, as the footpoints were occulted. Surprisingly, the Fermi Large
  Area Telescope (LAT) detected &gt;100 MeV gamma-rays for ∼30 minutes
  with energies up to 3 GeV. The LAT emission centroid is consistent
  with the RHESSI HXR source, but its uncertainty does not constrain the
  source to be located there. The gamma-ray spectra can be adequately
  described by bremsstrahlung radiation from relativistic electrons having
  a relatively hard power-law (PL) spectrum with a high-energy exponential
  cutoff, or by the decay of pions produced by accelerated protons and
  ions with an isotropic pitch-angle distribution and a PL spectrum with
  a number index of ∼3.8. We show that high optical depths rule out
  the gamma-rays originating from the flare site and a high-corona trap
  model requires very unusual conditions, so a scenario in which some
  of the particles accelerated by the CME shock travel to the visible
  side of the Sun to produce the observed gamma-rays may be at work.

---------------------------------------------------------
Title: Numerical simulation of radio signal from extended air showers
Authors: Liu, Wei; Chen, Xuelei
2015RAA....15..623L    Altcode: 2014arXiv1408.2234L
  The burst of radio emission by an extensive air shower provides a
  promising alternative for detecting ultra-high energy cosmic rays. We
  have developed an independent numerical program to simulate these
  radio signals. Our code is based on a microscopic treatment, with
  both the geosynchrotron radiation and charge included. Here we give
  the first presentation of our basic program and its results. When
  the time-domain signals for different polarizations are computed,
  we find that the pulses take on a bipolar pattern and the spectrum is
  suppressed towards the lower frequencies. We investigate how showers at
  different heights in the atmosphere contribute to the total signal, and
  examine the signal strength and distribution at sites with different
  elevations. We also study the signal from showers with different
  inclination angles and azimuth directions. In all these cases we find
  the charge excess effect is important. <P />Supported by the National
  Natural Science Foundation of China.

---------------------------------------------------------
Title: Solar Flare Chromospheric Line Emission: Comparison Between
    IBIS High-resolution Observations and Radiative Hydrodynamic
    Simulations
Authors: Rubio da Costa, Fatima; Kleint, Lucia; Petrosian, Vahé;
   Sainz Dalda, Alberto; Liu, Wei
2015ApJ...804...56R    Altcode: 2015ApJ...804...56D; 2014arXiv1412.1815R
  Solar flares involve impulsive energy release, which results in enhanced
  radiation over a broad spectral range and a wide range of heights. In
  particular, line emission from the chromosphere can provide critical
  diagnostics of plasma heating processes. Thus, a direct comparison
  between high-resolution spectroscopic observations and advanced
  numerical modeling results could be extremely valuable, but has not
  yet been attempted. In this paper, we present such a self-consistent
  investigation of an M3.0 flare observed by the Dunn Solar Telescope’s
  Interferometric Bi-dimensional Spectrometer (IBIS) on 2011 September 24
  which we have modeled using the radiative hydrodynamic code RADYN. We
  obtained images and spectra of the flaring region with IBIS in Hα
  6563 Å and Ca ii 8542 Å, and with RHESSI in X-rays. The latter
  observations were used to infer the non-thermal electron population,
  which was passed to RADYN to simulate the atmospheric response to
  electron collisional heating. We then synthesized spectral lines and
  compared their shapes and intensities to those observed by IBIS and
  found a general agreement. In particular, the synthetic Ca ii 8542
  Å profile fits well to the observed profile, while the synthetic Hα
  profile is fainter in the core than for the observation. This indicates
  that Hα emission is more responsive to the non-thermal electron flux
  than the Ca ii 8542 Å emission. We suggest that it is necessary to
  refine the energy input and other processes to resolve this discrepancy.

---------------------------------------------------------
Title: Simultaneous field-aligned currents at Swarm and Cluster
    satellites
Authors: Dunlop, M. W.; Yang, J. -Y.; Yang, Y. -Y.; Xiong, C.; Lühr,
   H.; Bogdanova, Y. V.; Shen, C.; Olsen, N.; Zhang, Q. -H.; Cao,
   J. -B.; Fu, H. -S.; Liu, W. -L.; Carr, C. M.; Ritter, P.; Masson,
   A.; Haagmans, R.
2015GeoRL..42.3683D    Altcode:
  We show for the first time, with direct, multispacecraft calculations
  of electric current density, and other methods, matched signatures
  of field-aligned currents (FACs) sampled simultaneously near the
  ionosphere at low (~500 km altitude) orbit and in the magnetosphere at
  medium (~2.5 R<SUB>E</SUB> altitude) orbits using a particular Swarm
  and Cluster conjunction. The Cluster signatures are interpreted and
  ordered through joint mapping of the ground/magnetospheric footprints
  and estimation of the auroral zone boundaries (taken as indication
  of the boundaries of Region 1 and Region 2 currents). We find clear
  evidence of both small-scale and large-scale FACs and clear matching of
  the behavior and structure of the large-scale currents at both Cluster
  and Swarm. The methodology is made possible through the joint operations
  of Cluster and Swarm, which contain, in the first several months of
  Swarm operations, a number of close three-spacecraft configurations.

---------------------------------------------------------
Title: Connecting the evolution and properties of CMEs to their low
    coronal signatures. A modeling case study of the ‘simple’ Feb
    13 2009 event
Authors: Downs, Cooper; Török, Tibor; Titov, Viacheslav; Liu, Wei;
   Linker, Jon; Mikić, Zoran
2015TESS....130401D    Altcode:
  The early onset and and evolution of a CME is a process that features
  an intimate coupling between the erupting flux-system and the
  ambient corona. For this reason low coronal signatures that we often
  observe in the EUV can be used to infer information on the physical
  nature and evolution of CMEs. In this presentation we will discuss
  a 3D thermodynamic MHD simulation of the Feb 13 2009 eruption,
  which occurred from an isolated region during solar minimum and
  produced well characterized EUV wave and transient coronal dimming
  features. Using observations as a guide, we simulate the entire
  evolution of the eruption and global corona, starting from the initial
  stable configuration through onset and evolution to the post-eruptive
  reconfiguration. With a particular focus on coronal dimmings, we
  track how the connectivity of the erupting flux-rope evolves with
  time and how this relates to corresponding dimmings in synthetic EUV
  observables. We find that the appearance of the core dimming regions
  and their migration over time can be related to when and where the
  erupting rope reconnects with itself and the adjacent arcade. Other
  aspects related to CME evolution, such as the generation of an EUV
  wave and quasi-periodic fast-propagating waves are also discussed.

---------------------------------------------------------
Title: Observations and Interpretation of Behind the Limb Solar
    Flares Detected by Fermi-LAT and Other Instruments
Authors: Petrosian, Vahe; Omodei, Nicola; Pesce-Rollins, Melissa;
   Rubio da Costa, Fatima; Liu, Wei
2015TESS....120505P    Altcode:
  The Fermi Large Area Telescope (LAT) is the most sensitive instrument
  ever deployed in space for observing &gt; 30 MeV gamma-rays. During the
  past active period of the Sun the LAT has detected more than 40 flares
  up to GeV energies some of which occur behind the limb as determined
  by STEREO observations. We will present the observations on two such
  flares with significant flux of &gt; 100 MeV (and some indication of
  1 to 10 MeV detected by Fermi-GBM) gamma-rays coming from the visible
  disk while the flare and associated CMEs are initiated in active regions
  tens of degrees behind the visible limb of the Sun. We will consider
  acceleration of particles, their transport and radiative signatures, and
  the transfer of these radiation in the solar atmosphere to distinguish
  between (i) acceleration in the low corona, in a high corona trap,
  and/or in the CME driven shock; (ii) between continuous and prompt
  acceleration; and (iii) between electron bremsstrahlung and decay of
  pions produced by accelerated ions.

---------------------------------------------------------
Title: First High-resolution Spectroscopic Observations of an Erupting
    Prominence Within a Coronal Mass Ejection by the Interface Region
    Imaging Spectrograph (IRIS)
Authors: Liu, Wei; De Pontieu, Bart; Vial, Jean-Claude; Title, Alan
   M.; Carlsson, Mats; Uitenbroek, Han; Okamoto, Takenori J.; Berger,
   Thomas E.; Antolin, Patrick
2015ApJ...803...85L    Altcode: 2015arXiv150204738L
  Spectroscopic observations of prominence eruptions associated with
  coronal mass ejections (CMEs), although relatively rare, can provide
  valuable plasma and three-dimensional geometry diagnostics. We report
  the first observations by the Interface Region Imaging Spectrograph
  mission of a spectacular fast CME/prominence eruption associated with
  an equivalent X1.6 flare on 2014 May 9. The maximum plane-of-sky and
  Doppler velocities of the eruption are 1200 and 460 km s<SUP>-1</SUP>,
  respectively. There are two eruption components separated by ∼200
  km s<SUP>-1</SUP> in Doppler velocity: a primary, bright component
  and a secondary, faint component, suggesting a hollow, rather than
  solid, cone-shaped distribution of material. The eruption involves
  a left-handed helical structure undergoing counterclockwise (viewed
  top-down) unwinding motion. There is a temporal evolution from upward
  eruption to downward fallback with less-than-free-fall speeds and
  decreasing nonthermal line widths. We find a wide range of Mg ii k/h
  line intensity ratios (less than ∼2 expected for optically-thin
  thermal emission): the lowest ever reported median value of 1.17
  found in the fallback material, a comparably high value of 1.63 in
  nearby coronal rain, and intermediate values of 1.53 and 1.41 in
  the two eruption components. The fallback material exhibits a strong
  (\gt 5σ ) linear correlation between the k/h ratio and the Doppler
  velocity as well as the line intensity. We demonstrate that Doppler
  dimming of scattered chromospheric emission by the erupted material
  can potentially explain such characteristics.

---------------------------------------------------------
Title: VizieR Online Data Catalog: HeI* in broad absorption line QSOs
    (Liu+, 2015)
Authors: Liu, W. -J.; Zhou, H.; Ji, T.; Yuan, W.; Wang, T. -G.; Jian,
   G.; Shi, X.; Zhang, S.; Jiang, P.; Shu, X.; Wang, H.; Wang, S. -F.;
   Sun, L.; Yang, C.; Liu, B.; Zhao, W.
2015yCat..22170011L    Altcode:
  Neutral helium multiplets, HeI*λλ3189, 3889, 10830, are very
  useful diagnostics for the geometry and physical conditions of the
  absorbing gas in quasars. So far only a handful of HeI* detections
  have been reported. Using a newly developed method, we detected the
  HeI*λ3889 absorption line in 101 sources of a well-defined sample
  of 285 MgII broad absorption line (BAL) quasars selected from SDSS
  DR5. This has increased the number of HeI* BAL quasars by more than
  one order of magnitude. We further detected HeI*λ3189 in 50% (52/101)
  of the quasars in the sample. The detection fraction of HeI* BALs in
  MgII BAL quasars is ~35% as a whole, and it increases dramatically
  with increasing spectral signal-to-noise ratio (S/N), from ~18% at
  S/N&lt;=10 to ~93% at S/N&gt;=35. This suggests that HeI* BALs could
  be detected in most MgII LoBAL quasars, provided the spectra S/N is
  high enough. Such a surprisingly high HeI* BAL fraction is actually
  predicted from photoionization calculations based on a simple BAL
  model. The result indicates that HeI* absorption lines can be used
  to search for BAL quasars at low z, which cannot be identified by
  ground-based optical spectroscopic surveys with commonly seen UV
  absorption lines. Using HeI*λ3889, we discovered 19 BAL quasars at
  z&lt;0.3 from the available SDSS spectral database. The fraction of HeI*
  BAL quasars is similar to that of LoBAL objects. <P />(7 data files).

---------------------------------------------------------
Title: Shedding new light on the Sun with the Fermi LAT
Authors: Omodei, N.; Petrosian, V.; Liu, W.; Rubio da Costa, F.;
   Chen, Q.; Pesce-Rollins, M.; Grove, E.; Longo, F.
2015arXiv150203895O    Altcode:
  During its first six years of operation, the Fermi Large Area Telescope
  (LAT) has detected &gt;30 MeV gamma-ray emission from more than
  40 solar flares, nearly a factor of 10 more than those detected by
  EGRET. These include detections of impulsive and sustained emissions,
  extending up to 20 hours in the case of the 2012 March 7 X-class
  flares. We will present an overview of solar flare detections with
  LAT, highlighting recent results and surprising features, including
  the detection of &gt;100 MeV emission associated with flares located
  behind the limb. Such flares may shed new light on the relationship
  between the sites of particle acceleration and gamma-ray emission.

---------------------------------------------------------
Title: An Unobscured Type II Quasar Candidate: SDSS
    J012032.19-005501.9
Authors: Li, Y.; Yuan, W.; Zhou, H. Y.; Komossa, S.; Ai, Y. L.; Liu,
   W. J.; Boisvert, J. H.
2015AJ....149...75L    Altcode: 2014arXiv1412.2776L
  We report the finding of an unobscured type II active galactic nucleus
  (AGN) candidate, SDSS J012032.19-005501.9, at a relatively high
  redshift of 0.601, which shows a number of unusual properties. It
  varies significantly on timescales of years, typical of type I AGNs,
  and marginally on timescales of weeks. The color-magnitude relation
  and the structure function are also consistent with that of type I
  AGNs, which implies that its variability likely originates from the
  black hole accretion system. However, no broad emission line (BEL) is
  detected in the Sloan Digital Sky Survey spectrum, and the upper limit
  of the equivalent width of the Hβ BEL is much less than that of type I
  AGNs. These properties suggest that SDSS J012032.19-005501.9 may be an
  unobscured quasar without intrinsically broad emission lines, namely,
  an unobscured type II AGN or “true” type II AGN. Furthermore,
  its continuum luminosity is at least one order of magnitude fainter
  than the average value over the past century from the [O iii] emission
  line. This indicates that SDSS J012032.19-005501.9 may be switching
  off. Additional possible scenarios to explain this intriguing source
  are also discussed. Future deep observations at multiwavelengths are
  needed to reveal the nature of this peculiar and intriguing AGN.

---------------------------------------------------------
Title: TeV cosmic-ray proton and helium spectra in the myriad model II
Authors: Liu, Wei; Salati, Pierre; Chen, Xuelei
2015RAA....15...15L    Altcode: 2014arXiv1405.2835L
  Recent observations show that the spectra of cosmic ray nuclei start to
  harden above ~ 10<SUP>2</SUP> GeV, which contradicts the conventional
  steady-state cosmic ray model. We had suggested that this anomaly
  is due to the propagation effect of cosmic rays released from local
  young cosmic ray sources; the total flux of cosmic rays should be
  computed with the Myriad Model, where a contribution from sources
  in the local catalog is added to the background. However, although
  the hardening could be elegantly explained in this model, the model
  parameters obtained from the fit are skewed toward a region with fast
  diffusion and a low supernova rate in the Galaxy, in disagreement with
  other observations. We further explore this model in order to set up
  a concordant picture. Two possible improvements related to cosmic ray
  sources are considered. First, instead of the usual axisymmetric disk
  model, we examine a spiral model for the source distribution. Second,
  for nearby and young sources which are necessary to explain the
  hardening, we allow for an energy-dependent escape. We find that a
  major improvement comes from incorporating an energy-dependent escape
  time for local sources, and with both modifications not only are the
  cosmic ray proton and helium anomalies resolved, but also the parameters
  attain values in a reasonable range compatible with other analyses.

---------------------------------------------------------
Title: Instant: An Innovative L5 Small Mission Concept for Coordinated
    Science with Solar Orbiter and Solar Probe Plus
Authors: Lavraud, B.; Liu, Y. D.; Harrison, R. A.; Liu, W.;
   Auchere, F.; Gan, W.; Lamy, P. L.; Xia, L.; Eastwood, J. P.;
   Wimmer-Schweingruber, R. F.; Zong, Q.; Rochus, P.; Maksimovic, M.;
   Temmer, M.; Escoubet, C. P.; Kilpua, E.; Rouillard, A. P.; Davies,
   J. A.; Vial, J. C.; Gopalswamy, N.; Bale, S. D.; Li, G.; Howard,
   T. A.; DeForest, C. E.
2014AGUFMSH21B4109L    Altcode:
  We will present both the science objectives and related instrumentation
  of a small solar and heliospheric mission concept, INSTANT:
  INvestigation of Solar-Terrestrial Activity aNd Transients. It will be
  submitted as an opportunity to the upcoming ESA-China S-class mission
  call later this year. This concept was conceived to allow innovative
  measurements and unprecedented, early determination of key properties
  of Earthbound CMEs from the L5 vantage point. Innovative measurements
  will include magnetic field determination in the corona thanks to
  Hanle measurement in Lyman-α and polarized heliospheric imaging
  for accurate determination of CME trajectories. With complementary
  in situ measurements, it will uniquely permit solar storm science,
  solar storm surveillance, and synergy with Solar Orbiter and Solar
  Probe Plus (the ESA-China S2 mission launch is planned in 2021).

---------------------------------------------------------
Title: The Relation Between Large-Scale Coronal Propagating Fronts
    and Type II Radio Bursts
Authors: Nitta, Nariaki V.; Liu, Wei; Gopalswamy, Nat; Yashiro, Seiji
2014SoPh..289.4589N    Altcode: 2014arXiv1409.4754N
  Large-scale, wave-like disturbances in extreme-ultraviolet (EUV) and
  type II radio bursts are often associated with coronal mass ejections
  (CMEs). Both phenomena may signify shock waves driven by CMEs. Taking
  EUV full-disk images at an unprecedented cadence, the Atmospheric
  Imaging Assembly (AIA) onboard the Solar Dynamics Observatory has
  observed the so-called EIT waves or large-scale coronal propagating
  fronts (LCPFs) from their early evolution, which coincides with the
  period when most metric type II bursts occur. This article discusses the
  relation of LCPFs as captured by AIA with metric type II bursts. We show
  examples of type II bursts without a clear LCPF and fast LCPFs without
  a type II burst. Part of the disconnect between the two phenomena may
  be due to the difficulty in identifying them objectively. Furthermore,
  it is possible that the individual LCPFs and type II bursts may reflect
  different physical processes and external factors. In particular,
  the type II bursts that start at low frequencies and high altitudes
  tend to accompany an extended arc-shaped feature, which probably
  represents the 3D structure of the CME and the shock wave around it,
  and not just its near-surface track, which has usually been identified
  with EIT waves. This feature expands and propagates toward and beyond
  the limb. These events may be characterized by stretching of field
  lines in the radial direction and may be distinct from other LCPFs,
  which may be explained in terms of sudden lateral expansion of the
  coronal volume. Neither LCPFs nor type II bursts by themselves serve
  as necessary conditions for coronal shock waves, but these phenomena
  may provide useful information on the early evolution of the shock
  waves in 3D when both are clearly identified in eruptive events.

---------------------------------------------------------
Title: Imaging and Spectroscopic Observations of Magnetic Reconnection
    and Chromospheric Evaporation in a Solar Flare
Authors: Tian, Hui; Li, Gang; Reeves, Katharine K.; Raymond, John C.;
   Guo, Fan; Liu, Wei; Chen, Bin; Murphy, Nicholas A.
2014ApJ...797L..14T    Altcode: 2014arXiv1411.2301T
  Magnetic reconnection is believed to be the dominant energy release
  mechanism in solar flares. The standard flare model predicts both
  downward and upward outflow plasmas with speeds close to the coronal
  Alfvén speed. Yet, spectroscopic observations of such outflows,
  especially the downflows, are extremely rare. With observations of
  the newly launched Interface Region Imaging Spectrograph (IRIS), we
  report the detection of a greatly redshifted (~125 km s<SUP>-1</SUP>
  along the line of sight) Fe XXI 1354.08 Å emission line with a ~100 km
  s<SUP>-1</SUP> nonthermal width at the reconnection site of a flare. The
  redshifted Fe XXI feature coincides spatially with the loop-top
  X-ray source observed by RHESSI. We interpret this large redshift as
  the signature of downward-moving reconnection outflow/hot retracting
  loops. Imaging observations from both IRIS and the Atmospheric Imaging
  Assembly (AIA) on board the Solar Dynamics Observatory also reveal
  the eruption and reconnection processes. Fast downward-propagating
  blobs along these loops are also found from cool emission lines (e.g.,
  Si IV, O IV, C II, Mg II) and images of AIA and IRIS. Furthermore,
  the entire Fe XXI line is blueshifted by ~260 km s<SUP>-1</SUP> at
  the loop footpoints, where the cool lines mentioned above all exhibit
  obvious redshift, a result that is consistent with the scenario of
  chromospheric evaporation induced by downward-propagating nonthermal
  electrons from the reconnection site.

---------------------------------------------------------
Title: Comparison between IBIS Observations and Radiative Transfer
    Hydrodynamic Simulations of a Solar Flare
Authors: Rubio da Costa, F.; Kleint, L.; Liu, W.; Sainz Dalda, A.;
   Petrosian, V.
2014AGUFMSH13B4104R    Altcode:
  High-resolution spectroscopic observations of solar flares are
  rare but can provide valuable diagnostics. On September 24, 2011 an
  M3.0 class flare was observed by the Interferometric BIdimensional
  Spectropolarimeter (IBIS) in chromospheric Hα and CaII 8542 Å
  lines and by the Reuven Ramaty High Energy Solar Spectroscopic Imager
  (RHESSI) in X-rays. We fitted the RHESSI spectra at different times
  with a power-law plus isothermal component. We then used the fitted
  real-time spectral parameters of nonthermal electrons as the input to
  the RADYN radiative hydrodynamic code (Carlsson et al, 1992, 1996;
  Allred et al, 2005) to simulate the low-chromospheric response to
  collisional heating by energetic electrons. We synthesized both the
  Hα and CaII 8542 Å lines from the simulation results and compare
  them with the IBIS observations. We discuss the constraints from this
  comparison on particle acceleration mechanisms in solar flares.

---------------------------------------------------------
Title: Coronal Extreme Ultraviolet (EUV) Waves and Their Seismological
    Applications
Authors: Liu, W.; Ofman, L.
2014AGUFMSH23C..01L    Altcode:
  Magnetohydrodynamic (MHD) waves can be used as seismological tools
  to probe the physical conditions of the solar corona, including its
  magnetic field and plasma parameters. Recent high cadence and full-disk
  imaging observations in extreme ultraviolet (EUV) by the Atmospheric
  Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO)
  have opened a new chapter in understanding these waves and utilizing
  them for coronal seismology. We will review such new observations,
  focusing on two intimately related phenomena - global EUV waves
  (so-called "EIT waves") associated with coronal mass ejections (CMEs)
  and quasi-periodic, fast-mode magnetosonic wave trains associated
  with flares: (1) The generation and propagation of global EUV waves
  and their interaction with coronal structures, e.g., reflection and
  refraction, can provide diagnostics for the global corona in which they
  propagate, such as mapping the spatial distribution of the wave phase
  speed and thus the magnetic field strength. (2) AIA-detected fast-mode
  wave trains are closely correlated with flare pulsations seen from
  radio to hard X-rays and propagate at typically 500-2000 km/s along
  funnel-shaped waveguides often located within CME bubbles. They can
  provide diagnostics for flare energy release mechanisms and the local
  corona around the flaring active region. We will discuss the roles
  of such waves in energy transport within the solar atmosphere and in
  their associated CME/flare eruptions.

---------------------------------------------------------
Title: First High-resolution Spectroscopic Observations by IRIS
    of a Fast, Helical Prominence Eruption Associated with a Coronal
    Mass Ejection
Authors: Liu, W.; De Pontieu, B.; Okamoto, T. J.; Vial, J. C.; Title,
   A. M.; Antolin, P.; Berger, T. E.; Uitenbroek, H.
2014AGUFMSH11D..04L    Altcode:
  High-resolution spectroscopic observations of prominence eruptions and
  associated coronal mass ejections (CMEs) are rare but can provide
  valuable plasma and energy diagnostics. New opportunities have
  recently become available with the advent of the Interface Region
  Imaging Spectrograph (IRIS) mission equipped with high resolution of
  0.33-0.4 arcsec in space and 1 km/s in velocity, together with the
  Hinode Solar Optical Telescope of 0.2 arcsec spatial resolution. We
  report the first result of joint IRIS-Hinode observations of a
  spectacular prominence eruption occurring on 2014-May-09. IRIS
  detected a maximum redshift of 450 km/s, which, combined with the
  plane-of-sky speed of 800 km/s, gives a large velocity vector of 920
  km/s at 30 degrees from the sky plane. This direction agrees with the
  source location at 30 degrees behind the limb observed by STEREO-A
  and indicates a nearly vertical ejection. We found two branches of
  redshifts separated by 200 km/s appearing in all strong lines at
  chromospheric to transition-region temperatures, including Mg II k/h,
  C II, and Si IV, suggesting a hollow, rather than solid, cone in the
  velocity space of the ejected material. Opposite blue- and redshifts
  on the two sides of the prominence exhibit corkscrew variations both
  in space and time, suggestive of unwinding rotations of a left-handed
  helical flux rope. Some erupted material returns as nearly streamline
  flows, exhibiting distinctly narrow line widths (~10 km/s), about
  50% of those of the nearby coronal rain at the apexes of coronal
  loops, where the rain material is initially formed out of cooling
  condensation. We estimate the mass and kinetic energy of the ejected
  and returning material and compare them with those of the associated
  CME. We will discuss the implications of these observations for CME
  initiation mechanisms.

---------------------------------------------------------
Title: Whistler-mode waves inside flux pileup region: Structured
    or unstructured?
Authors: Fu, H. S.; Cao, J. B.; Cully, C. M.; Khotyaintsev,
   Y. V.; Vaivads, A.; Angelopoulos, V.; Zong, Q. -G.; Santolík, O.;
   Macúšová, E.; André, M.; Liu, W. L.; Lu, H. Y.; Zhou, M.; Huang,
   S. Y.; Zhima, Z.
2014JGRA..119.9089F    Altcode:
  During reconnection, a flux pileup region (FPR) is formed behind a
  dipolarization front in an outflow jet. Inside the FPR, the magnetic
  field magnitude and Bz component increase and the whistler-mode waves
  are observed frequently. As the FPR convects toward the Earth during
  substorms, it is obstructed by the dipolar geomagnetic field to form
  a near-Earth FPR. Unlike the structureless emissions inside the tail
  FPR, we find that the whistler-mode waves inside the near-Earth FPR
  can exhibit a discrete structure similar to chorus. Both upper band
  and lower band chorus are observed, with the upper band having a
  larger propagation angle (and smaller wave amplitude) than the lower
  band. Most chorus elements we observed are "rising-tone" type, but
  some are "falling-tone" type. We notice that the rising-tone chorus
  can evolve into falling-tone chorus within &lt;3 s. One of the factors
  that may explain why the waves are unstructured inside the tail FPR but
  become discrete inside the near-Earth FPR is the spatial inhomogeneity
  of magnetic field: we find that such inhomogeneity is small inside
  the near-Earth FPR but large inside the tail FPR.

---------------------------------------------------------
Title: Multi-fluid Model of a Sun-grazing Comet in the Rapidly
    Ionizing, Magnetized Low Corona
Authors: Jia, Y. -D.; Russell, C. T.; Liu, W.; Shou, Y. S.
2014ApJ...796...42J    Altcode:
  Two Sun-grazing comets were recently imaged in the low solar corona
  by space telescopes in unprecedented detail, revealing a wide range
  of new phenomena. This sparked growing interest in the interaction of
  comets with the coronal plasma and magnetic field and their diagnostic
  potential as solar probes. However, interpretation of such rich
  observational data requires profound understanding of relevant physical
  processes in an unexplored regime. Here advanced numerical modeling
  can provide critical clues. To this end, we present a prototype,
  multi-fluid, magnetohydrodynamic model of a steady-state comet in
  the low solar corona. These simulation results are compared with
  previously modeled comets in the solar wind environment. By inspecting
  their projection and column densities, we find a dominance of O<SUP>6
  +</SUP> ions in the cometary tail, which can explain the observed
  extreme ultraviolet emission. The tail is found to be comparable to
  recent EUV images of these comets. In addition, the comet tail appears
  wider when the observer's line of sight is perpendicular rather than
  parallel to the local magnetic field. This is opposite to the trend
  in the interplanetary space permeated in the solar wind, because the
  ratio between dynamic pressure and magnetic pressure is an order of
  magnitude smaller than at 1 AU. On the other hand, we find that iron
  ions in the comet head build up to a density comparable to that of
  oxygen ions, but are unlikely to form a visible tail because of the
  shorter mean free paths of the neutrals.

---------------------------------------------------------
Title: Evidence of nonthermal particles in coronal loops heated
    impulsively by nanoflares
Authors: Testa, P.; De Pontieu, B.; Allred, J.; Carlsson, M.; Reale,
   F.; Daw, A.; Hansteen, V.; Martinez-Sykora, J.; Liu, W.; DeLuca, E. E.;
   Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Tian, H.; Lemen, J.;
   Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.;
   Kleint, L.; Kankelborg, C.; Jaeggli, S.
2014Sci...346B.315T    Altcode: 2014arXiv1410.6130T
  The physical processes causing energy exchange between the Sun’s
  hot corona and its cool lower atmosphere remain poorly understood. The
  chromosphere and transition region (TR) form an interface region between
  the surface and the corona that is highly sensitive to the coronal
  heating mechanism. High-resolution observations with the Interface
  Region Imaging Spectrograph (IRIS) reveal rapid variability (~20 to
  60 seconds) of intensity and velocity on small spatial scales (≲500
  kilometers) at the footpoints of hot and dynamic coronal loops. The
  observations are consistent with numerical simulations of heating by
  beams of nonthermal electrons, which are generated in small impulsive
  (≲30 seconds) heating events called “coronal nanoflares.” The
  accelerated electrons deposit a sizable fraction of their energy
  (≲10<SUP>25 </SUP>erg) in the chromosphere and TR. Our analysis
  provides tight constraints on the properties of such electron beams
  and new diagnostics for their presence in the nonflaring corona.

---------------------------------------------------------
Title: Linear weakening of the AMOC in response to receding glacial
    ice sheets in CCSM3
Authors: Zhu, Jiang; Liu, Zhengyu; Zhang, Xu; Eisenman, Ian; Liu, Wei
2014GeoRL..41.6252Z    Altcode:
  The transient response of the Atlantic Meridional Overturning
  Circulation (AMOC) to a deglacial ice sheet retreat is studied using
  the Community Climate System Model version 3 (CCSM3), with a focus on
  orographic effects rather than meltwater discharge. It is found that
  the AMOC weakens significantly (41%) in response to the deglacial
  ice sheet retreat. The AMOC weakening follows the decrease of the
  Northern Hemisphere ice sheet volume linearly, with no evidence of
  abrupt thresholds. A wind-driven mechanism is proposed to explain the
  weakening of the AMOC: lowering the Northern Hemisphere ice sheets
  induces a northward shift of the westerlies, which causes a rapid
  eastward sea ice transport and expanded sea ice cover over the subpolar
  North Atlantic; this expanded sea ice insulates the ocean from heat
  loss and leads to suppressed deep convection and a weakened AMOC. A
  sea ice-ocean positive feedback could be further established between
  the AMOC decrease and sea ice expansion.

---------------------------------------------------------
Title: Hawking Radiations from an Arbitrarily Accelerating Kerr
    Black Hole
Authors: Yang, Xue-Jun; Zhang, Yan-Nv; Liu, Wei
2014JApA...35..559Y    Altcode: 2014JApA..tmp...38Y
  The Hawking radiation from an arbitrarily accelerating Kerr black hole
  is calculated by using a new tortoise coordinate transformation and
  the improved Damour-Ruffini method.

---------------------------------------------------------
Title: γ-Rays Radiation of High Redshift Fermi Blazars
Authors: Liu, W. G.; Fu, S. H.; Zhang, X.; Ma, L.; Li, Y. B.; Xiong,
   D. R.
2014JApA...35..349L    Altcode: 2014JApA..tmp...65L
  Based on the 31 high redshift ( z &gt; 2) Flat Spectral Radio Quasars
  (FSRQs), which is from the second Fermi-LAT AGNs catalogue (2LAC),
  we studied the correlation between flux densities ( F <SUB>R</SUB>,
  F <SUB>K</SUB>, F γ) in the radio, infrared and γ-ray wave bands. We
  found that there is a significant positive correlation between F <SUB>
  γ </SUB> and F <SUB>R</SUB>, and a weak anticorrelation between F<SUB>
  γ </SUB> and F<SUB>K</SUB> in the average state. For high redshift
  blazars, we argue that the seed photon of γ-ray emission mainly comes
  from the jet itself and partially from the dusty torus.

---------------------------------------------------------
Title: Hawking Temperature of an Arbitrarily Accelerating Black Hole
Authors: Pan, Wei-Zhen; Liu, Wei
2014JApA...35..533P    Altcode: 2014JApA..tmp...94P
  Hawking temperature of an arbitrarily accelerating black hole
  with electric and magnetic charges are obtained based on the
  Klein-Gordon equation with a correct-dimension new tortoise coordinate
  transformation.

---------------------------------------------------------
Title: Advances in Observing Various Coronal EUV Waves in the SDO
    Era and Their Seismological Applications (Invited Review)
Authors: Liu, Wei; Ofman, Leon
2014SoPh..289.3233L    Altcode: 2014SoPh..tmp...67L; 2014arXiv1404.0670L
  Global extreme-ultraviolet (EUV) waves are spectacular traveling
  disturbances in the solar corona associated with energetic eruptions
  such as coronal mass ejections (CMEs) and flares. Over the past
  15 years, observations from three generations of space-borne EUV
  telescopes have shaped our understanding of this phenomenon and at
  the same time led to controversy about its physical nature. Since its
  launch in 2010, the Atmospheric Imaging Assembly (AIA) onboard the
  Solar Dynamics Observatory (SDO) has observed more than 210 global
  EUV waves in exquisite detail, thanks to its high spatio-temporal
  resolution and full-disk, wide-temperature coverage. A combination of
  statistical analysis of this large sample, more than 30 detailed case
  studies, and data-driven MHD modeling, has been leading their physical
  interpretations to a convergence, favoring a bimodal composition
  of an outer, fast-mode magnetosonic wave component and an inner,
  non-wave CME component. Adding to this multifaceted picture, AIA has
  also discovered new EUV wave and wave-like phenomena associated with
  various eruptions, including quasi-periodic fast propagating (QFP)
  wave trains, magnetic Kelvin-Helmholtz instabilities (KHI) in the
  corona and associated nonlinear waves, and a variety of mini-EUV
  waves. Seismological applications using such waves are now being
  actively pursued, especially for the global corona. We review such
  advances in EUV wave research focusing on recent SDO/AIA observations,
  their seismological applications, related data-analysis techniques,
  and numerical and analytical models.

---------------------------------------------------------
Title: Three-dimensional lunar wake reconstructed from ARTEMIS data
Authors: Zhang, H.; Khurana, K. K.; Kivelson, M. G.; Angelopoulos, V.;
   Wan, W. X.; Liu, L. B.; Zong, Q. -G.; Pu, Z. Y.; Shi, Q. Q.; Liu, W. L.
2014JGRA..119.5220Z    Altcode:
  Data from the two-spacecraft Acceleration, Reconnection, Turbulence
  and Electrodynamics of the Moon's Interaction with the Sun mission
  to the Moon have been exploited to characterize the lunar wake
  with unprecedented fidelity. The differences between measurements
  made by a spacecraft in the solar wind very near the Moon and
  concurrent measurements made by a second spacecraft in the near
  lunar wake are small but systematic. They enabled us to establish the
  perturbations of plasma density, temperature, thermal, magnetic and
  total pressure, field, and flow downstream of the Moon to distances of
  12 lunar radii (R<SUB>M</SUB>). The wake disturbances are initiated
  immediately behind the Moon by the diamagnetic currents at the lunar
  terminator. Rarefaction waves propagate outward at fast MHD wave
  velocities. Beyond ~6.5 R<SUB>M</SUB>, all plasma and field parameters
  are poorly structured which suggests the presence of instabilities
  excited by counter-streaming particles. Inward flowing plasma
  accelerated through pressure gradient force and ambipolar electric
  field compresses the magnetic field and leads to continuous increase in
  magnitude of magnetic perturbations. Besides the downstream distance,
  the field perturbation magnitude is also a function of the solar wind
  ion beta and the angle between the solar wind and the interplanetary
  magnetic field (IMF). Both ion and electron temperatures increase
  as a consequence of an energy dispersion effect, whose explanation
  requires fully kinetic models. Downstream of the Moon, the IMF field
  lines are observed to bulge toward the Moon, which is unexpected and
  may be caused by a plasma pressure gradient force or/and the pickup
  of heavy charged dust grains behind the Moon.

---------------------------------------------------------
Title: Thermochemical sulphate reduction (TSR) versus maturation
    and their effects on hydrogen stable isotopes of very dry alkane gases
Authors: Liu, Q. Y.; Worden, R. H.; Jin, Z. J.; Liu, W. H.; Li, J.;
   Gao, B.; Zhang, D. W.; Hu, A. P.; Yang, C.
2014GeCoA.137..208L    Altcode:
  Here we report the first study of the effect of thermochemical sulphate
  reduction (TSR) on the hydrogen isotopes of natural gas. Variably sour
  (H<SUB>2</SUB>S-bearing) and very dry (&gt;97% methane) gas samples from
  Lower Triassic, Permian and Carboniferous marine carbonate reservoirs
  in the Sichuan Basin, China, have been analysed. All gases seem to have
  been sourced from mature marine kerogen and contain H<SUB>2</SUB>S that
  resulted from TSR. The Carboniferous samples are largely unaffected by
  TSR and were used to assess the effects of normal thermal maturation
  processes on the carbon and hydrogen isotopes of methane and ethane as
  a function of gas dryness (a proxy for thermal maturity). Maturation
  led to heavier carbon isotopes of methane and ethane and hydrogen
  isotopes of ethane; in contrast methane hydrogen isotopes seem to have
  little systematic variation with increasing maturity. TSR did not have
  a systematic effect on the hydrogen isotopes of methane, although
  the spread of values diminished (ending up at a constant -120‰)
  as TSR proceeded. This was possibly due to the partial thermochemical
  sulphate reduction of ethane adding isotopically light methane and thus
  offsetting the Rayleigh fractionation effects of TSR of methane. In
  contrast, hydrogen isotopes of ethane became much heavier as TSR
  proceeded, to values greater than those for samples only influenced
  by maturation. Under some circumstances, the effects of TSR can be
  identified and discerned from the effects of normal thermal maturation
  by plotting the difference between the carbon isotope compositions of
  methane and ethane and the difference between the hydrogen isotope
  compositions of methane and ethane. <P />Do the hydrogen isotope
  ratios of alkane gases systematically vary as a function of dryness
  or sourness? <P />Do the hydrogen isotope ratios of alkane gases from
  the Carboniferous, Permian and Lower Triassic dry gas reservoirs help
  reveal the maturity and/or extent of TSR in the Sichuan Basin? <P
  />Is it possible to separate and discriminate the effects of TSR and
  non-TSR processes on alkane hydrogen isotopes in dry gas accumulations?

---------------------------------------------------------
Title: Magnetic braking of Ap/Bp stars: an alternative formation
    mechanism of compact intermediate-mass binary pulsars
Authors: Liu, Wei-Min; Chen, Wen-Cong
2014MNRAS.441.3615L    Altcode: 2014arXiv1405.0691L
  It is difficult for the intermediate-mass X-ray binaries (IMXBs)
  evolutionary channel to form intermediate-mass binary pulsars
  (IMBPs) with a short orbital period (less than 3 d) via stable mass
  transfer. The main reason is that the magnetic braking mechanisms
  are generally thought not to work for donor stars with a mass of
  greater than 1.5 M<SUB>⊙</SUB> in the canonical model. However,
  some intermediate-mass stars have anomalously strong magnetic fields
  (about 100-10 000 G), i.e. so-called Ap or Bp stars. With the coupling
  between the magnetic field and the irradiation-driven wind from the
  surface of Ap/Bp stars, a plausible magnetic braking mechanism should
  be expected. In this work, we attempt to investigate if IMXBs with
  Ap/Bp stars can produce IMBPs with a short orbital period (less than
  3 d) by such an anomalous magnetic braking mechanism. Using a stellar
  evolution code, we have simulated the evolution of a large number of
  IMXBs consisting of a neutron star (NS) and an Ap/Bp star. For the spin
  evolution of the NS, we consider the accretion torque, the propeller
  torque and the spin-down torque caused by the interaction between the
  magnetic field and the accretion disc. The calculated results show that,
  employing anomalous magnetic braking of Ap/Bp stars, IMXBs can evolve
  into compact IMBPs with short orbital periods of less than 3 d. However,
  there exists significant discrepancy between the spin periods of IMBPs
  in our simulated results and those observed.

---------------------------------------------------------
Title: The Rayleigh-Taylor Instability and the role of Prominences
    in the Chromosphere-Corona Mass Cycle
Authors: Berger, Thomas; Liu, Wei; Hillier, Andrew; Scullion, Eamon;
   Low, Boon Chye
2014AAS...22421201B    Altcode:
  We review recent results in the study of so-called "prominence
  bubbles", a buoyant instability discovered in quiescent solar
  prominences by the Hinode/SOT instrument in 2007. Analysis of the
  plasma flows along the boundary of the bubbles indicates that shear
  flows leading to Kelvin-Helmholtz instability waves can develop into
  the seed perturbations triggering the Rayleigh-Taylor instability. The
  non-linear phase of the RT instability leads to the formation of large
  turbulent plumes that transport the bubble plasma (and presumably
  magnetic flux) into the overlying coronal flux rope. We propose that
  the upward turbulent transport of hot bubble plasma and the downflows
  of cooler chromospheric plasma in the prominence are related aspects
  of a large-scale "chromosphere-corona mass cycle" in which hot plasma
  and magnetic flux and helicity from the chromosphere are transported
  upwards while the cooler prominence plasma downflows, which decouple
  from the magnetic field they are originally frozen-into, represent
  the condensation return flows of the cycle. This cycling enables a
  mechanism by which magnetic flux and helicity build up in the coronal
  flux rope while mass drains out of the flux rope, eventually triggering
  a "loss of confinement" eruption in the form of a CME.

---------------------------------------------------------
Title: Fermi Detection of Gamma-ray Emission from a Behind-the-limb
    M1.5 Flare on 2013 October 11
Authors: Pesce-Rollins, Melissa; Omodei, Nicola; Petrosian, Vahe;
   Liu, Wei; Chen, Qingrong; Rubio Da Costa, Fatima
2014shin.confE..91P    Altcode:
  On 2013 October 11 an M1.5 class solar flare erupted from the NOAA
  active region 11868, which was then behind the solar limb. RHESSI images
  reveal hard X-ray emission well above the limb, most likely from the
  top of the flare loop whose footpoints were occulted. Surprisingly the
  Fermi Large Area Telescope (LAT) detected gamma-rays up to 3 GeV for
  30 minutes from this flare, making it the first behind-the-limb flare
  observed by Fermi. The LAT gamma-ray emission centroid is consistent
  with the vicinity of the RHESSI hard X-ray source. The gamma-ray
  spectra can be adequately described by a power law with a high-energy
  exponential cutoff, or as a result of the decay of pions produced by
  accelerated protons and ions with an isotropic pitch angle distribution
  and a power-law energy spectrum. The required proton spectrum would
  have a number index of 3.8. STEREO-B detected enhanced electron,
  proton, and other ion fluxes from this flare. We present the Fermi and
  RHESSI observations together with STEREO and SDO data to explore the
  various emission scenarios of this behind-the-limb flare, as well as
  the possible correlation with the SEPs.

---------------------------------------------------------
Title: Evidence of Magnetic Reconnection Involving Partially Ionized
    Coronal Rain near Null Points Observed by SDO/AIA and IRIS
Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Berger, Thomas E.
2014shin.confE..50L    Altcode:
  Coronal rain is cool, partially ionized material formed in the hot,
  fully ionized corona. We report a newly discovered class of coronal
  rain formed near cusp-shaped portions of coronal loops, indicative
  of topological null points. We present evidence of cross-field flows
  associated with magnetic reconnection near such null points from
  SDO/AIA and IRIS observations, investigate the responsible magnetic
  environment, and infer clues to where and when catastrophic cooling
  take place to produce coronal rain. We also discuss the implications
  of such a cooling process for the enigmatic coronal heating mechanisms
  (e.g., Antolin et al. 2010) and compare transient coronal rain and
  persistent prominence downflows.

---------------------------------------------------------
Title: IRIS Observations of Coronal Rain and Prominences: Return
    Flows of the Chromosphere-Corona Mass Cycle
Authors: Liu, Wei; Berger, Thomas; Antolin, Patrick; Schrijver, Karel
2014AAS...22431303L    Altcode:
  It has recently been recognized that a mass cycle (e.g., Berger
  et al. 2011; McIntosh et al. 2012) between the hot, tenuous solar
  corona and the cool, dense chromosphere underneath it plays an
  important role in the mass budget and dynamic evolution of the solar
  atmosphere. Although the corona ultimately loses mass through the solar
  wind and coronal mass ejections, a fraction of its mass returns to the
  chromosphere in coronal rain, downflows of prominences, and other as-yet
  unidentified processes. We present here analysis of joint observations
  of IRIS, SDO/AIA, and Hinode/SOT of such phenomena. By utilizing the
  wide temperature coverage (logT: 4 - 7) provided by these instruments
  combined, we track the coronal cooling sequence (e.g., Schrijver 2001;
  Liu et al. 2012; Berger et al. 2012) leading to the formation of such
  material at transition region or chromospheric temperatures (logT: 4 -
  5) in the million-degree corona. We compare the cooling times with those
  expected from the radiative cooling instability. We also measure the
  kinematics and densities of such downflows and infer their mass fluxes,
  which are compared to the upward mass fluxes into the corona, e.g.,
  those associated with spicules and flux emergence. Special attention is
  paid to coronal rain formed near cusp-shaped portions of coronal loops,
  funnel-shaped prominences at dips of coronal loops, and their respective
  magnetic environments. With the information about where and when such
  catastrophic cooling events take place, we discuss the implications for
  the enigmatic coronal heating mechanisms (e.g., Antolin et al. 2010).

---------------------------------------------------------
Title: Solar wind pressure pulse-driven magnetospheric vortices and
    their global consequences
Authors: Shi, Q. Q.; Hartinger, M. D.; Angelopoulos, V.; Tian, A. M.;
   Fu, S. Y.; Zong, Q. -G.; Weygand, J. M.; Raeder, J.; Pu, Z. Y.; Zhou,
   X. Z.; Dunlop, M. W.; Liu, W. L.; Zhang, H.; Yao, Z. H.; Shen, X. C.
2014JGRA..119.4274S    Altcode:
  We report the in situ observation of a plasma vortex induced by a solar
  wind dynamic pressure enhancement in the nightside plasma sheet using
  multipoint measurements from Time History of Events and Macroscale
  Interactions during Substorms (THEMIS) satellites. The vortex has
  a scale of 5-10 Re and propagates several Re downtail, expanding
  while propagating. The features of the vortex are consistent with the
  prediction of the Sibeck (1990) model, and the vortex can penetrate
  deep ( 8 Re) in the dawn-dusk direction and couple to field line
  oscillations. Global magnetohydrodynamics simulations are carried out,
  and it is found that the simulation and observations are consistent with
  each other. Data from THEMIS ground magnetometer stations indicate a
  poleward propagating vortex in the ionosphere, with a rotational sense
  consistent with the existence of the vortex observed in the magnetotail.

---------------------------------------------------------
Title: Height-dependent Refraction of A Global EUV Wave and Its
    Associated Sympathetic Eruptions
Authors: Liu, Wei; Ofman, Leon; Downs, Cooper; Schrijver, Karel
2014AAS...22421814L    Altcode:
  The height dependence of global extreme-ultraviolet (EUV) waves in
  the solar corona, especially of their wave-like behaviors such as
  transmission and reflection, is critical to understanding their physical
  nature. Prior observations of such behaviors, when detected on the solar
  disk, were compromised because height-dependent information is lost
  due to the line-of-sight projection from a top-down view. We report a
  global EUV wave on the limb observed by SDO/AIA from a side-view that
  evidently shows height-dependent transmission and refraction. As the
  wave travels through an active region, the orientation of the low-corona
  wave front changes from a forward inclination toward the solar surface
  to a backward inclination. This indicates that the EUV wave speed
  is lower at higher altitudes, which is expected because of the rapid
  drop with height of the Alfven and fast-mode speeds in active regions,
  as predicted by MHD models. When traveling into the active region,
  the EUV wave speed in the low corona increases from ~600 km/s to ~900
  km/s. In addition, in the neighborhood of the active region, sympathetic
  eruptions of local coronal structures take place sequentially upon
  the wave impact and may appear as wave reflection. Understanding
  propagation behaviors of global EUV waves brings us one step closer
  to fully utilizing them for seismological diagnostics of the global
  corona, such as mapping the spatial distribution of the Alfven speed
  and magnetic field strength.

---------------------------------------------------------
Title: Fermi Detection of Gamma-ray Emission from a Behind-the-limb
    M1.5 Flare on 2013 October 11
Authors: Pesce-Rollins, Melissa; Omodei, Nicola; Petrosian, Vahe;
   Liu, Wei; Chen, Qingrong; Rubio Da Costa, Fatima
2014AAS...22441404P    Altcode:
  On 2013 October 11 an M1.5 class solar flare erupted from the NOAA
  active region 11868, which was then behind the solar limb. RHESSI images
  reveal hard X-ray emission well above the limb, most likely from the
  top of the flare loop whose footpoints were occulted. Surprisingly
  the Fermi Large Area Telescope (LAT) detected gamma-rays up to 3 GeV
  for ~30 minutes from this flare, making it the first behind-the-limb
  flare observed by Fermi. The LAT gamma-ray emission centroid is
  consistent with the vicinity of the RHESSI hard X-ray source. The
  gamma-ray spectra can be adequately described by a power law with a
  high-energy exponential cutoff, or as a result of the decay of pions
  produced by accelerated protons and ions with an isotropic pitch angle
  distribution and a power-law energy spectrum. The required proton
  spectrum would have a number index of ~3.8. We present the Fermi and
  RHESSI observations together with STEREO and SDO data to explore the
  various emission scenarios of this behind-the-limb flare.

---------------------------------------------------------
Title: Quasi-periodic Fast-mode Magnetosonic Wave Trains Detected
    by SDO/AIA and Their Correlation with Quasi-period Flare Pulsations
Authors: Liu, Wei; Ofman, Leon; Fleishman, Gregory; Downs, Cooper
2014shin.confE.157L    Altcode:
  Quasi-periodic fast propagating wave trains (QFPs; Liu et al. 2011,
  2012) are a new phenomenon recently discovered in extreme ultraviolet
  (EUV) by the Atmospheric Imaging Assembly (AIA) onboard the Solar
  Dynamics Observatory (SDO). They are fast-mode magnetosonic waves,
  closely related to quasi-periodic pulsations of solar flares observed
  from radio to hard X-rays. QFPs usually originate from a flare and
  propagate at typically 500-2000 km/s within a funnel-shaped waveguide
  located inside a CME bubble. QFPs can potentially be used for coronal
  seismological diagnostics and provide critical clues to flare energy
  release and particle acceleration processes. We will present recent
  observational and numerical results of QFPs and compare them with
  quasi-periodic flare pulsations.

---------------------------------------------------------
Title: Hybrid Kinetic and Radiative Hydrodynamic Simulations of
    Solar Flares and Comparison With Multiwavelength Observations
Authors: Rubio Da Costa, Fatima; Petrosian, Vahe; Liu, Wei; Carlsson,
   Mats; Kleint, Lucia
2014AAS...22440906R    Altcode:
  We present a unified simulation which combines two physical processes:
  how the particles are accelerated and the energy is transported along
  a coronal loop, and how the atmosphere responds. The “flare”
  code from Stanford University (Petrosian et al, 2001) models the
  stochastic acceleration and transport of particles and radiation of
  solar flares. It includes pitch angle diffusion and energy loss, and
  computes collisional heating to the background plasma and bremsstrahlung
  emission along the loop. The radiative hydrodynamic RADYN Code
  (Carlsson et al, 1992, 1996; Allred et al, 2005) computes the energy
  transport by the injected non-thermal electrons at the top of a 1D
  coronal loop. Recently, we have combined the two codes by updating the
  non-thermal heating in the RADYN code from the "flare" code, allowing us
  to develop a self-consistent simulation. In addition, we can now model
  more realistically the multi-wavelength emission of solar flares and
  compare it with observations, e.g., at optical wavelengths from IBIS at
  the Dunn Solar Telescope and in X-rays from RHESSI. The high resolution
  UV observations from the recently launched IRIS imaging spectrograph
  will be particularly useful in this regard. These will allow us to
  compare numerically modeled and observed emissions of solar flares in
  several lines using more robust simulations than possible before.

---------------------------------------------------------
Title: Phase transition and elasticity of enstatite under pressure
    from experiments and first-principles studies
Authors: Li, Baosheng; Kung, Jennifer; Liu, Wei; Liebermann, Robert C.
2014PEPI..228...63L    Altcode:
  We have investigated the thermodynamic stability, crystal structure,
  elastic constants, and sound velocities of MgSiO<SUB>3</SUB>-enstatite
  using data from X-ray diffraction and ultrasonic measurements up to
  16.8 GPa and first-principles calculations up to 30 GPa. The calculated
  enthalpies provide theoretical support for the phase transition from
  Pbca to P2<SUB>1</SUB>/c between 9 and 14 GPa previously observed
  in natural orthoensatite and MgSiO<SUB>3</SUB> enstatite. A density
  increase of 1.4-1.5% for the Pbca → P2<SUB>1</SUB>/c transition is
  obtained from both first-principles and experimental studies. Elastic
  constants of Pbca, P2<SUB>1</SUB>/c, C2/c, P2<SUB>1</SUB>ca and Pbca-II
  are all calculated, and a softening in the shear constant C<SUB>55</SUB>
  is predicted for Pbca and Pbca-II phases. C<SUB>55</SUB> of Pbca
  is found to be closely correlated with the A-site SiO<SUB>4</SUB>
  tetrahedra chain angle while C<SUB>44</SUB> and C<SUB>66</SUB> are
  correlated with the B-site chain angle. Pbca, P2<SUB>1</SUB>/c and C2/c
  all exhibit similar volumetric compressibilities at all pressures. The
  calculated velocities of the P2<SUB>1</SUB>/c phase at 12 GPa are equal
  to those of Pbca for P and 1.3% higher for S waves. The experimentally
  observed P and S wave velocity anomalies can be qualitatively described
  by the transformation from Pbca to P2<SUB>1</SUB>/c; however, the
  magnitudes of the velocity decreases between 10 and 14 GPa remain to be
  verified by future single crystal data or polycrystalline measurements
  at high pressures. The predicted velocity jumps of 2.8% and 4.5% for P
  and S waves, respectively, between Pbca and C2/c in the pressure range
  of 5-12 GPa are in excellent agreement with the values of ∼3(1)%
  and ∼5(1)% obtained from the directly measured data, thereby making
  it a plausible candidate for the seismic X-discontinuity at depths of
  250-300 km in the Earth’s upper mantle.

---------------------------------------------------------
Title: Mysterious abrupt carbon-14 increase in coral contributed by
    a comet
Authors: Liu, Yi; Zhang, Zhao-Feng; Peng, Zi-Cheng; Ling, Ming-Xing;
   Shen, Chuan-Chou; Liu, Wei-Guo; Sun, Xiao-Chun; Shen, Cheng-De; Liu,
   Ke-Xin; Sun, Weidong
2014NatSR...4E3728L    Altcode:
  A large and sudden increase in radiocarbon (<SUP>14</SUP>C) around AD
  773 are documented in coral skeletons from the South China Sea. The
  <SUP>14</SUP>C increased by ~ 15‰ during winter, and remain elevated
  for more than 4 months, then increased and dropped down within two
  months, forming a spike of 45‰ high in late spring, followed by two
  smaller spikes. The <SUP>14</SUP>C anomalies coincide with an historic
  comet collision with the Earth's atmosphere on 17 January AD 773. Comas
  are known to have percent-levels of nitrogen by weight, and are exposed
  to cosmic radiation in space. Hence they may be expected to contain
  highly elevated <SUP>14</SUP>C/<SUP>12</SUP>C ratios, as compared to
  the Earth's atmosphere. The significant input of <SUP>14</SUP>C by
  comets may have contributed to the fluctuation of <SUP>14</SUP>C in the
  atmosphere throughout the Earth's history, which should be considered
  carefully to better constrain the cosmic ray fluctuation.

---------------------------------------------------------
Title: Spectroscopic factors for low-lying N16 levels and the
    astrophysical N15(n ,γ)N16 reaction rate
Authors: Guo, B.; Li, Z. H.; Li, Y. J.; Su, J.; Pang, D. Y.; Yan,
   S. Q.; Wu, Z. D.; Li, E. T.; Bai, X. X.; Du, X. C.; Fan, Q. W.; Gan,
   L.; He, J. J.; Jin, S. J.; Jing, L.; Li, L.; Li, Z. C.; Lian, G.;
   Liu, J. C.; Shen, Y. P.; Wang, Y. B.; Yu, X. Q.; Zeng, S.; Zhang,
   L. Y.; Zhang, W. J.; Liu, W. P.
2014PhRvC..89a2801G    Altcode: 2014arXiv1401.0067G
  Background: Fluorine is a key element for nucleosynthetic studies
  since it is extremely sensitive to the physical conditions within
  stars. The astrophysical site to produce fluorine is suggested to
  be asymptotic giant branch stars. In these stars the N15(n,γ)N16
  reaction could affect the abundance of fluorine by competing with
  N15(α ,γ)F19. <P />Purpose: The N15(n ,γ)N16 reaction rate depends
  directly on the neutron spectroscopic factors of the low-lying states
  in N16. Shell model calculations and two previous measurements of the
  (d ,p) reaction yielded the spectroscopic factors with a discrepancy
  by a factor of ∼2. The present work aims to explore these neutron
  spectroscopic factors through an independent transfer reaction
  and to determine the stellar rate of the N15(n,γ)N16 reaction. <P
  />Methods: The angular distributions of the N15(Li7,Li6)N16 reaction
  populating the ground state and the first three excited states in N16
  are measured using a Q3D magnetic spectrograph and are used to derive
  the spectroscopic factors of these states based on distorted wave Born
  approximation analysis. <P />Results: The spectroscopic factors of
  these four states are extracted to be 0.96 ± 0.09, 0.69 ± 0.09, 0.84
  ± 0.08, and 0.65 ± 0.08, respectively. Based on the new spectroscopic
  factors we derive the N15(n ,γ)N16 reaction rate. <P />Conclusions:
  The accuracy and precision of the spectroscopic factors are enhanced
  due to the first application of high-precision magnetic spectrograph
  for resolving the closely spaced N16 levels which cannot be achieved
  in most recent measurements. The present result demonstrates that two
  levels corresponding to neutron transfers to the 2s<SUB>1/2</SUB>
  orbit in N16 are not good single-particle levels although N15 is a
  closed neutron-shell nucleus. This finding is contrary to the shell
  model expectation. The present work also provides an independent
  examination to shed some light on the existing discrepancies in the
  spectroscopic factors and the N15(n ,γ)N16 rate.

---------------------------------------------------------
Title: Mixture steering law design for control moment gyroscopes
Authors: Zhang, JingRui; Luo, Yang; Liu, Wei; Zhang, Yao
2014SCPMA..57..138Z    Altcode: 2014ScChG..57..138Z
  Focusing on the singularities of a spacecraft using control moment
  gyros (CMGs) to do the large angle maneuvers, a new mixture steering
  law is proposed to avoid the singularities. According to this method,
  if the CMGs are far away from the singularity, the Moore-Penrose
  pseudo-inverse steering law (MP) is used directly. If the CMGs are
  close to the singularity, instead of solving the inverse matrix, a
  set of optimal gimbal angles are sought for the singular measurement
  to reach the maximum, which can avoid the singularities. Simulations
  show that the designed steering law enables the spacecraft to carry
  out the large angle maneuver and avoid the singularities simultaneously.

---------------------------------------------------------
Title: Hubble Space Telescope STIS Coronagraphy of WISE Debris
    Disk Candidates
Authors: Padgett, Deborah; Stapelfeldt, K. R.; Krist, J. E.; Liu,
   W. M.; Leisawitz, D.; Fajardo-Acosta, S.; Debes, J. H.
2014AAS...22340907P    Altcode:
  We report on an HST imaging program to search for debris disks in
  scattered light using the STIS coronagraph. The targets are 13 Hipparcos
  stars selected for robust levels of WISE 22 micron emission in excess
  of photospheric levels. These sources represent some of the closest
  and brightest of the large set of new WISE debris disk candidates
  (Padgett et al. 2013). Many of the sources appear as bare point spread
  functions with no extended nebulosity; two others are revealed as blends
  of bright stars with adjacent background star-forming galaxies. Debris
  disks were directly imaged in 5/13 targets, one of which is a marginal
  detection. Among these is an outstanding new edge-on system with
  diameter of 1000 AU and clear structural asymmetries suggestive of
  perturbations from planetary-mass companions. In this talk we will
  present HST images of these five new debris disk systems and discuss
  their characteristics.

---------------------------------------------------------
Title: Analysis of Satellite Drag Coefficient Based on Wavelet
    Transform
Authors: Liu, Wei; Wang, Ronglan; Liu, Siqing
2014cosp...40E1855L    Altcode:
  Abstract: Drag coefficient sequence was obtained by solving Tiangong1
  continuous 55days GPS orbit data with different arc length. The same
  period solar flux f10.7 and geomagnetic index Ap ap series were high and
  low frequency multi-wavelet decomposition. Statistical analysis results
  of the layers sliding correlation between space environmental parameters
  and decomposition of Cd, showed that the satellite drag coefficient
  sequence after wavelet decomposition and the corresponding level of
  f10.7 Ap sequence with good lag correlation. It also verified that the
  Cd prediction is feasible. Prediction residuals of Cd with different
  regression models and different sample length were analysed. The results
  showed that the case was best when setting sample length 20 days and
  f10.7 regression model were used. It also showed that NRLMSIS-00
  model's response in the region of 350km (Tiangong's altitude) and
  low-middle latitude (Tiangong's inclination) is excessive in ascent
  stage of geomagnetic activity Ap and is inadequate during fall off
  segment. Additionally, the low-frequency decomposition components
  NRLMSIS-00 model's response is appropriate in f10.7 rising segment. High
  frequency decomposition section, Showed NRLMSIS-00 model's response is
  small-scale inadequate during f10.7 ascent segment and is reverse in
  decline of f10.7. Finally, the potential use of a summary and outlook
  were listed; This method has an important reference value to improve
  the spacecraft orbit prediction accuracy. Key words: wavelet transform;
  drag coefficient; lag correlation; Tiangong1;space environment

---------------------------------------------------------
Title: Coronal Condensation in Funnel Prominences as Return Flows
    of the Chromosphere-Corona Mass Cycle
Authors: Liu, Wei; Berger, Thomas E.; Low, B. C.
2014IAUS..300..441L    Altcode:
  We present SDO/AIA observations of a potentially novel type of
  prominence, called “funnel prominence”, that forms out of coronal
  condensation at magnetic dips. <P />They can drain a large amount
  of mass (up to ~10<SUP>15</SUP> g day<SUP>-1</SUP>) and may play an
  important role as return flows of the chromosphere-corona mass cycle.

---------------------------------------------------------
Title: The WIYN One Degree Imager: Upgrading for the Future
Authors: Harbeck, Daniel R.; Liu, W. M.; Rajagopal, J.; ODI Team
2014AAS...22314819H    Altcode:
  The WIYN One Degree Imager has been in shared risk operations since
  February 2013. At this time, the focal plane is populated with 13
  out of 64 possible Orthogonal Transfer Array (OTA) CCD detectors,
  yielding a science field of view of 24’ x 24’. In this poster we
  first report on the performance of the instrument during its first year
  of operations. Then we will update on the progress towards improving
  ODI for the future: As of this writing, WIYN is acquiring a new
  batch of OTA detectors with a better low light level charge transfer
  efficiency. With the new detectors in a 6x6 detector configuration,
  the field of view will be increased to 48x48 arcminutes. Other ODI
  improvements will focus on observing efficiency, including a redesign
  of the filter drive mechanism and an improvement on WIYN’s pointing
  accuracy. Commissioning of upgraded 6x6 ODI is scheduled for late 2014.

---------------------------------------------------------
Title: The Perihelion Passage of Comet ISON as seen by SDO
Authors: Pesnell, W. D.; Schrijver, C. J.; Boerner, P.; DeRosa, M. L.;
   Liu, W.; Thompson, B. J.
2013AGUFM.P24A..10P    Altcode:
  Comet ISON will fly through perihelion on November 28, 2013. It is one
  of the largest sungrazing comets to be seen in the Space Age. The Solar
  Dynamics Observatory (SDO) has seen two previous sungrazing comets in
  the extreme ultraviolet channels of the Atmospheric Imaging Assembly
  (AIA). Comet ISON will fly farther from the Sun (perihelion distance
  of 2.7 Rsun compared to 1.15 for Comet Lovejoy), meaning it probes
  a different part of the solar corona, but its larger size should
  provide enough mass to illuminate the path of the nucleus. Based on
  the latest ephemeris, SDO will be able to track Comet ISON through
  the entire perihelion passage by a series of off-point maneuvers. We
  will present the AIA data obtained from the Comet ISON perihelion,
  discussing the differences between Comets ISON and Lovejoy. We will
  then summarize what we have learned from the observations and offer
  some thoughts on what sungrazing comets may reveal about comets,
  the Sun, and their interaction.

---------------------------------------------------------
Title: Distribution of thermal oxygen ions in the near earth
    magnetosphere
Authors: Liu, W.; Cao, J.
2013AGUFMSM51B2172L    Altcode:
  Based on eleven years of Cluster particle observations, we investigate
  the distribution of thermal oxygen ions in the near earth magnetosphere
  with full spatial coverage between 4 to 20 Re. Averaged oxygen ion
  fluxes are calculated for three energy ranges (E1: 25-136eV; E2:
  136eV-3keV; E3 3-35keV) based on measurements from CIS instrument. In
  a preliminary analysis, we found that oxygen ions of E1 energy are
  observed mostly in the Polar Regions flowing toward the nightside with
  average speed of ~20 km/s at 5 Re. They are accelerated to E2 energy
  range before they arrive at plasmasheet. Clear dawn-dusk asymmetry is
  observed in the plasmasheet for oxygen ions of the E1 and E2 energy
  that they are distributed beyond 10 Re on the duskside and beyond 15
  Re on the dawnside, suggesting the transportation from ionosphere to
  plasmasheet is asymmetric for dawn and dusk sides. These oxygen ions
  are further accelerated in the plasmasheet to E3 energy range and are
  transported toward the Earth, while they drift westward. These oxygen
  ions finally reach the dayside, and then either return to the ionosphere
  or escape from the dayside magnetopause to magnetosheeth. This study
  provides background knowledge on complete distribution of thermal
  oxygen ions in the near earth magnetosphere for the modelling and
  simulation studies on ionosphere-magnetosphere coupling.

---------------------------------------------------------
Title: Nonlinear fluid equations for fully toroidal electromagnetic
    waves for the core tokamak plasma
Authors: Weiland, J.; Liu, C. S.; Liu
2013JPlPh..79.1015W    Altcode:
  The rather general set of fluid equations with full curvature effects
  (Shukla and Weiland, Phys. Rev. A 40, 341 (1989)) has been modified
  to apply to the core and generalized to include also microtearing modes.

---------------------------------------------------------
Title: Estimating the Power per Mode Number and Power vs L-shell of
    Broadband, Storm-time ULF Waves
Authors: Sarris, T. E.; Li, X.; Liu, W.; Argyriadis, E.
2013AGUFMSM53D2258S    Altcode:
  In studies of particles' radial diffusion processes in the magnetosphere
  it is well known that Ultra-Low Frequency (ULF) waves of frequency m*ωd
  can resonantly interact with particles of drift frequency ωd, where m
  is the azimuthal mode number of the waves; however due to difficulties
  in estimating m an over-simplifying assumption is often made in radial
  diffusion simulations, namely that all ULF wave power is located at
  m=1 or, in some cases, m=2. In another assumption that is commonly
  made, power measured from geosynchronous satellites is assumed to be
  uniform across L-shells. In the present work, a technique is presented
  for extracting information on the distribution of ULF wave power in a
  range of azimuthal mode numbers, through calculations of the cross-power
  and phase differences between a number of azimuthally aligned pairs
  of magnetometers, either in space or on the ground. We find that the
  temporal evolution of power at each mode number gives unique insight
  into the temporal evolution of ULF waves during a storm as well as a
  more accurate characterization of broadband ULF waves. Furthermore,
  using multi-spacecraft measurements during a particular storm, we
  calculate the L-dependence of ULF wave power. These measurements and
  calculations can be used in more accurate ULF wave representation in
  radial diffusion simulations.

---------------------------------------------------------
Title: Turbulence in the Earth's cusp region: k-filtering analysis
Authors: Wang, T.; Cao, J.; Fu, H.; Liu, W.
2013AGUFMSM53B2228W    Altcode:
  On April 13 2002, four Cluster spacecraft with separation up to 127 km
  measured similar turbulence in the Earth's mid-altitude cusp region
  during southward IMF Bz. Using the k-filtering technique, we obtain
  the propagation angle and dispersion relation of the turbulence. The
  propagation angle is quite large and ranges from 80° to 92°, meaning
  that the turbulence propagates perpendicularly to the background
  magnetic field. By comparing the dispersion relationship with the
  linear solution of the Vlasov kinetic theory obtained by WHAMP,
  we conclude that the turbulence is Kinetic Alfvén mode (KAWs). The
  regions of KAWs are located within an inhomogeneous high density plasma
  background, suggesting that it is the ion drift, not field aligned ion
  beam that plays an important role in the wave generation. The magnetic
  flied fluctuation spectrum resembles the classical Kolmogorov power law
  under the proton gyrofrequency ωci, but breaks and steepens near ωci,
  indicating that the KAW may be powered by a turbulent cascade transverse
  to the magnetic field from large MHD scales to proton gyroradius scales.

---------------------------------------------------------
Title: An electromagnetic gamma-ray free electron laser*
Authors: Eliasson, Bengt; Liu, Chuan Sheng; Liu
2013JPlPh..79..995E    Altcode:
  We present a theoretical model for the generation of coherent gamma
  rays by a free electron laser, where a high-energy electron beam
  interacts with an electromagnetic wiggler. By replacing the static
  undulator with a 1-μm laser wiggler, the resulting radiation would go
  from X-rays currently observed in experiments, to gamma rays. Coherent
  light in the gamma-ray range would have wide-ranging applications in
  the probing of matter on sub-atomic scales.

---------------------------------------------------------
Title: Observations of chorus at sun-synchronous orbit
Authors: zhima, Z.; Cao, J.; Liu, W.; Fu, H.
2013AGUFMSM41A2214Z    Altcode:
  Using the data of the DEMTER satellite during the magnetic storm on
  14 April 2006, we study the storm time VLF electromagnetic waves, and
  find the first observational evidence of chorus waves propagating to
  high latitude and entering the plasmasphere. During this geomagnetic
  storm, ';banded' emissions of a few hertz to 20 kHz are observed to be
  intensified and to be organized in the frequency range of 0.1-0.5fce
  (equatorial electron cyclotron frequency) in high latitude region
  of magnetic latitude between ~40°to ~60°. The signatures in the
  wave power spectra suggest these emissions are likely lower-band
  chorus. We also investigate the spatial coverage and temporal variation
  of the observed high-latitude chorus emissions and their relation to
  plasmapause locations. It is convincing that the plasmapause location
  obtained from the observations by DEMETER and the one from the empirical
  model are consistent. The observed chorus waves are generally outside
  the plasmasphere. However, interestingly, these waves are frequently
  observed inside the plasmasphere at regions with low L value during the
  main phase and early recover phase, which has never been reported in
  previous studies of chorus in low latitude regions. The present study
  gives observational supports for the theory and simulations suggesting
  that chorus waves propagate into the plasmasphere and evolve into
  hiss waves.

---------------------------------------------------------
Title: Mode number calculations of ULF field-line resonances using
    ground magnetometers and THEMIS measurements
Authors: Sarris, T. E.; Li, X.; Liu, W.; Argyriadis, E.; Boudouridis,
   A.; Ergun, R.
2013JGRA..118.6986S    Altcode:
  multiple pairs of International Monitor for Auroral Geomagnetic Effects
  ground magnetometers together with simultaneous measurements from two of
  the Time History of Events and Macroscale Interactions during Substorms
  (THEMIS) spacecraft constellation, when they were flying over the
  magnetometers in magnetic conjunction and in close azimuthal separation,
  we are able to calculate the phase differences of Ultra Low Frequency
  Field-Line Resonances, and, through that, their azimuthal mode number,
  wavelength and propagation characteristics. A cross-wavelet technique is
  applied, that exposes the times and frequencies of common power between
  time series from azimuthally aligned magnetometers in space or on the
  ground, yielding their relative phase. Using the amplitude ratio and
  phase differences between ground stations with similar longitudes that
  are separated in latitude, a correction to the mode number calculation
  is demonstrated, accounting for the phase differences that arise from
  the L shell separation of the THEMIS probes.

---------------------------------------------------------
Title: Constraining nova observables: Direct measurements of resonance
    strengths in <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl
Authors: Fallis, J.; Parikh, A.; Bertone, P. F.; Bishop, S.; Buchmann,
   L.; Chen, A. A.; Christian, G.; Clark, J. A.; D'Auria, J. M.; Davids,
   B.; Deibel, C. M.; Fulton, B. R.; Greife, U.; Guo, B.; Hager, U.;
   Herlitzius, C.; Hutcheon, D. A.; José, J.; Laird, A. M.; Li, E. T.;
   Li, Z. H.; Lian, G.; Liu, W. P.; Martin, L.; Nelson, K.; Ottewell,
   D.; Parker, P. D.; Reeve, S.; Rojas, A.; Ruiz, C.; Setoodehnia, K.;
   Sjue, S.; Vockenhuber, C.; Wang, Y. B.; Wrede, C.
2013PhRvC..88d5801F    Altcode: 2013arXiv1309.3543F
  The <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl reaction is important for
  constraining predictions of certain isotopic abundances in oxygen-neon
  novae. Models currently predict as much as 150 times the solar abundance
  of <SUP>33</SUP>S in oxygen-neon nova ejecta. This overproduction
  factor may vary by orders of magnitude due to uncertainties in
  the <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl reaction rate at nova peak
  temperatures. Depending on this rate, <SUP>33</SUP>S could potentially
  be used as a diagnostic tool for classifying certain types of presolar
  grains. Better knowledge of the <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl
  rate would also aid in interpreting nova observations over the S-Ca
  mass region and contribute to the firm establishment of the maximum
  endpoint of nova nucleosynthesis. Additionally, the total S elemental
  abundance which is affected by this reaction has been proposed as
  a thermometer to study the peak temperatures of novae. Previously,
  the <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl reaction rate had only been
  studied directly down to resonance energies of 432 keV. However, for
  nova peak temperatures of 0.2-0.4 GK there are seven known states
  in <SUP>34</SUP>Cl both below the 432-keV resonance and within the
  Gamow window that could play a dominant role. Direct measurements
  of the resonance strengths of these states were performed using
  the DRAGON (Detector of Recoils And Gammas of Nuclear reactions)
  recoil separator at TRIUMF. Additionally two new states within this
  energy region are reported. Several hydrodynamic simulations have
  been performed, using all available experimental information for the
  <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl rate, to explore the impact of
  the remaining uncertainty in this rate on nucleosynthesis in nova
  explosions. These calculations give a range of ≈20-150 for the
  expected <SUP>33</SUP>S overproduction factor, and a range of ≈100-450
  for the <SUP>32</SUP>S/<SUP>33</SUP>S ratio expected in ONe novae.

---------------------------------------------------------
Title: Large-scale Coronal Propagating Fronts in Solar Eruptions
    as Observed by the Atmospheric Imaging Assembly on Board the Solar
    Dynamics Observatory—an Ensemble Study
Authors: Nitta, Nariaki V.; Schrijver, Carolus J.; Title, Alan M.;
   Liu, Wei
2013ApJ...776...58N    Altcode: 2013arXiv1308.3544N
  This paper presents a study of a large sample of global disturbances
  in the solar corona with characteristic propagating fronts as
  intensity enhancement, similar to the phenomena that have often
  been referred to as Extreme Ultraviolet Imaging Telescope (EIT)
  waves or extreme-ultraviolet (EUV) waves. Now EUV images obtained by
  the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics
  Observatory provide a significantly improved view of these large-scale
  coronal propagating fronts (LCPFs). Between 2010 April and 2013 January,
  a total of 171 LCPFs have been identified through visual inspection of
  AIA images in the 193 Å channel. Here we focus on the 138 LCPFs that
  are seen to propagate across the solar disk, first studying how they
  are associated with flares, coronal mass ejections (CMEs), and type II
  radio bursts. We measure the speed of the LCPF in various directions
  until it is clearly altered by active regions or coronal holes. The
  highest speed is extracted for each LCPF. It is often considerably
  higher than EIT waves. We do not find a pattern where faster LCPFs
  decelerate and slow LCPFs accelerate. Furthermore, the speeds are
  not strongly correlated with the flare intensity or CME magnitude,
  nor do they show an association with type II bursts. We do not find
  a good correlation either between the speeds of LCPFs and CMEs in a
  subset of 86 LCPFs observed by one or both of the Solar and Terrestrial
  Relations Observatory spacecraft as limb events.

---------------------------------------------------------
Title: Multi-fluid MHD model for Sun-grazing comets
Authors: Jia, Y. -D.; Russell, C. T.; Liu, W.; Gombosi, T. I.
2013EPSC....8..760J    Altcode:
  Sun-grazing comets are comets that dive into the lower corona. Recent
  advances in spacecraft capabilities have enabled us to observe
  these comets with high resolution both in time and space. These
  comets exhibit rich tail activity, even multiple tails. This study
  investigates a collection of these activities, models the cometary
  plasma with model-generated coronal conditions.

---------------------------------------------------------
Title: Resonant scattering of <SUP>22</SUP>Na + p studied by the
    thick-target inverse-kinematic method
Authors: Jin, S. J.; Wang, Y. B.; Su, J.; Yan, S. Q.; Li, Y. J.; Guo,
   B.; Li, Z. H.; Zeng, S.; Lian, G.; Bai, X. X.; Liu, W. P.; Yamaguchi,
   H.; Kubono, S.; Hu, J.; Kahl, D.; Jung, H. S.; Moon, J. Y.; Lee, C. S.;
   Teranishi, T.; Wang, H. W.; Ishiyama, H.; Iwasa, N.; Komatsubara,
   T.; Brown, B. A.
2013PhRvC..88c5801J    Altcode:
  Background: In presolar low-density graphite grains, an extraordinarily
  large <SUP>22</SUP>Ne/<SUP>20</SUP>Ne ratio or even nearly pure
  <SUP>22</SUP>Ne is found, pointing to the condensation of radioactive
  <SUP>22</SUP>Na in grains. Supernovae and neon-rich novae are the
  main events that produce <SUP>22</SUP>Na via the explosive hydrogen
  burning process. The <SUP>22</SUP>Na(p, γ)<SUP>23</SUP>Mg reaction
  is one of the key reactions that influences the <SUP>22</SUP>Na
  abundance in ejecta.Purpose:The present work aims to explore
  the proton resonant states in <SUP>23</SUP>Mg relevant to the
  astrophysical <SUP>22</SUP>Na(p, γ)<SUP>23</SUP>Mg reaction. The
  determined <SUP>23</SUP>Mg resonant parameters can be used to
  evaluate the <SUP>22</SUP>Na(p, γ)<SUP>23</SUP>Mg reaction
  rate.Method:A low-energy <SUP>22</SUP>Na radioactive ion beam is
  produced via the <SUP>1</SUP>H(<SUP>22</SUP>Ne, <SUP>22</SUP>Na)n
  reaction, and used to measure the experimental excitation function
  of the <SUP>22</SUP>Na + p resonant scattering with a conventional
  thick-target inverse kinematic method. R-matrix analysis is applied to
  deduce the <SUP>23</SUP>Mg resonance parameters from the experimental
  excitation function.Results: Three proton resonance states in
  <SUP>23</SUP>Mg are observed. Spins/parities and the proton partial
  widths are determined. The deduced excitation energies agree with
  the compiled values.Conclusions: The new spin and parity assignments
  allow us to perform a shell-model calculation of the γ widths
  of the <SUP>23</SUP>Mg resonant states for the evaluation of the
  <SUP>22</SUP>Na(p, γ)<SUP>23</SUP>Mg astrophysical reaction rate. The
  two s-wave resonant states established in this work at 8.793 and 8.916
  MeV in <SUP>23</SUP>Mg, respectively, increase the total reaction rate
  by about 5% at a temperature greater than 2 GK.

---------------------------------------------------------
Title: SDO/AIA and Hinode/EIS Observations of Interaction between
    an EUV Wave and Active Region Loops
Authors: Yang, Liheng; Zhang, Jun; Liu, Wei; Li, Ting; Shen, Yuandeng
2013ApJ...775...39Y    Altcode: 2013arXiv1308.1821Y
  We present detailed analysis of an extreme-ultraviolet (EUV) wave
  and its interaction with active region (AR) loops observed by the
  Solar Dynamics Observatory/Atmospheric Imaging Assembly and the
  Hinode EUV Imaging Spectrometer (EIS). This wave was initiated from
  AR 11261 on 2011 August 4 and propagated at velocities of 430-910
  km s<SUP>-1</SUP>. It was observed to traverse another AR and
  cross over a filament channel on its path. The EUV wave perturbed
  neighboring AR loops and excited a disturbance that propagated toward
  the footpoints of these loops. EIS observations of AR loops revealed
  that at the time of the wave transit, the original redshift increased
  by about 3 km s<SUP>-1</SUP>, while the original blueshift decreased
  slightly. After the wave transit, these changes were reversed. When
  the EUV wave arrived at the boundary of a polar coronal hole, two
  reflected waves were successively produced and part of them propagated
  above the solar limb. The first reflected wave above the solar limb
  encountered a large-scale loop system on its path, and a secondary wave
  rapidly emerged 144 Mm ahead of it at a higher speed. These findings
  can be explained in the framework of a fast-mode magnetosonic wave
  interpretation for EUV waves, in which observed EUV waves are generated
  by expanding coronal mass ejections.

---------------------------------------------------------
Title: Observation of a Moreton Wave and Wave-Filament Interactions
    Associated with the Renowned X9 Flare on 1990 May 24
Authors: Liu, Rui; Liu, Chang; Xu, Yan; Liu, Wei; Kliem, Bernhard;
   Wang, Haimin
2013ApJ...773..166L    Altcode:
  Using Big Bear Solar Observatory film data recently digitized at
  NJIT, we investigate a Moreton wave associated with an X9 flare
  on 1990 May 24, as well as its interactions with four filaments
  F1-F4 located close to the flaring region. The interaction yields
  interesting insight into physical properties of both the wave and
  the filaments. The first clear Moreton wavefront appears at the
  flaring-region periphery at approximately the same time as the peak
  of a microwave burst and the first of two γ-ray peaks. The wavefront
  propagates at different speeds ranging from 1500-2600 km s<SUP>-1</SUP>
  in different directions, reaching as far as 600 Mm away from the flaring
  site. Sequential chromospheric brightenings are observed ahead of the
  Moreton wavefront. A slower diffuse front at 300-600 km s<SUP>-1</SUP>
  is observed to trail the fast Moreton wavefront about one minute after
  the onset. The Moreton wave decelerates to ~550 km s<SUP>-1</SUP> as it
  sweeps through F1. The wave passage results in F1's oscillation which
  is featured by ~1 mHz signals with coherent Fourier phases over the
  filament, the activation of F3 and F4 followed by gradual recovery,
  but no disturbance in F2. Different height and magnetic environment
  together may account for the distinct responses of the filaments to
  the wave passage. The wavefront bulges at F4, whose spine is oriented
  perpendicular to the upcoming wavefront. The deformation of the
  wavefront is suggested to be due to both the forward inclination of
  the wavefront and the enhancement of the local Alfvén speed within
  the filament channel.

---------------------------------------------------------
Title: Thinking Problems of the Present Collision Warning Work by
    Analyzing the Intersection Between Cosmos 2251 and Iridium 33
Authors: Wang, R. L.; Liu, W.; Yan, R. D.; Gong, J. C.
2013ESASP.723E.156W    Altcode:
  After Cosmos 2251 and Iridium 33 collision breakup event, the
  institutions at home and abroad began the collision warning analysis for
  the event. This paper compared the results from the different research
  units and discussed the problems of the current collision warning work,
  then gave the suggestions of further study.

---------------------------------------------------------
Title: TeV cosmic-ray proton and helium spectra in the myriad model
Authors: Bernard, G.; Delahaye, T.; Keum, Y. -Y.; Liu, W.; Salati,
   P.; Taillet, R.
2013A&A...555A..48B    Altcode: 2012arXiv1207.4670B
  Context. Recent measurements of cosmic ray proton and helium spectra
  show a hardening above a few hundred GeV. This excess is hard to
  understand in the framework of the conventional models of Galactic
  cosmic ray production and propagation. <BR /> Aims: We propose here
  to explain this anomaly by the presence of local sources (myriad
  model). <BR /> Methods: Cosmic ray propagation is described as a
  diffusion process taking place inside a two-zone magnetic halo. We
  calculate the proton and helium fluxes at the Earth between 50 GeV and
  100 TeV. As an improvement over a similar analysis, we consistently
  derive these fluxes by taking both local and remote sources for which a
  unique injection rate is assumed into account. <BR /> Results: We find
  cosmic ray propagation parameters compatible with B/C measurements for
  which the proton and helium spectra agree remarkably with the PAMELA
  and CREAM measurements over four decades in energy.

---------------------------------------------------------
Title: Evidence of Particle Acceleration and Plasma Heating in
    Magnetic Reconnection Outflows in an Eruptive Solar Flare
Authors: Liu, Wei; Chen, Q.; Petrosian, V.
2013SPD....44...89L    Altcode:
  Where particle acceleration and plasma heating take place in relation
  to magnetic reconnection is a fundamental question for solar flares. We
  present here analysis of an M7.7 flare on 2012 July 19 observed by
  SDO/AIA and RHESSI that sheds new light on this question (Liu, Chen,
  &amp; Petrosian, 2013, ApJ). Bi-directional outflows in forms of
  plasmoid ejections and contracting cusp-shaped loops originate between
  an erupting flux rope (Patsourakos et al. 2013, ApJ) and underlying
  flare loops at speeds of typically 200-300 km/s up to 1050 km/s. These
  outflows are associated with spatially separated double coronal X-ray
  sources with their centroid separation decreasing with energy. The
  highest temperature is located near the nonthermal X-ray loop-top
  source, well below the original heights of contracting cusps near the
  inferred reconnection site. These observations suggest that the primary
  loci of particle acceleration and plasma heating are in the reconnection
  outflow regions, rather than the reconnection site itself. We stress
  that models with this ingredient were proposed long ago (e.g., Forbes
  &amp; Priest 1983) and backed by recent numerical simulations (e.g.,
  Drake &amp; Swisdak 2012), but solid observational evidence as presented
  here has been lacking. In addition, there is an initial ascent of the
  X-ray and EUV loop-top source prior to its recently recognized descent,
  which we ascribe to the interplay among multiple processes including
  the upward development of reconnection and the downward contractions of
  reconnected loops. The impulsive phase onset coincides with the rapid
  speed increases of the upward plasmoids, the individual loop shrinkages,
  and the overall loop-top descent, suggestive of an intimate relation
  of the energy release rate and the reconnection outflow speed.Abstract
  (2,250 Maximum Characters): Where particle acceleration and plasma
  heating take place in relation to magnetic reconnection is a fundamental
  question for solar flares. We present here analysis of an M7.7 flare
  on 2012 July 19 observed by SDO/AIA and RHESSI that sheds new light on
  this question (Liu, Chen, &amp; Petrosian, 2013, ApJ). Bi-directional
  outflows in forms of plasmoid ejections and contracting cusp-shaped
  loops originate between an erupting flux rope (Patsourakos et al. 2013,
  ApJ) and underlying flare loops at speeds of typically 200-300 km/s up
  to 1050 km/s. These outflows are associated with spatially separated
  double coronal X-ray sources with their centroid separation decreasing
  with energy. The highest temperature is located near the nonthermal
  X-ray loop-top source, well below the original heights of contracting
  cusps near the inferred reconnection site. These observations suggest
  that the primary loci of particle acceleration and plasma heating are
  in the reconnection outflow regions, rather than the reconnection site
  itself. We stress that models with this ingredient were proposed long
  ago (e.g., Forbes &amp; Priest 1983) and backed by recent numerical
  simulations (e.g., Drake &amp; Swisdak 2012), but solid observational
  evidence as presented here has been lacking. In addition, there is
  an initial ascent of the X-ray and EUV loop-top source prior to its
  recently recognized descent, which we ascribe to the interplay among
  multiple processes including the upward development of reconnection
  and the downward contractions of reconnected loops. The impulsive phase
  onset coincides with the rapid speed increases of the upward plasmoids,
  the individual loop shrinkages, and the overall loop-top descent,
  suggestive of an intimate relation of the energy release rate and the
  reconnection outflow speed.

---------------------------------------------------------
Title: Quasi-periodic Fast-mode Magnetosonic Wave Trains Inside and
    Outside CME Bubbles Detected by SDO/AIA
Authors: Liu, Wei; Ofman, L.; Downs, C.; Title, A. M.
2013SPD....44...50L    Altcode:
  Quasi-periodic fast-mode magnetosonic wave trains both inside and
  outside expanding CME bubbles have recently been discovered by
  SDO/AIA (Liu et al. 2011, 2012; Shen &amp; Liu 2012). In general,
  a wave train inside a CME bubble originates from a flare site and
  propagates along a funnel of coronal loops at typically 1000-2000 km/s
  (Ofman et al. 2011). A wave train outside a CME usually originates
  from a CME flank and propagates in the low corona along the solar
  surface following the leading front of a global EUV wave at typically
  500-1000 km/s. The former is primarily seen in the cooler 171 Angstrom
  channel with a characteristic temperature of 0.8 MK, while the latter
  is pronounced in the hotter 193 and 211 Angstrom channels of typically
  1.6-2.0 MK. What is the relationship between the two types of wave
  trains? Why do they appear differently in location and wavelength
  (temperature)? To answer these questions, we report here for the
  first time the evidence that the wave train beyond the CME bubble is
  the continuation of the same wave train along the funnel within the
  CME. The continuous deceleration of the waves is consistent with the
  expected decrease of the local fast-mode speed with distance from the
  active region (e.g., Ofman et al. 2011; Downs et al. 2012). There is
  an abrupt change of the wave speed at the topological interface where
  the expanding CME flank is located, indicative of contrasting magnetic
  and plasma conditions, which can give rise to different (fast-mode)
  speeds and wavelength (temperature) dependent appearances of these wave
  trains.Abstract (2,250 Maximum Characters): Quasi-periodic fast-mode
  magnetosonic wave trains both inside and outside expanding CME bubbles
  have recently been discovered by SDO/AIA (Liu et al. 2011, 2012;
  Shen &amp; Liu 2012). In general, a wave train inside a CME bubble
  originates from a flare site and propagates along a funnel of coronal
  loops at typically 1000-2000 km/s (Ofman et al. 2011). A wave train
  outside a CME usually originates from a CME flank and propagates in
  the low corona along the solar surface following the leading front of a
  global EUV wave at typically 500-1000 km/s. The former is primarily seen
  in the cooler 171 Angstrom channel with a characteristic temperature
  of 0.8 MK, while the latter is pronounced in the hotter 193 and 211
  Angstrom channels of typically 1.6-2.0 MK. What is the relationship
  between the two types of wave trains? Why do they appear differently
  in location and wavelength (temperature)? To answer these questions,
  we report here for the first time the evidence that the wave train
  beyond the CME bubble is the continuation of the same wave train
  along the funnel within the CME. The continuous deceleration of the
  waves is consistent with the expected decrease of the local fast-mode
  speed with distance from the active region (e.g., Ofman et al. 2011;
  Downs et al. 2012). There is an abrupt change of the wave speed at
  the topological interface where the expanding CME flank is located,
  indicative of contrasting magnetic and plasma conditions, which can
  give rise to different (fast-mode) speeds and wavelength (temperature)
  dependent appearances of these wave trains.

---------------------------------------------------------
Title: Observation of a Moreton Wave and Wave-Filament Interactions
    Using Digitized Film Data at BBSO
Authors: Wang, Haimin; Liu, R.; Liu, C.; Xu, Y.; Liu, W.
2013SPD....4410402W    Altcode:
  We have finished digitizing all full disk and a fraction of high
  resolution films obtained by Big Bear Solar Observatory (BBSO) from
  1969 to 1997. Using high-cadence (10s) digitized data we investigate
  a Moreton wave associated with an X9 flare on 1990 May 24, as well
  as its interactions with four filaments F1-F4 located close to the
  flaring active region. The interaction yields interesting insight
  into physical properties of both the wave and the filaments. The
  first Moreton wavefront appears at the active-region periphery at
  21UT, about the same time as the peak of the microwave burst and the
  first of the double-peak gamma-ray burst. The wavefront propagates at
  2 Mm/s within five minutes of its initiation, reaching as far as 600
  Mm away from the flaring site. Sequential chromospheric brightenings
  (SCBs) are observed ahead of the Moreton wavefront, with similar
  appearance as the subsequent sequential brightenings due to the wave
  passage. A slower diffuse moving front at 300 o 600 km/s is observed
  to trail the fast Moreton wavefront about 1 min after the onset. The
  Moreton wave decelerates to 550 km/s as it sweeps through F1. The
  wave passage results in oscillations throughout the entire filament,
  predominantly perpendicular to F1’s spine, a temporary disappearance
  of F3 and F4 followed by a gradual recovery, but no disturbance in
  F2. Different height and magnetic configuration together may account
  for the distinct responses of the filaments to the wave passage. The
  wavefront bulges at F4 whose spine is oriented perpendicular to the
  upcoming wavefront. The deformation of the wavefront is suggested to
  be due both to the forward inclination of the wavefront and to the
  enhancement of the local Alfven speed within the filament channel.

---------------------------------------------------------
Title: SDO/AIA and Hinode/EIS observations of interaction between
    an EUV wave and active region loops
Authors: Yang, Liheng; Zhang, Jun; Li, Ting; Liu, Wei
2013IAUS..294..567Y    Altcode:
  We study an EUV wave initiated in active region (AR) 11261 on 2011
  August 4 by using the SDO/AIA and the Hinode/EIS. We found that: (1)
  the EUV wave interacted with AR loops between AR 11261 and AR 11263,
  and exited mass flows in these loops. (2) EIS observations of AR loops
  in AR 11263 revealed that at the time of the wave transit, the original
  red-shifted feature had an increase of about 3 km s<SUP>-1</SUP>, and
  the original blue-shifted feature slightly weakened. These findings
  could be explained in the framework of a fast-mode magnetosonic wave
  interpretation for EUV waves.

---------------------------------------------------------
Title: UV and EUV Emissions at the Flare Foot-points Observed by AIA
Authors: Qiu, Jiong; Sturrock, Z.; Longcope, D.; Klimchuk, J. A.;
   Liu, W.
2013SPD....44...53Q    Altcode:
  A solar flare is composed of impulsive energy release events by magnetic
  reconnection, which forms and heats flare loops. Recent studies have
  revealed a two-phase evolution pattern of UV 1600A emission at the
  feet of these loops: a rapid pulse lasting for a few seconds to a
  few minutes, followed by a gradual decay on timescales of a few tens
  of minutes. Multiple band EUV observations by AIA further reveal
  very similar signatures. These two phases represent different but
  related signatures of an impulsive energy release in the corona. The
  rapid pulse is an immediate response of the lower atmosphere to an
  intense thermal conduction flux resulting from the sudden heating of
  the corona to high temperatures (we rule out energetic particles due
  to a lack of significant hard X-ray emission). The gradual phase is
  associated with the cooling of hot plasma that has been evaporated
  into the corona. The observed footpoint emission is again powered
  by thermal conduction (and enthalpy), but now during a period when
  approximate steady state conditions are established in the loop. UV
  and EUV light curves of individual pixels may therefore be separated
  into contributions from two distinct physical mechanisms to shed
  light on the nature of energy transport in a flare. We demonstrate
  this technique using coordinated, spatially resolved observations of
  UV and EUV emission from the footpoints of a C3.2 thermal flare.

---------------------------------------------------------
Title: An interferometric study of the Fomalhaut inner debris
    disk. III. Detailed models of the exozodiacal disk and its origin
Authors: Lebreton, J.; van Lieshout, R.; Augereau, J. -C.; Absil,
   O.; Mennesson, B.; Kama, M.; Dominik, C.; Bonsor, A.; Vandeportal,
   J.; Beust, H.; Defrère, D.; Ertel, S.; Faramaz, V.; Hinz, P.; Kral,
   Q.; Lagrange, A. -M.; Liu, W.; Thébault, P.
2013A&A...555A.146L    Altcode: 2013arXiv1306.0956L
  Context. Debris disks are thought to be extrasolar analogs to the
  solar system planetesimal belts. The star Fomalhaut harbors a cold
  debris belt at 140 AU comparable to the Edgeworth-Kuiper belt, as
  well as evidence of a warm dust component, unresolved by single-dish
  telescopes, which is suspected of being a bright analog to the solar
  system's zodiacal dust. <BR /> Aims: Interferometric observations
  obtained with the VLTI/VINCI instrument and the Keck Interferometer
  Nuller have identified near- and mid-infrared excesses attributed
  respectively to hot and warm exozodiacal dust residing in the inner few
  AU of the Fomalhaut environment. We aim to characterize the properties
  of this double inner dust belt and to unveil its origin. <BR />
  Methods: We performed parametric modeling of the exozodiacal disk
  ("exozodi") using the GRaTeR radiative transfer code to reproduce the
  interferometric data, complemented by mid- to far-infrared photometric
  measurements from Spitzer and Herschel. A detailed treatment of
  sublimation temperatures was introduced to explore the hot population
  at the size-dependent sublimation rim. We then used an analytical
  approach to successively testing several source mechanisms for the
  dust and suspected parent bodies. <BR /> Results: A good fit to the
  multiwavelength data is found by two distinct dust populations: (1)
  a population of very small (0.01 to 0.5 μm), hence unbound, hot dust
  grains confined in a narrow region (~0.1-0.3 AU) at the sublimation
  rim of carbonaceous material; (2) a population of bound grains at ~2
  AU that is protected from sublimation and has a higher mass despite
  its fainter flux level. We propose that the hot dust is produced by
  the release of small carbon grains following the disruption of dust
  aggregates that originate in the warm component. A mechanism, such
  as gas braking, is required to further confine the small grains for
  a long enough time. In situ dust production could hardly be ensured
  for the age of the star, so we conclude that the observed amount of
  dust is triggered by intense dynamical activity. <BR /> Conclusions:
  Fomalhaut may be representative of exozodis that are currently being
  surveyed at near and mid-infrared wavelengths worldwide. We propose a
  framework for reconciling the "hot exozodi phenomenon" with theoretical
  constraints: the hot component of Fomalhaut is likely the "tip of the
  iceberg" since it could originate in the more massive, but fainter,
  warm dust component residing near the ice line. This inner disk exhibits
  interesting morphology and can be considered a prime target for future
  exoplanet research. <P />Appendices are available in electronic form
  at <A href="http://www.aanda.org">http://www.aanda.org</A>

---------------------------------------------------------
Title: Poloidal ULF wave observed in the plasmasphere boundary layer
Authors: Liu, W.; Cao, J. B.; Li, X.; Sarris, T. E.; Zong, Q. -G.;
   Hartinger, M.; Takahashi, K.; Zhang, H.; Shi, Q. Q.; Angelopoulos, V.
2013JGRA..118.4298L    Altcode:
  report on a rare ultra-low-frequency (ULF) wave generation event
  associated with the formation of a plasmasphere boundary layer (PBL),
  which was well observed by one of the THEMIS satellites, TH-D, during
  subsequent outbound passes. On 13 September 2011, TH-D observed a sharp
  plasmapause at L = 3.4. The plasmasphere started to expand and continued
  to be refilled on 14 September. On 15 September, a PBL was formed with
  two density gradients at L = 4.4 and 6.5, respectively. Within the two
  density gradients, strong radial magnetic field and azimuthal electric
  field oscillations were observed, suggesting poloidal ULF waves. Based
  on the phase delay between magnetic and electric field signals, as well
  as the comparison between the observed wave frequency and predicted
  harmonic eigenfrequency, we find that the observed oscillations are
  second harmonic poloidal waves. Further investigation shows that the
  observed waves are likely generated by drift-bounce resonance with
  "bump-on-tail" plasma distributions at ~10 keV. We demonstrate that
  the waves are excited within the PBL where the eigenfrequency is close
  to the bounce frequency of these hot protons, but not outside the PBL
  where the eigenfrequency deviates from the bounce frequency. Finally,
  we suggest that cold plasma density seems to be a controlling factor
  for ULF wave generation as well, in addition to the bump-on-tail energy
  source, by altering eigenfrequency of the local field lines.

---------------------------------------------------------
Title: Funnel Prominences as Return Flows of the Chromosphere-Corona
Mass Cycle: SDO/AIA Observations of Coronal Condensation
Authors: Liu, Wei; Berger, T.; Low, B. C.
2013SPD....44...42L    Altcode:
  It has recently been proposed that prominences play an important role
  as return flows of the chromosphere-corona mass cycle, in which hot
  plasma is transported upward in forms of spicules and prominence bubbles
  (likely due to flux emergence), while cool plasma drains downward in
  forms of vertical prominence threads (Berger et al. 2011 Nature). A
  critical step in this cycle is the condensation of the million-degree
  coronal plasma into T&lt;10,000 K prominence material by a radiative
  cooling instability (i.e., thermal non-equilibrium), as numerically
  simulated (Karpen &amp; Antiochos 2008; Xia et al. 2012) and first
  evidenced in recent SDO/AIA observations (Liu et al. 2012; Berger et
  al. 2012 ApJL). Such a runaway cooling process occurs in coronal loops
  of various sizes and generally leads to condensation at magnetic dips
  and formation of funnel-shaped prominences. A moderate-sized prominence
  can drain a significant mass of typically 10^15 gram/day, which is
  comparable to the mass of a CME or a fraction of the entire corona. Here
  we present a survey of funnel prominences that appear to be common
  in AIA observations at various locations and times. We find longer
  cooling times in longer/taller coronal loops whose densities are lower,
  consistent with the expected quadratic dependence on density of the
  optically-thin radiative loss. We propose that such funnel prominences,
  usually small in size, can constitute a new type of prominences, and
  similar processes can produce elementary building blocks of large-scale
  quiescent prominences in filament channels. This picture is supported
  by the recent theoretical development on spontaneous formation of
  current sheets and condensations manifested as prominence threads
  (Low et al. 2012a, b, ApJ).Abstract (2,250 Maximum Characters): It
  has recently been proposed that prominences play an important role
  as return flows of the chromosphere-corona mass cycle, in which hot
  plasma is transported upward in forms of spicules and prominence bubbles
  (likely due to flux emergence), while cool plasma drains downward in
  forms of vertical prominence threads (Berger et al. 2011 Nature). A
  critical step in this cycle is the condensation of the million-degree
  coronal plasma into T&lt;10,000 K prominence material by a radiative
  cooling instability (i.e., thermal non-equilibrium), as numerically
  simulated (Karpen &amp; Antiochos 2008; Xia et al. 2012) and first
  evidenced in recent SDO/AIA observations (Liu et al. 2012; Berger et
  al. 2012 ApJL). Such a runaway cooling process occurs in coronal loops
  of various sizes and generally leads to condensation at magnetic dips
  and formation of funnel-shaped prominences. A moderate-sized prominence
  can drain a significant mass of typically 10^15 gram/day, which is
  comparable to the mass of a CME or a fraction of the entire corona. Here
  we present a survey of funnel prominences that appear to be common
  in AIA observations at various locations and times. We find longer
  cooling times in longer/taller coronal loops whose densities are lower,
  consistent with the expected quadratic dependence on density of the
  optically-thin radiative loss. We propose that such funnel prominences,
  usually small in size, can constitute a new type of prominences, and
  similar processes can produce elementary building blocks of large-scale
  quiescent prominences in filament channels. This picture is supported
  by the recent theoretical development on spontaneous formation of
  current sheets and condensations manifested as prominence threads
  (Low et al. 2012a, b, ApJ).

---------------------------------------------------------
Title: A new approach to model particle acceleration and energy
    transfer in solar flares
Authors: Rubio Da Costa, Fatima; Zuccarello, F.; Fletcher, L.;
   Labrosse, N.; Kasparova, J.; Prosecký, T.; Carlsson, M.; Petrosian,
   V.; Liu, W.
2013SPD....4440401R    Altcode:
  Motivated by available observations of two different flares in Lyα and
  Hα, we model the conditions of the solar atmosphere using a radiation
  hydrodynamics code (RADYN, Carlsson &amp; Stein, 1992) and analyze the
  energy transport carried by a beam of non-thermal electrons injected
  at the top of a 1D coronal loop. The numerical Lyα and Hα intensities
  match with the observations. The electron energy distribution is assumed
  to follow a power law of the form (E/E<SUP>c</SUP> )<SUB>-δ</SUB> for
  energies greater than a cutoff value of E<SUP>c</SUP>. Abbett &amp;
  Hawley (1999) and Allred et al. (2005) assumed that the non-thermal
  electrons flux injected at the top of a flaring loop, the cut-off energy
  and the power law index are constant over time. An improvement was
  achieved by Allred &amp; Hawley (2006), who modified the RADYN code
  in such a way that the input parameters were time dependent. Their
  inputs were based on observations of a flare obtained with RHESSI. By
  combining RADYN with the “flare” code from Stanford University
  which models the acceleration and transport of particles and radiation
  of solar flares in non-LTE regime, we can calculate the non-thermal
  electrons flux, the cut-off energy and the power law index at every
  simulated time step. The atmospheric parameters calculated by RADYN
  could in turn be used as updated inputs for "flare", providing several
  advantages over the results from Liu et al. (2009), who combined the
  particle acceleration code with a 1-D hydrodynamic code, improving
  the atmospheric conditions.

---------------------------------------------------------
Title: SDO AIA Observations of Large-Scale Coronal Propagating Fronts
Authors: Nitta, Nariaki; Schrijver, C. J.; Title, A. M.; Liu, W.
2013SPD....44...40N    Altcode:
  The discovery of "EIT waves" rekindled interests in what used to be
  called flare waves, which had been typically observed in H-alpha. In
  addition to Moreton waves, first observed at the Lockheed Solar
  Observatory, other manifestations of shock waves propagating in the
  corona include type II radio bursts and filament oscillations away from
  flare sites. Identification of EIT waves with the postulated fast-mode
  MHD shock waves in the corona has been questioned, however, largely
  because of their low speeds (e.g., 200-400 km/s). EIT's 10-20 minute
  cadence could be a contributing factor for this, and we need to find how
  fast large-scale coronal propagating fronts are in higher-cadence EUV
  images. It is clear that AIA on SDO is the best instrument at the moment
  for this type of work. With the availability of high-cadence full-disk
  images, we now can compare propagating fronts in different directions,
  and determine the highest speed of each event on AIA images more
  objectively and accurately than on EIT (and STEREO EUVI) images. In a
  large number of EIT wave events, we have measured speeds of propagating
  fronts using AIA's 193 A images. Before the fronts are deflected by the
  discontinuities, e.g., active regions and coronal holes, the mean and
  median speeds are 620 km/s and 600 km/s, respectively, and many exceed
  800 km/s. Higher speeds are often seen in events that accompany a type
  II burst, strong flare or energetic CME, but the distribution of the
  speed with these attributes is broad. We also find that the speeds of
  the large-scale coronal propagating fronts are not well correlated
  with those of the associated CMEs. Given that large-scale coronal
  propagating fronts at large distances represent freely propagating MHD
  waves, we discuss how to understand their nature close to their origins.

---------------------------------------------------------
Title: Asteroid Rotation Studies
Authors: Han, Xianming L.; Liu, W.; Sun, L.; Gao, S.; Shi, J.; Wang,
   S.; Pan, X.; Jiang, P.; Zhou, H.; Li, B.; Zhao, H.
2013AAS...22231502H    Altcode:
  During winter of 2012-2013, we measured the rotation periods of seven
  asteroids using the 0.9-m SARA North telescope located at the Kitt
  Peak National Observatory in Arizona and at the 0.6-m SARA South
  telescope located at the Cerro Tololo Inter-American Observatory in
  Chile. The asteroids that we carried out photometry studies include:
  1614 Goldschmidt, 1727 Mette, 2207 Antenor, 2616 Lesya, 2972 Niilo,
  4387 Tanaka, 34898 (2622 P-L). We will present their rotation periods,
  and compare with previous results where available.

---------------------------------------------------------
Title: Broad line and multi-wave luminosity relations in Fermi FSRQs
Authors: Xiong, D. R.; Zhang, H. J.; Zhang, X.; Zheng, Y. G.; Yi,
   T. F.; Liu, W. G.; Cha, Y. J.; Li, B. J.
2013Ap&SS.345..345X    Altcode: 2013Ap&SS.tmp...70X; 2013Ap&SS.tmp...59X
  We study broad line and multi-wave luminosity relations for 80
  flat-spectrum radio quasars (FSRQs) detected by Fermi LAT. Our results
  are as follows: for FSRQs, the correlations between log L <SUB> γ
  </SUB> and log L <SUB>BLR</SUB>, between log L <SUB>X</SUB> and log L
  <SUB>BLR</SUB>, between log L <SUB>O</SUB> and log L <SUB>BLR</SUB>,
  between log L <SUB>R</SUB> and log L <SUB>BLR</SUB> are significant;
  the correlation between log L <SUB>IR</SUB> and log L <SUB>BLR</SUB>
  ( P=0.08) is not significant, but might be refereed as a "trend"
  of significant correlation. These results support a close link
  between jet formation and accretion disk, and the L <SUB> γ </SUB>-
  L <SUB>BLR</SUB> correlation suggests that the radiation mechanism of
  the γ-ray emission in FSRQs is likely to be inverse Compton scattering
  of seed photons from BLR or outflowing BLR.

---------------------------------------------------------
Title: Evolution of neutron star + He star binaries: an alternative
    evolutionary  channel to intermediate-mass binary pulsars.
Authors: Chen, W. -C.; Liu, W. -M.
2013MNRAS.432L..75C    Altcode: 2013MNRAS.tmpL..93C; 2013arXiv1303.6155C
  It is difficult for intermediate-mass X-ray binaries to form compact
  intermediate-mass binary pulsars (IMBPs) with a short orbital-period
  ( ≲ 3 d), which have heavy ( ≳ 0.4 M<SUB>⊙</SUB>) CO or ONeMg
  white dwarf (WD) companions. Since neutron star + He star binaries
  may experience common-envelope evolution, they have some advantage
  to account for the formation of short orbital-period IMBPs. In this
  work, we explore the probability of IMBPs formed by this evolutionary
  channel. Using Eggleton's stellar evolution code, considering that
  the dead pulsars were spun up by the accreting material and angular
  momentum from the He star companions, we have calculated the evolution
  of a large number of neutron star + He star binaries. Our simulated
  results indicate that the NS + He star evolutionary channel can produce
  IMBPs with a WD of ∼ 0.5-1.1 M<SUB>⊙</SUB> and an orbital period of
  0.03-20 d, in which pulsars have a spin period of 1.4-200 ms. Comparing
  the calculated results with the observational parameters (spin period
  and orbital period) of nine compact IMBPs, the NS + He star evolutionary
  channel can account for the formation of four sources. Therefore,
  NS + He star binaries offer an alternative evolutionary channel to
  compact IMBPs.

---------------------------------------------------------
Title: Plasmoid Ejections and Loop Contractions in an Eruptive M7.7
Solar Flare: Evidence of Particle Acceleration and Heating in Magnetic
    Reconnection Outflows
Authors: Liu, Wei; Chen, Qingrong; Petrosian, Vahé
2013ApJ...767..168L    Altcode: 2013arXiv1303.3321L
  Where particle acceleration and plasma heating take place in relation
  to magnetic reconnection is a fundamental question for solar flares. We
  report analysis of an M7.7 flare on 2012 July 19 observed by SDO/AIA
  and RHESSI. Bi-directional outflows in forms of plasmoid ejections
  and contracting cusp-shaped loops originate between an erupting
  flux rope and underlying flare loops at speeds of typically 200-300
  km s<SUP>-1</SUP> up to 1050 km s<SUP>-1</SUP>. These outflows are
  associated with spatially separated double coronal X-ray sources with
  centroid separation decreasing with energy. The highest temperature
  is located near the nonthermal X-ray loop-top source well below the
  original heights of contracting cusps near the inferred reconnection
  site. These observations suggest that the primary loci of particle
  acceleration and plasma heating are in the reconnection outflow regions,
  rather than the reconnection site itself. In addition, there is an
  initial ascent of the X-ray and EUV loop-top source prior to its
  recently recognized descent, which we ascribe to the interplay among
  multiple processes including the upward development of reconnection
  and the downward contractions of reconnected loops. The impulsive
  phase onset is delayed by 10 minutes from the start of the descent,
  but coincides with the rapid speed increases of the upward plasmoids,
  the individual loop shrinkages, and the overall loop-top descent,
  suggestive of an intimate relation of the energy release rate and
  reconnection outflow speed.

---------------------------------------------------------
Title: The stability of an evolving Atlantic meridional overturning
    circulation
Authors: Liu, Wei; Liu, Zhengyu; Hu, Aixue
2013GeoRL..40.1562L    Altcode:
  In this study, we propose a generalized stability indicator, L, for
  a slowly evolving and quasi-steady Atlantic meridional overturning
  circulation (AMOC), which represents a feedback related to the AMOC
  and its associated freshwater transport within the Atlantic basin. As
  an improvement from previous indicators for the AMOC in equilibrium,
  this generalized indicator does not require a divergence-free freshwater
  transport in the Atlantic for a collapsed AMOC, which enables it to
  correctly monitor the AMOC stability through the AMOC hysteresis loop
  in the coupled atmosphere-ocean general circulation models. From the
  simulation, the indicator L suggests that the AMOC is in a stable
  regime, with single equilibrium under the present-day and the Last
  Glacial Maximum (LGM) climates. However, under the present-day climate,
  a Bering Strait (BS) closure will diminish the freshwater outflow from
  the North Atlantic into the Arctic as the AMOC collapses, resulting in a
  freshwater convergence in the Atlantic basin and making the AMOC reside
  in a stable collapsed state, i.e., the AMOC exhibits characteristics
  of multiple equilibria. Further analysis shows that the BS effect
  is much reduced under the LGM climate. This generalized indicator L
  has great implications for paleoclimate studies in understanding the
  abrupt climate change due to the instability of the AMOC.

---------------------------------------------------------
Title: A multi-fluid MHD Model for Sun-grazing comets
Authors: Jia, Ying-Dong; Russell, Christopher; Liu, Wei; Gombosi, Tamas
2013EGUGA..15.6348J    Altcode:
  Cometary plasma has been modeled with numerical codes for decades,
  to study its shock, contact surface and tail under nominal solar wind
  conditions. Recently, comets have been observed under very different
  conditions, the lower corona. This region contains plasma, orders of
  magnitude denser, and much stronger field. The cometary molecules are
  ionized much faster as well. Tail activity has been observed, providing
  a new way to study the plasma in coronal loops. In this study we model
  the charging-balanced cometary plasma, and its interaction with the
  lower corona. We simulate the momentum exchange between solar corona
  plasma and the cometary ions. Typical structures of the coronal field
  are studied to observe their effects on the tail, and to model the
  observed tail activity.

---------------------------------------------------------
Title: Recent Advances in Observations of Coronal EUV Waves
Authors: Liu, Wei; Ofman, Leon; Aschwanden, Markus J.; Nitta, Nariaki;
   Zhao, Junwei; Title, Alan M.
2013enss.confE..67L    Altcode:
  MHD waves can be used as seismological tools to decipher otherwise
  elusive physical parameters of the solar corona, such as the magnetic
  field strength and plasma density. Recent high cadence, high resolution,
  full-disk imaging observations from SDO/AIA have opened a new chapter
  in understanding these waves. Various types of EUV waves associated with
  flares/CMEs have been discovered or observed in unprecedented detail. In
  this talk, we will review such new observations, focusing on the
  following topics and their interrelationships: (1) quasi-periodic fast
  waves traveling along coronal funnels within CME bubbles at speeds up
  to 2000 km/s, associated with flare pulsations at similar frequencies;
  (2) quasi-periodic wave trains within broad, diffuse pulses of global
  EUV waves (so-called "EIT waves") running ahead of CME fronts; (3)
  interactions of global EUV waves with local coronal structures on
  their paths, such as flux-rope coronal cavities and their embedded
  filaments (kink oscillations) and coronal holes or active regions
  (deflections). We will discuss the implications of these observations
  on coronal seismology, on their roles in transporting energy through
  different parts of the solar atmosphere, and on understanding their
  associated eruptive flares/CMEs.

---------------------------------------------------------
Title: Heating of Flare Loops During a Two-ribbon Flare on 2011
    March 07 Observed by AIA and EVE
Authors: Liu, W. -J.; O'Hara, J.; Peck, C.; Qiu, J.; Longcope, D. W.
2013enss.confE.109L    Altcode:
  Recent high-resolution EUV observations have revealed that flare
  loops are formed and heated by reconnection events taking place
  successively. Our recent work shows that the rapidly rising phase of
  the UV emission at the foot-points of the flare loops could be used to
  infer the time profile of the impulsive heating rate. In this study,
  we analyze an M-class flare observed by AIA and EVE. We utilize the
  spatially resolved UV brightness time profiles to infer heating rates of
  a few thousand flux tubes anchored at the UV foot-points, and compute
  plasma evolution in each flux tube using the EBTEL model (Klimchuk
  et al. 2008, Cargrill et al. 2012). The coronal radiation is then
  calculated and compared with soft X-ray and EUV light curves observed
  by GOES and AIA. With a steady-state assumption, we also compute the
  transition-region DEM for each flux tube during its decay phase, and
  compare the predicted optically-thin transition-region emission in
  UV and EUV with AIA foot-points observations. The EUV emissions from
  both loops and foot points are also compared with irradiance observed
  by EVE. This study presents a method to infer heating functions of
  reconnection formed flare loops and how they affect evolution of the
  overlying corona as well as the lower-atmosphere dynamics coherently.

---------------------------------------------------------
Title: SDO AIA Observations of Large-Scale Coronal Disturbances in
    the Form of Propagating Fronts
Authors: Nitta, Nariaki V.; Schrijver, Carolus J.; Title, Alan M.;
   Liu, Wei
2013enss.confE.111N    Altcode:
  One of the most spectacular phenomena detected by SOHO EIT
  was the large-scale propagating fronts associated with solar
  eruptions. Initially these 'EIT' waves were thought to be coronal
  counterparts of chromospheric Moreton waves. However, different
  spatial and kinematic properties of the fronts seen in H-alpha and
  EUV images, and far more frequent occurrences of the latter have
  led to various interpretations that are still actively debated by
  a number of researchers. A major factor for the lack of closure was
  the various limitation in EIT data, including the cadence that was
  typically every 12 minutes. Now we have significantly improved data
  from SDO AIA, which have revealed some very interesting phenomena
  associated with EIT waves. However, the studies so far conducted
  using AIA data have primarily dealt with single or a small number of
  events, where selection bias and particular observational conditions
  may prevent us from discovering the general and true nature of EIT
  waves. Although automated detection of EIT waves was promised for
  AIA images some time ago, it is still not actually implemented in the
  data pipeline. Therefore we have manually found nearly 200 examples
  of large-scale propagating fronts, going through movies of difference
  images from the AIA 193 A channel up to January 2013. We present our
  study of the kinematic properties of the fronts in a subset of about
  150 well-observed events in relation with other phenomena that can
  accompany EIT waves. Our emphasis is on the relation of the fronts
  with the associated coronal eruptions often but not always taking
  the form of full-blown CMEs, utilizing STEREO data for a subset of
  more than 80 events that have occurred near the limb as viewed from
  one of the STEREO spacecraft. In these events, the availability of
  data from the STEREO inner coronagraph (COR1) as well as from the EUVI
  allows us to trace eruptions off the solar disk during the times of our
  propagating fronts. The representative relations between the fronts and
  CMEs will be discussed in terms of the evolution of EIT waves observed
  in different channels of AIA, which provide information of the thermal
  properties of the fronts. Our study will further clarify the variety
  of solar eruptions and their associated manifestations in the corona.

---------------------------------------------------------
Title: Bi-directional Ejections and Loop Contractions in an Eruptive
M7.7 Solar Flare: Evidence of Particle Acceleration and Heating in
    Magnetic Reconnection Outflows
Authors: Liu, Wei; Chen, Qingrong; Petrosian, Vahe
2013enss.confE.119L    Altcode:
  Where particle acceleration and plasma heating take place in relation
  to magnetic reconnection is a fundamental question for solar flares. We
  report analysis of an M7.7 flare on 2012 July 19 observed by SDO/AIA
  and RHESSI. Bi-directional ejections in forms of plasmoids and
  contracting cusp-shaped loops originate between an erupting flux rope
  and underlying flare loops at speeds of typically 200-300 km/s up to
  1050 km/s. These ejections are associated with spatially separated
  double coronal X-ray sources with centroid separation decreasing with
  energy. The highest temperature is located near the nonthermal X-ray
  loop-top source well below the original heights of contracting cusps
  near the inferred reconnection site. These observations suggest that
  the primary loci of particle acceleration and plasma heating are in
  the reconnection outflow regions, rather than the reconnection site
  itself. This supports particle acceleration by turbulence, shocks,
  and/or collapsing traps associated with reconnection outflows, not by
  a DC electric field within the reconnection region. In addition, there
  is an initial ascent of the X-ray and EUV loop-top source prior to its
  recently recognized descent. The impulsive phase onset is delayed by
  10 minutes from the start of the descent, but coincides with the rapid
  speed increases of the upward plasmoids, the individual loop shrinkages,
  and the overall loop-top descent, suggestive of an intimate relation
  of the energy release rate and reconnection outflow speed.

---------------------------------------------------------
Title: An Interferometric Study of the Fomalhaut Inner Debris
    Disk. II. Keck Nuller Mid-infrared Observations
Authors: Mennesson, B.; Absil, O.; Lebreton, J.; Augereau, J. -C.;
   Serabyn, E.; Colavita, M. M.; Millan-Gabet, R.; Liu, W.; Hinz, P.;
   Thébault, P.
2013ApJ...763..119M    Altcode: 2012arXiv1211.7143M
  We report on high-contrast mid-infrared observations of Fomalhaut
  obtained with the Keck Interferometer Nuller (KIN) showing a
  small resolved excess over the level expected from the stellar
  photosphere. The measured null excess has a mean value of 0.35% ± 0.10%
  between 8 and 11 μm and increases from 8 to 13 μm. Given the small
  field of view of the instrument, the source of this marginal excess
  must be contained within 2 AU of Fomalhaut. This result is reminiscent
  of previous VLTI K-band (sime2μm) observations, which implied the
  presence of a ~0.88% excess, and argued that thermal emission from hot
  dusty grains located within 6 AU from Fomalhaut was the most plausible
  explanation. Using a parametric two-dimensional radiative transfer code
  and a Bayesian analysis, we examine different dust disk structures to
  reproduce both the near- and mid-infrared data simultaneously. While
  not a definitive explanation of the hot excess of Fomalhaut, our model
  suggests that the most likely inner few AU disk geometry consists of
  a two-component structure, with two different and spatially distinct
  grain populations. The 2-11 μm data are consistent with an inner hot
  ring of very small (sime10-300 nm) carbon-rich grains concentrating
  around 0.1 AU. The second dust population—inferred from the KIN
  data at longer mid-infrared wavelengths—consists of larger grains
  (size of a few microns to a few tens of microns) located further out
  in a colder region where regular astronomical silicates could survive,
  with an inner edge around 0.4 AU-1 AU. From a dynamical point of view,
  the presence of the inner concentration of submicron-sized grains is
  surprising, as such grains should be expelled from the inner planetary
  system by radiation pressure within only a few years. This could either
  point to some inordinate replenishment rates (e.g., many grazing comets
  coming from an outer reservoir) or to the existence of some braking
  mechanism preventing the grains from moving out.

---------------------------------------------------------
Title: Reexamining the β decay of <SUP>53,54</SUP>Ni,
    <SUP>52,53</SUP>Co, <SUP>51</SUP>Fe, and <SUP>50</SUP>Mn
Authors: Su, J.; Liu, W. P.; Shu, N. C.; Yan, S. Q.; Li, Z. H.; Guo,
   B.; Huang, W. Z.; Zeng, S.; Li, E. T.; Jin, S. J.; Liu, X.; Wang,
   Y. B.; Lian, G.; Li, Y. J.; Chen, Y. S.; Bai, X. X.; Wang, J. S.;
   Yang, Y. Y.; Chen, R. F.; Xu, S. W.; Hu, J.; Chen, S. Z.; Ma, S. B.;
   Han, J. L.; Ma, P.; Hu, Q.; Ma, J. B.; Cao, X. G.; Jin, S. L.; Bai, Z.;
   Yang, K.; Shi, F. D.; Zhang, W.; Chen, Z.; Liu, L. X.; Lin, Q. Y.; Yan,
   X. S.; Zhang, X. H.; Fu, F.; He, J. J.; Li, X. Q.; He, C.; Smith, M. S.
2013PhRvC..87b4312S    Altcode:
  The β decay of <SUP>53,54</SUP>Ni, <SUP>52,53</SUP>Co, <SUP>51</SUP>Fe,
  and <SUP>50</SUP>Mn was investigated via the fragmentation of a
  <SUP>58</SUP>Ni primary beam with an energy of 68.6 MeV/u. The proton-γ
  coincidences of <SUP>53</SUP>Ni β-delayed proton emission were
  observed. Based on the analysis of the proton-γ coincidence events,
  it was inferred that the previous assignment of the excitation energy
  for the isobaric analog state in <SUP>53</SUP>Co may be problematic. The
  half-lives of these nuclei were obtained, in which the uncertainty of
  <SUP>52</SUP>Co half-life was reduced by a factor of 3. The half-lives
  were evaluated and used as inputs of nucleosynthesis calculations of
  the rapid proton-capture process in an x-ray burst.

---------------------------------------------------------
Title: Discovery of an unusual radio galaxy with a hybrid
    double-double and X-shaped morphology
Authors: Wang, C. C.; Zhou, H. Yan.; Ji, T.; Liu, W. J.; Jiang, N.
2013IAUS..290..323W    Altcode:
  We report the discovery of the first `X'-shaped double-double radio
  galaxy (DDRG), MRC0929+164 (J0932+1611), from FIRST radio survey. The
  intersection angle of the lines of two pairs of radio lobes is around
  20.6° for this object, much larger than other DDRGs. This unusual
  morphology may be a hint that the growth of its central super-massive
  black hole suffered a violent galaxy merger once.

---------------------------------------------------------
Title: TeV Cosmic-ray Proton and Helium Spectra in the Myriad Model
Authors: Bernard, Guilhem; Delahaye, Timur; Keum, Y. -Y.; Liu, Wei;
   Salati, Pierre; Taillet, Richard
2013ICRC...33..750B    Altcode:
  Recent measurements of cosmic ray proton and helium spectra show a
  hardening above a few hundred GeV. This excess is hard to understand
  in the framework of the conventional models of Galactic cosmic ray
  production and propagation. We propose to explain this anomaly by the
  presence of local sources (myriad model). We consistently derive the
  proton and helium fluxes between 50 GeV and 100 TeV by taking both local
  and remote sources for which a unique injection rate is assumed into
  account. We find cosmic ray propagation parameters compatible with B/C
  measurements for which the proton and helium spectra agree remarkably
  with the PAMELA and CREAM measurements over four decades in energy.

---------------------------------------------------------
Title: TSR versus non-TSR processes and their impact on gas
    geochemistry and carbon stable isotopes in Carboniferous, Permian
    and Lower Triassic marine carbonate gas reservoirs in the Eastern
    Sichuan Basin, China
Authors: Liu, Q. Y.; Worden, R. H.; Jin, Z. J.; Liu, W. H.; Li, J.;
   Gao, B.; Zhang, D. W.; Hu, A. P.; Yang, C.
2013GeCoA.100...96L    Altcode:
  The Palaeozoic and lowermost Mesozoic marine carbonate reservoirs of
  the Sichuan Basin in China contain variably sour and very dry gas. The
  source of the gas in the Carboniferous, Permian and Lower Triassic
  reservoirs is not known for certain and it has proved difficult to
  discriminate and differentiate the effects of thermal cracking- and
  TSR-related processes for these gases. Sixty-three gas samples were
  collected and analysed for their composition and carbon stable isotope
  values. The gases are all typically very dry (alkane gases being
  &gt;97.5% methane), with low (&lt;1%) nitrogen and highly variable
  H<SUB>2</SUB>S and CO<SUB>2</SUB>. Carboniferous gas is negligibly
  sour while the Lower Triassic gas tends to be most sour. The elevated
  H<SUB>2</SUB>S (up to 62%) is due to thermochemical sulphate reduction
  with the most sour Triassic and Permian reservoirs being deeper than
  4800 m. The non-TSR affected Carboniferous gas is a secondary gas that
  was derived from the cracking of sapropelic kerogen-derived oil and
  primary gas and is highly mature. Carboniferous (and non-sour Triassic
  and Permian) gas has unusual carbon isotopes with methane and propane
  being isotopically heavier than ethane (a reversal of typical low-
  to moderate-maturity patterns). The gas in the non-sour Triassic and
  Permian reservoirs has the same geochemical and isotopic characteristics
  (and therefore the same source) as the Carboniferous gas. TSR in the
  deepest Triassic reservoirs altered the gas composition reaching 100%
  dryness in the deepest, most sour reservoirs showing that ethane and
  propane react faster than methane during TSR. Ethane evolves to heavier
  carbon isotope values than methane during TSR leading to removal
  of the reversed alkane gas isotope trend found in the Carboniferous
  and non-sour Triassic and Permian reservoirs. However, methane was
  directly involved in TSR as shown by the progressive increase in its
  carbon isotope ratio as gas souring proceeded. CO<SUB>2</SUB> increased
  in concentration as gas souring proceeded, but typical CO<SUB>2</SUB>
  carbon isotope ratios in sour gases remained about -4‰ V-PDB showing
  that it was not solely derived from the oxidation of alkanes. Instead
  CO<SUB>2</SUB> may partly result from reaction of sour gas with
  carbonate reservoir minerals, such as Fe-rich dolomite or calcite,
  resulting in pyrite growth as well as CO<SUB>2</SUB>-generation.

---------------------------------------------------------
Title: Determination of the astrophysical
    <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O reaction rate from the
    <SUP>2</SUP>H(<SUP>12</SUP>N,<SUP>13</SUP>O)n reaction and its
    astrophysical implications
Authors: Guo, B.; Su, J.; Li, Z. H.; Wang, Y. B.; Yan, S. Q.; Li,
   Y. J.; Shu, N. C.; Han, Y. L.; Bai, X. X.; Chen, Y. S.; Liu, W. P.;
   Yamaguchi, H.; Binh, D. N.; Hashimoto, T.; Hayakawa, S.; Kahl, D.;
   Kubono, S.; He, J. J.; Hu, J.; Xu, S. W.; Iwasa, N.; Kume, N.; Li,
   Z. H.
2013PhRvC..87a5803G    Altcode: 2012arXiv1211.4972G
  The evolution of massive stars with very low-metallicities depends
  critically on the amount of CNO nuclides which they produce. The
  <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O reaction is an important branching
  point in the rap processes, which are believed to be alternative paths
  to the slow 3α process for producing CNO seed nuclei and thus could
  change the fate of massive stars. In the present work, the angular
  distribution of the <SUP>2</SUP>H(<SUP>12</SUP>N, <SUP>13</SUP>O)n
  proton transfer reaction at E<SUB>c.m.</SUB>=8.4 MeV has been measured
  for the first time. Based on the Johnson-Soper approach, the square
  of the asymptotic normalization coefficient (ANC) for the virtual
  decay of <SUP>13</SUP>O<SUB>g</SUB>.s. → <SUP>12</SUP>N+p was
  extracted to be 3.92±1.47 fm<SUP>-1</SUP> from the measured angular
  distribution and utilized to compute the direct component in the
  <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O reaction. The direct astrophysical
  S factor at zero energy was then found to be 0.39±0.15 keV b. By
  considering the direct capture into the ground state of <SUP>13</SUP>O,
  the resonant capture via the first excited state of <SUP>13</SUP>O and
  their interference, we determined the total astrophysical S factors
  and rates of the <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O reaction. The new
  rate is two orders of magnitude slower than that from the REACLIB
  compilation. Our reaction network calculations with the present
  rate imply that <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O will only compete
  successfully with the β<SUP>+</SUP> decay of <SUP>12</SUP>N at higher
  (∼2 orders of magnitude) densities than initially predicted.

---------------------------------------------------------
Title: Warm Debris Disks from WISE
Authors: Padgett, Deborah; Stapelfeldt, K. R.; Liu, W. M.; Leisawitz,
   D.; Krist, J. E.; Debes, J. H.; Fajardo-Acosta, S.; WISE Science Team
2013AAS...22140303P    Altcode:
  We report on an all-sky survey for warm debris disks in the solar
  neighborhood using data from the Wide-field Infrared Survey Explorer
  (WISE). Cross-correlation of robustly-detected WISE 22 micron
  sources with the Hipparcos 2 catalog yields 25,964 stars within
  120 pc of the Sun and 47,204 Tycho stars whose proper motions are
  suggestive of the same distance horizon. After careful vetting to
  exclude sources compromised by image artifacts, source confusion,
  and astronomical contaminants, a total of 508 Hipparcos and 296 Tycho
  high-confidence disk candidates emerge from the samples. Three hundred
  forty-six Hipparcos and 277 Tycho stars are newly-identified infrared
  excess stars. We have observed a subsample of the new FGK debris disk
  candidates with Herschel at 70 and 160 microns and find a mixture of
  warm and cold debris disks. In this talk, we will discuss the new WISE
  debris disks and their ongoing characterization.

---------------------------------------------------------
Title: Photometry Studies of Asteroids and Variable Stars
Authors: Han, Xianming; Li, B.; Zhao, H.; Liu, W.; Sun, L.; Gao, S.;
   Shi, J.; Wang, S.; Pan, X.; Jiang, P.; Zhou, H.
2013AAS...22144503H    Altcode:
  During the fall semester of 2012, we carried out extensive photometry
  studies of asteroids to obtain their rotation periods using the 0.9-m
  SARA North telescope located at the Kitt Peak National Observatory in
  Arizona and at the 0.6-m SARA South telescope located at the Cerro
  Tololo Inter-American Observatory in Chile. The asteroids that we
  carried out photometry studies include: 782 Montefiore, 3024 Hainan,
  3842 Harlansmith, 3920 Aubignan, 5542 Moffatt, 5951 AliceMone,
  6720 Gifu, 19978 1989VJ. We will present their rotation periods,
  and compare with previous results where available. During the course
  of photometry studies, we also discovered several variable stars. We
  will also present these new variable stars and their periods.

---------------------------------------------------------
Title: Numerical study of collisionless q = 1 double tearing
    instability in a cylindrical plasma
Authors: Wei, Lai; Yang, Xuefeng; Zheng, Shu; Liu, Yue; Liu
2012JPlPh..78..663W    Altcode:
  The double tearing mode (DTM) instability with two q <SUB>s</SUB>
  = 1 rational surfaces is investigated by taking into account the
  collisionless effects, including electron inertia and electron
  viscosity in a cylindrical geometry. The calculations show that for
  q-profile with a small distance between two rational surfaces, Δr
  <SUB>s</SUB>, there exists a broad linear spectrum of collisionless
  DTMs. The collisionless effects not only can significantly increase the
  linear growth rate of DTMs but can also enlarge the width of spectrum
  of unstable modes. For the q-profile with fixed Δr <SUB>s</SUB>
  and fixed magnetic shears at two rational surfaces, the high-order
  harmonics with smaller wavelength, such as the m/n = 2/2, 3/3 and 4/4
  modes, can be easily excited to have larger growth rates than the m/n
  = 1/1 mode by `lifting' the safety factor value between two rational
  surfaces. The characteristics of eigenmode structures of the most
  unstable and secondly unstable DTMs with various mode numbers are
  analyzed in detail and the corresponding collisionless scalings are
  numerically obtained and verified theoretically based on the previous
  relevant analytical theories. In addition, the synergetic effects of
  plasma resistivity, electron inertia and electron viscosity on the
  linear growth rates of DTMs are analyzed.

---------------------------------------------------------
Title: Quantifying Coronal Dimming as Observed in EUV and X-ray
    Images in Eruptive Events
Authors: Nitta, N. V.; Aschwanden, M. J.; Boerner, P.; Hill, S. M.;
   Lemen, J. R.; Liu, W.; Schrijver, C.; Wuelser, J.
2012AGUFMSH41A2097N    Altcode:
  Data from SOHO have shown that coronal dimming is closely related
  with coronal mass ejections (CMEs). In particular, dimming areas in
  EIT 195 A images often match the lateral extension of the associated
  CMEs. In this presentation, we summarize how CMEs compare with dimming
  as identified at different wavelengths and by other instruments, such as
  Yohkoh SXT, TRACE, GOES (12-15) SXI, STEREO EUVI and SDO AIA. Emphasis
  is placed on recent data, since the combination of AIA and STEREO
  data can lead us to better characterize CMEs and to more accurately
  estimate how much mass is ejected. We discuss technical issues that
  arise when quantifying dimming as a proxy for a CME. The issues include
  instrument calibration, effects of heating and cooling and integration
  along the line of sight. We also touch on the relation of dimming with
  globally propagating coronal fronts, which are routinely isolated in
  running difference images, and its implications on the magnitudes of
  the associated CMEs.

---------------------------------------------------------
Title: Observation and Theoretical Interpretation of Fermi Detected
    Solar Flares with Gamma-ray Emission &gt;100 MeV
Authors: Petrosian, V.; Chen, Q.; Liu, W.; Omodei, N.; Allafort, A.
2012AGUFMSH51C..06P    Altcode:
  With solar activity ramping up Fermi Space Telescope is accumulating
  data from increasing number of solar flares with some having
  substantial flux above 100 MeV, as detected by Fermi-Large Area
  Telescope. Unlike previous such detection by EGRET on board Compton
  Gamma-ray Observatory, some of the Fermi detections are not from
  powerful GOES X-class flares. We will review the observations of
  these flares by Fermi and other instruments, notably RHESSI, GOES,
  SDO and ground based observations. As examples of an impulsive and
  a long duration gamma-ray flare we will focus on the 2010 June 12
  and 2011 March 7-8 with 12 hours of gamma-ray emission. Based on the
  temporal and spectral characteristics of these flares we will discuss
  the competing processes (i) for production of the gamma-ray and other
  radiation (leptonic vs hadronic), (ii) affecting the transport of
  the accelerated particle (turbulence and field geometry), and (iii)
  those involved in determining the site (CME shock or flaring loop)
  and mechanism of the acceleration of particles into the GeV range
  (first or second order Fermi). This paper is presented on behalf of
  Fermi Collaboration.

---------------------------------------------------------
Title: Poloidal ULF wave observed in the plasmasphere boundary layer
Authors: Liu, W.; Cao, J.; Zong, Q.; Li, X.; Sarris, T. E.;
   Angelopoulos, V.
2012AGUFMSM33A..01L    Altcode:
  We investigate an event on the formation of a plasmasphere boundary
  layer and its effect on ULF wave generation observed by THEMIS
  satellites during three consecutive outbound passes. On September 13
  2011, TH-D observed a sharp plasmapause at L=3.4. The plasmasphere
  starts to expand and to be refilled on September 14th. On September
  15th, a plasmasphere boundary layer is formed with two density drops
  at L=4.5 and 6.5, respectively. Strong radial magnetic field and
  azimuthal electric field oscillations are observed within the two
  density gradients, suggesting poloidal ULF wave. Even mode signature
  and bump-on-tail plasma distribution at ~10keV observed in this event
  favour the mechanism of drift-bounce resonance. We suggest that
  the plasma density structures in plasmasphere boundary layers can
  provide conditions for resonances that could generate ULF waves. All
  the above features suggest that plasmasphere boundary layer may have
  impact on the generation of ULF wave and potential impact on radiation
  belt acceleration.

---------------------------------------------------------
Title: Three Dimensional Lunar Wake Reconstructed by the ARTEMIS Data
Authors: Zhang, H.; Khurana, K. K.; Kivelson, M. G.; Angelopoulos,
   V.; Zong, Q.; Pu, Z.; Hsu, T.; Wan, W.; Shi, Q.; Liu, W.
2012AGUFM.P43D1942Z    Altcode:
  Thanks to large data coverage of the ARTEMIS mission within the lunar
  wake, we reconstructed the lunar wake in a three dimensional manner
  by presenting distributions of key plasma and field parameters: the
  ion density, parallel and perpendicular temperatures, ion thermal
  pressure, magnetic pressure (field magnitude), total pressure, and
  field and flow perturbations. Our observations suggest that the wake
  is confined within a rarefaction front, which propagates at fast mode
  velocities in the rest frame of solar wind. When solar wind plasma is
  absorbed by the dayside lunar surface, a diamagnetic current system
  with thickness of ~2 ri forms on the surface of the Moon and initiates
  field disturbances there (bend and compression). These disturbances are
  controlled by the solar wind ion beta. In the wake behind the Moon, due
  to force unbalance, plasma reenters into the wake through perpendicular
  and parallel ways. In the perpendicular way, the inward flowing plasma
  continues to squeeze flux tubes in the wake, and thus enhances field
  magnitude there. In the parallel way, the refilling process presents
  more kinetic features, and leads to higher perpendicular temperature
  inside the wake. The refilling plasma from opposite sides of the
  wake may mix with each other significantly at ~6 RM downstream from
  the Moon, and the lunar wake is found to have fine structure within
  that distance. In addition, our data also shows that plasma may be
  decelerated by a total pressure gradient force in the direction against
  the background solar wind. Our observations thus establish a global
  lunar wake picture to be tested by theories or simulations.

---------------------------------------------------------
Title: Interaction of Cometary Material With the Solar Corona:
    EUV Observations and MHD Simulations
Authors: Liu, W.; Jia, Y.; Downs, C.; Schrijver, C.; Saint-Hilaire,
   P.; Battams, K.; Tarbell, T. D.; Shine, R. A.
2012AGUFMSH13B2254L    Altcode:
  Extreme ultraviolet (EUV) emission from two recent sun-grazing comets,
  C/2011 N3 and C/2011 W3 (Lovejoy), has been observed in the solar corona
  for the first time by the SDO/AIA and STEREO/EUVI instruments (Schrijver
  et al. 2011). These observations provided a unique opportunity to
  investigate the interaction of the cometary material with the solar
  corona and probe their physical conditions. We present here EUV
  observations and MHD simulations on this subject, focusing on the
  deceleration of the cometary tail material within the corona. We found
  that despite their different local coronal environments, the two comets
  exhibited quite similar characteristics. The initial EUV emitting tail
  had a projected velocity of 100-200 km/s, which was much lower than the
  orbital velocity of 500-600 km/s in the plane-of-sky. This indicates
  that significant deceleration had taken place while the tail material
  was heated to coronal temperatures on the order of 1 MK before it
  started to emit in EUV (Bryans &amp; Pesnell 2012). After its initial
  appearance, the tail further experienced a projected deceleration
  of ~1 km/s^2 (or 4 g_Sun). In particular, in the Lovejoy case, the
  tail appeared as clusters of bright parallel striations roughly at
  right angles to the orbit direction, suggestive of magnetic field
  lines illuminated by the plasma frozen onto them. These striations
  came to a stop and then accelerated in an opposite direction (seen
  in projection), approaching a constant velocity of ~50 km/s. These
  observations suggest that a Lorentz force from the coronal magnetic
  field was operating on the newly ionized cometary plasma. To test this
  hypothesis and understand tail deceleration mechanisms, we adopted a
  multi-fluid MHD model (Jia et al. 2012) to simulate the interaction
  between charged particles and the magnetized coronal plasma. We used
  potential extrapolation (Schrijver &amp; DeRosa 2003) and a more
  sophisticated global MHD model (Lionello et al. 2009) to infer the
  magnetic field and plasma conditions of the corona along the comet's
  orbit as inputs to the simulations. We will compare the observations and
  simulation results, and discuss the implications for using sun-grazing
  comets as probes to the solar corona in the context of NASA's future
  Solar Probe Plus mission.

---------------------------------------------------------
Title: Next Generation Auroral Imaging From Space
Authors: Spanswick, E. L.; Donovan, E.; Liu, W.; Unick, C.; Uritsky,
   V. M.
2012AGUFMSA13D..05S    Altcode:
  Geospace multi-scale dynamics are projected (albeit imperfectly)
  onto the upper atmosphere via the aurora, and consequently auroral
  observations provide us with our best way of observing geospace at the
  system-level. Over the last 40 years, there have been great successes
  in auroral imaging from space. Still, we must acknowledge that there
  are shortcomings. For example, true daylight suppression has eluded us,
  and the dynamic range of past auroral imagers has not been sufficient
  to allow for reliable determination of the open-closed boundary (OCB)
  from auroral images. As well, the spatial resolution of satellite-borne
  imagers to date has not been sufficient to enable tracking of dynamic
  auroral features such as arcs. Finally, all auroral imaging missions
  to date have been single satellite, so that we have never imaged
  complete sequences spanning long-duration processes such as storms and
  SMC events. Much more importantly, the inability to specify the OCB
  means we have never reliably measured the time series of open flux,
  and so the fundamental driver of all geospace dynamics has never been
  quantified. In terms of the underlying dynamics of geospace, we have
  yet to specify the space/time distribution of auroral structures
  across all relevant scales, so transients and the non-equilibrium
  cascade cannot be studied within the context of the overall system
  dynamics. In this talk, we present the results of a decade of planning
  for the "next generation" of auroral imaging. We discuss how new imaging
  technologies, flown on three-axis stabilized satellites will allow for
  accurate specification of the OCB at all local times, for near-perfect
  suppression of daylight and thus excellent dayside auroral imaging, and
  spatial resolution allowing for identification and tracking of arcs,
  patches, and other features that have never been imaged globally. We
  present the significant advantages of a two-satellite imaging mission
  as envisaged for the concepts of Canada's Ravens and PCW missions,
  and China's Kuafu B satellite pair. Finally, we argue that 24/7 "next
  generation" auroral imaging, complimented by equally innovative ENA
  and X-ray imaging, will form the cornerstone of what we call the Great
  Geospace Observatory.

---------------------------------------------------------
Title: If substorm onset triggers tail reconnection, what triggers
    substorm onset?
Authors: Liu, W. W.; Liang, J.; Donovan, E. F.; Spanswick, E.
2012JGRA..11711220L    Altcode:
  Despite the claim that tail reconnection triggers substorm onset,
  there is an abundance of cases wherein substorm onset triggers tail
  reconnection. In such cases, the first observable precursor to onset
  is a periodic rippling (beads) along an equatorward auroral arc. In
  this study, through an example, we show that substorms arising out
  of arcs of this type have the classical “inside-out” evolution,
  including the triggering of tail reconnection as a possible result. We
  then investigate what the magnetospheric mode underlying the ripples
  along the arcs might be. The classical MHD ballooning invoked by some
  substorm theories is inconsistent with the observation, which exhibits
  a finite azimuthal wavelength comparable to the local ion gyroradius
  and the propensity of onset to occur under moderately high (1-10)
  rather than extremely high plasma β. We show that the onset is due
  to a modified ballooning mode, subject to corrections by the General
  Ohm's Law and ion heat flux. The net result is that the necessary
  condition for the instability remains unchanged from the classical
  MHD, but the growth rate of the instability is heavily attenuated or
  quenched in the high β and short azimuthal wavelength limits. In
  the actual magnetosphere, the mode has a wavelength ∼1,500 km,
  growth timescale ∼10 s, and critical plasma beta in the 3-13 range,
  all consistent with observations.

---------------------------------------------------------
Title: Indirect measurements of reactions in hot p-p chain and
    CNO cycles
Authors: Wang, Y. B.; Guo, B.; Jin, S. J.; Li, Z. H.; Binh, D. N.;
   Hashimoto, H.; Hayakawa, S.; He, J. J.; Hu, J.; Iwasa, N.; Kahl,
   D. M.; Kubono, S.; Kume, N.; Li, E. T.; Li, Y. J.; Liu, X.; Su, J.;
   Xu, S. W.; Yamaguchi, H.; Yan, S. Q.; Zeng, S.; Bai, X. X.; Lian,
   G.; Wang, B. X.; Liu, W. P.
2012AIPC.1484...19W    Altcode:
  Several reactions have been experimentally studied, including
  the <SUP>12</SUP>N(d,n)<SUP>13</SUP>O and the ones induced by
  the <SUP>3</SUP>He+<SUP>12</SUP>C entrance channel. The former
  was carried out at the CRIB facility of University of Tokyo,
  aiming to indirectly determine the astrophysical reaction rates
  of the <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O reaction. For the
  <SUP>3</SUP>He+<SUP>12</SUP>C entrance channel, many excited states
  of several nuclei are populated and the angular distribution of each
  state is being analyzed.

---------------------------------------------------------
Title: SDO/AIA Detection of Solar Prominence Formation within a
    Coronal Cavity
Authors: Berger, Thomas E.; Liu, Wei; Low, B. C.
2012ApJ...758L..37B    Altcode: 2012arXiv1208.3431B
  We report the first analyses of SDO/AIA observations of the formation of
  a quiescent polar crown prominence in a coronal cavity. The He II 304 Å
  (log T <SUB>max </SUB> ~ 4.8 K) data show both the gradual disappearance
  of the prominence due to vertical drainage and lateral transport of
  plasma followed by the formation of a new prominence 12 hr later. The
  formation is preceded by the appearance of a bright emission "cloud"
  in the central region of the coronal cavity. The peak brightness of
  the cloud progressively shifts in time from the Fe XIV 211 Å channel,
  through the Fe XII 193 Å channel, to the Fe IX 171 Å channel (log T
  <SUB>max </SUB> ~ 6.2, 6.1, 5.8 K, respectively) while simultaneously
  decreasing in altitude. Filter ratio analysis estimates the initial
  temperature of the cloud to be approximately log T ~ 6.25 K with
  evidence of cooling over time. The subsequent growth of the prominence
  is accompanied by darkening of the cavity in the 211 Å channel. The
  observations imply prominence formation via in situ condensation of hot
  plasma from the coronal cavity, in support of our previously proposed
  process of magnetothermal convection in coronal magnetic flux ropes.

---------------------------------------------------------
Title: Resistive wall mode in cylindrical plasmas in the presence
    of surface currents
Authors: Cui, Shaoyan; Lu, Gaimin; Liu, Yue; Liu
2012JPlPh..78..501C    Altcode:
  Stability of the resistive wall mode in cylindrical plasmas confined by
  surface currents is investigated for the δ-function and step-function
  equilibrium surface-current profiles. For the former, it is shown that
  the perturbations oscillate and even decay for all locations of the
  initial perturbation. The entire system is stable and the plasma flow
  has little effect. For the step-function surface-current distribution,
  it is found that the thicker the surface current layer, the more stable
  is the system even if the largest initial perturbation is located on
  the rational surface, but the plasma flow also has little effect on
  the system.

---------------------------------------------------------
Title: The Black Hole Mass and Radio Characteristics of Radio Quasars
Authors: Xiong, D. R.; Zhang, X.; Zheng, Y. G.; Huang, B. R.; Mao,
   L. S.; Liu, W. G.
2012AcASn..53..369X    Altcode:
  In this paper, we collect the redshift, bolometric luminosity,
  full-width at half maximum (FWHM), monochromatic luminosity at
  5100&amp;:Aring;, radio loudness of 117 quasars, including 20 radio
  quiet quasars and 97 radio loud quasars. Then we calculate the black
  hole mass and Eddington ratio with the reverberation mapping method,
  and calculate the radio luminosity using total 5 GHz flux density. By
  analyzing the relations among them, our conclusions are as follows:
  (1) there are weak correlations between black hole mass and bolometric
  luminosity, between black hole mass and radio loudness, and between
  black hole mass and radio luminosity for radio quiet quasars (RQQs),
  while there are strong correlations between black hole mass and
  bolometric luminosity, between black hole mass and radio loudness,
  and between black hole mass and radio luminosity for radio loud
  quasars (RLQs); (2) there are weak correlations between bolometric
  luminosity and radio luminosity, and between bolometric luminosity and
  monochromatic luminosity at 5100Å for RQQs, while there are strong
  correlations between bolometric luminosity and radio luminosity, and
  between bolometric luminosity and monochromatic luminosity at 5100Å for
  RLQs; (3) the distributions of black hole mass, FWHM and Eddington ratio
  between RQQs and RLQs are different. From these results we suggest that
  the difference in black hole mass between RQQs and RLQs is predominantly
  due to the difference in FWHM between RQQs and RLQs; the difference
  between RQQs and RLQs is not due to the difference in orientation,
  but due to the difference in intrinsic property; the black hole mass,
  spin of black hole, Eddington ratio and morphology of host galaxy play
  an important role in explaining the origin of radio loudness and the
  radio loudness "bimodality"; there is a close link between the disk
  accretion rate and the generation of the relativistic radio jet.

---------------------------------------------------------
Title: Outward expansion of the lunar wake: ARTEMIS observations
Authors: Zhang, H.; Khurana, K. K.; Zong, Q. -G.; Kivelson, M. G.;
   Hsu, T. -S.; Wan, W. X.; Pu, Z. Y.; Angelopoulos, V.; Cao, X.; Wang,
   Y. F.; Shi, Q. Q.; Liu, W. L.; Tian, A. M.; Tang, C. L.
2012GeoRL..3918104Z    Altcode:
  Magnetohydrodynamics (MHD) predicts that lunar wake expands outward at
  magnetosonic velocities in all directions perpendicular to background
  solar wind; however, fluid theories emphasize that lunar wake expands
  outward at sound speeds mainly along the interplanetary magnetic field
  (IMF). Early observations supported the MHD predictions in the near-moon
  region despite lack of solar wind and IMF observations. Thanks to the
  special orbit design of the ARTEMIS mission, the solar wind conditions
  are well determined at the time of concurrent observations in the
  lunar wake. 164 wake crossings made by ARTEMIS are statistically
  studied in this paper. Observations indicated that, in either distant
  or near-Moon regions, the lunar wake expands outward at the fast
  MHD wave velocities. This simple model provides a powerful way to
  determine wake boundaries, particularly at large distances where the
  boundary signatures are indistinct, thus allowing further studies on
  the Moon-solar wind/crustal field-solar wind interactions.

---------------------------------------------------------
Title: New Determination of the <SUP>13</SUP>C(α, n)<SUP>16</SUP>O
    Reaction Rate and its Influence on the s-process Nucleosynthesis in
    AGB Stars
Authors: Guo, B.; Li, Z. H.; Lugaro, M.; Buntain, J.; Pang, D. Y.; Li,
   Y. J.; Su, J.; Yan, S. Q.; Bai, X. X.; Chen, Y. S.; Fan, Q. W.; Jin,
   S. J.; Karakas, A. I.; Li, E. T.; Li, Z. C.; Lian, G.; Liu, J. C.;
   Liu, X.; Shi, J. R.; Shu, N. C.; Wang, B. X.; Wang, Y. B.; Zeng, S.;
   Liu, W. P.
2012ApJ...756..193G    Altcode: 2012arXiv1208.0714G
  We present a new measurement of the α-spectroscopic factor (S
  <SUB>α</SUB>) and the asymptotic normalization coefficient for the
  6.356 MeV 1/2<SUP>+</SUP> subthreshold state of <SUP>17</SUP>O through
  the <SUP>13</SUP>C(<SUP>11</SUP>B, <SUP>7</SUP>Li)<SUP>17</SUP>O
  transfer reaction and we determine the α-width of this state. This is
  believed to have a strong effect on the rate of the <SUP>13</SUP>C(α,
  n)<SUP>16</SUP>O reaction, the main neutron source for slow
  neutron captures (the s-process) in asymptotic giant branch (AGB)
  stars. Based on the new width we derive the astrophysical S-factor
  and the stellar rate of the <SUP>13</SUP>C(α, n)<SUP>16</SUP>O
  reaction. At a temperature of 100 MK, our rate is roughly two times
  larger than that by Caughlan &amp; Fowler and two times smaller than
  that recommended by the NACRE compilation. We use the new rate and
  different rates available in the literature as input in simulations
  of AGB stars to study their influence on the abundances of selected
  s-process elements and isotopic ratios. There are no changes in the
  final results using the different rates for the <SUP>13</SUP>C(α,
  n)<SUP>16</SUP>O reaction when the <SUP>13</SUP>C burns completely
  in radiative conditions. When the <SUP>13</SUP>C burns in convective
  conditions, as in stars of initial mass lower than ~2 M <SUB>⊙</SUB>
  and in post-AGB stars, some changes are to be expected, e.g., of up to
  25% for Pb in our models. These variations will have to be carefully
  analyzed when more accurate stellar mixing models and more precise
  observational constraints are available.

---------------------------------------------------------
Title: Discovery of Kangite, (Sc,Ti,Al,Zr,Mg,Ca,□)2O3, a New
    Ultra-Refractory Mineral in Allende
Authors: Ma, C.; Tschauner, O.; Beckett, J. R.; Rossman, G. R.; Liu, W.
2012M&PSA..75.5004M    Altcode:
  Here we report the first occurrence of kangite in nature, as a new
  ultra-refractory mineral among the earliest solids formed in the solar
  system, and discuss its origin and significance for nebular processes.

---------------------------------------------------------
Title: The Hydromagnetic Interior of a Solar Quiescent
    Prominence. II. Magnetic Discontinuities and Cross-field Mass
    Transport
Authors: Low, B. C.; Liu, W.; Berger, T.; Casini, R.
2012ApJ...757...21L    Altcode:
  This second paper of the series investigates the transverse response
  of a magnetic field to the independent relaxation of its flux tubes
  of fluid seeking hydrostatic and energy balance, under the frozen-in
  condition and suppression of cross-field thermal conduction. The
  temperature, density, and pressure naturally develop discontinuities
  across the magnetic flux surfaces separating the tubes, requiring the
  finite pressure jumps to be compensated by magnetic-pressure jumps in
  cross-field force balance. The tangentially discontinuous fields are
  due to discrete currents in these surfaces, δ-function singularities
  in the current density that are fully admissible under the rigorous
  frozen-in condition but must dissipate resistively if the electrical
  conductivity is high but finite. The magnetic field and fluid must
  thus endlessly evolve by this spontaneous formation and resistive
  dissipation of discrete currents taking place intermittently in
  spacetime, even in a low-β environment. This is a multi-dimensional
  effect in which the field plays a central role suppressed in the
  one-dimensional (1D) slab model of the first paper. The study begins
  with an order-of-magnitude demonstration that of the weak resistive
  and cross-field thermal diffusivities in the corona, the latter is
  significantly weaker for small β. This case for spontaneous discrete
  currents, as an important example of the general theory of Parker, is
  illustrated with an analysis of singularity formation in three families
  of two-dimensional generalizations of the 1D slab model. The physical
  picture emerging completes the hypothesis formulated in Paper I that
  this intermittent process is the origin of the dynamic interiors of
  a class of quiescent prominences revealed by recent Hinode/SOT and
  SDO/AIA high-resolution observations.

---------------------------------------------------------
Title: A dipole pattern of the sea surface height anomaly in the
North Atlantic: 1990s-2000s
Authors: Li, Feili; Jo, Young-Heon; Liu, W. Timothy; Yan, Xiao-Hai
2012GeoRL..3915604L    Altcode:
  Despite a long-term trend of sea level rise continuing into the 2000s
  in the subpolar North Atlantic, variations in the sea surface height
  have behaved differently in both spatial and temporal domains. A dipole
  pattern, centered between the Northern Atlantic subpolar region and
  the region near the Gulf Stream, was observed in the linear trends
  of the sea surface height anomaly (SSHA). By applying the Ensemble
  Empirical Mode Decomposition (EEMD), we found that this dipole pattern
  is mainly associated with the interannual to decadal SSHA oscillations
  of the two regions, which are 180° out of phase with each other over
  the time span of this study. The low-frequency variations of the
  SSHA in the subpolar region are strongly inversely correlated with
  the cumulative North Atlantic Oscillation (NAO) index (r = -0.84), in
  contrast with the Gulf Stream region, which is positively correlated (r
  = 0.22). This therefore reveals an asymmetric response of the regional
  SSHA to the cumulative NAO-forcing, in which the subpolar variability
  leads that of the Gulf Stream region by 29 months. Moreover, there is
  a remarkable reversal of the SSHA trends from the 1990s to the 2000s,
  which is unexpected given a weak and fluctuating NAO behavior since
  mid-1990s. Such SSHA variations in the 2000s might be related to the
  lagged variations of the Atlantic meridional overturning circulation
  (AMOC).

---------------------------------------------------------
Title: Interaction of solar wind pressure pulses with the
magnetosphere: IMF modulation and cavity mode
Authors: Liu, W. W.
2012JGRA..117.8234L    Altcode: 2012JGRA..11708234L
  Energy transfer through the magnetopause involves an interplay of
  two processes. On one hand, microphysics of reconnection determines
  how easily the magnetopause can be opened. On the other hand, the
  global state of the solar wind and magnetosphere determines how much
  energy is available for transfer and whether there exist "resonant"
  interactions whereby the transfer is particularly efficient. In
  the case of solar wind pressure pulses, empirical evidence has
  suggested that the solar wind-magnetosphere interaction can become
  unusually intense, leading to large-scale global auroral response and
  occasionally geomagnetic storms. In this study, for the first time,
  magnetic reconnection and global magnetospheric oscillation known as
  the cavity mode are integrated to give a comprehensive description of
  energy transfer through the dayside magnetopause. Using a heuristic
  model in which the inflow into the magnetopause is proportional to the
  magnitude of pressure pulse and an IMF proxy, we derive the fractions
  of energy converted to reconnection and field-line resonance per unit
  incident compressional energy in a pressure pulse. It is found that the
  magnitude of energy transfer is modulated by the IMF proxy, whereas
  the frequency spectrum of the transfer is modulated by the cavity
  mode. Under extreme conditions, reconnection can transfer almost 100%
  of incident compressional energy at the maximum absorption bands. Even
  under the typical value reconnection rate (∼0.1), approximately 30%
  of the incident energy can be absorbed in these bands. The frequency
  response of reconnection transfer has pulse-like peaks in the &gt;3 mHz
  range and rather insensitive to the solar wind and wave parameters. In
  contrast, the frequency response of the shear-Alfvénic transfer
  centers in the 1-4 mHz range and has a more broadband shape that is
  significantly influenced by the solar wind density.

---------------------------------------------------------
Title: The Hydromagnetic Interior of a Solar Quiescent
    Prominence. I. Coupling between Force Balance and Steady Energy
    Transport
Authors: Low, B. C.; Berger, T.; Casini, R.; Liu, W.
2012ApJ...755...34L    Altcode: 2012arXiv1203.1056L
  This series of papers investigates the dynamic interiors of quiescent
  prominences revealed by recent Hinode and SDO/AIA high-resolution
  observations. This first paper is a study of the static equilibrium
  of the Kippenhahn-Schlüter diffuse plasma slab, suspended vertically
  in a bowed magnetic field, under the frozen-in condition and subject
  to a theoretical thermal balance among an optically thin radiation,
  heating, and field-aligned thermal conduction. The everywhere-analytical
  solutions to this nonlinear problem are an extremely restricted subset
  of the physically admissible states of the system. For most values
  of the total mass frozen into a given bowed field, force balance
  and steady energy transport cannot both be met without a finite
  fraction of the total mass having collapsed into a cold sheet of zero
  thickness, within which the frozen-in condition must break down. An
  exact, resistive hydromagnetic extension of the Kippenhahn-Schlüter
  slab is also presented, resolving the mass-sheet singularity into
  a finite-thickness layer of steadily falling dense fluid. Our
  hydromagnetic result suggests that the narrow, vertical prominence
  H<SUB>α</SUB> threads may be falling across magnetic fields, with
  optically thick cores much denser and ionized to much lower degrees than
  conventionally considered. This implication is discussed in relation
  to (1) the recent SDO/AIA observations of quiescent prominences that
  are massive and yet draining mass everywhere in their interiors, (2)
  the canonical range of 5-60 G determined from spectral polarimetric
  observations of prominence magnetic fields over the years, and (3)
  the need for a more realistic multi-fluid treatment.

---------------------------------------------------------
Title: Quasi-periodic Fast-mode Wave Trains within a Global EUV Wave
    and Sequential Transverse Oscillations Detected by SDO/AIA
Authors: Liu, Wei; Ofman, Leon; Nitta, Nariaki V.; Aschwanden, Markus
   J.; Schrijver, Carolus J.; Title, Alan M.; Tarbell, Theodore D.
2012ApJ...753...52L    Altcode: 2012arXiv1204.5470L
  We present the first unambiguous detection of quasi-periodic wave
  trains within the broad pulse of a global EUV wave (so-called EIT wave)
  occurring on the limb. These wave trains, running ahead of the lateral
  coronal mass ejection (CME) front of 2-4 times slower, coherently
  travel to distances &gt;~ R <SUB>⊙</SUB>/2 along the solar surface,
  with initial velocities up to 1400 km s<SUP>-1</SUP> decelerating to
  ~650 km s<SUP>-1</SUP>. The rapid expansion of the CME initiated at
  an elevated height of 110 Mm produces a strong downward and lateral
  compression, which may play an important role in driving the primary
  EUV wave and shaping its front forwardly inclined toward the solar
  surface. The wave trains have a dominant 2 minute periodicity that
  matches the X-ray flare pulsations, suggesting a causal connection. The
  arrival of the leading EUV wave front at increasing distances produces
  an uninterrupted chain sequence of deflections and/or transverse (likely
  fast kink mode) oscillations of local structures, including a flux-rope
  coronal cavity and its embedded filament with delayed onsets consistent
  with the wave travel time at an elevated (by ~50%) velocity within
  it. This suggests that the EUV wave penetrates through a topological
  separatrix surface into the cavity, unexpected from CME-caused magnetic
  reconfiguration. These observations, when taken together, provide
  compelling evidence of the fast-mode MHD wave nature of the primary
  (outer) fast component of a global EUV wave, running ahead of the
  secondary (inner) slow component of CME-caused restructuring.

---------------------------------------------------------
Title: Keck Interferometer Nuller science highlights
Authors: Mennesson, Bertrand; Millan-Gabet, Rafael; Colavita, M. M.;
   Serabyn, E.; Hinz, P.; Kuchner, M.; Liu, W.; Barry, R.; Stark, C.;
   Ragland, S.; Woillez, J.; Traub, W.; Absil, O.; Defrère, Denis;
   Augereau, J. C.; Lebreton, J.
2012SPIE.8445E..07M    Altcode:
  We report here on some of the major astronomical observations obtained
  by the Keck Interferometer Nuller (KIN), the high dynamic range
  instrument recombining the Keck Telescopes at wavelengths of 8 to 13
  microns. A few science targets were observed during the commissioning
  phase (2004-2007). These early observations aimed at demonstrating the
  KIN’s ability to spatially resolve and characterize circumstellar
  dust emission around a variety of targets, ranging from evolved stars
  to young debris disks. Science operations started then in 2008 with
  the more demanding KIN exozodi key science programs, augmented by
  observations of YSOs and hot debris disks between 2009 and 2011. The
  last KIN observations were gathered in 2011B, and the interpretation
  of some of the results depicted here is still preliminary (exo-zodi
  survey) or pending (complicated behavior observed in YSOs). We discuss
  in particular the initial results of the KIN’s exo-zodi observations,
  which targeted a total of 40 nearby main sequence single stars. We look
  for trends in this sample, searching for possible correlations between
  the measured KIN excesses and basic stellar properties such as spectral
  type or the presence of dust inferred from separate observations.

---------------------------------------------------------
Title: Large-Scale Coronal Disturbances as Observed by SDO AIA
Authors: Nitta, Nariaki; Schrijver, Carolus; Title, Alan; Lemen,
   James; Liu, Wei
2012cosp...39.1378N    Altcode: 2012cosp.meet.1378N
  With increasing solar activity, the Atmospheric Imaging Assembly
  (AIA) on the Solar Dynamics Observatory (SDO) has observed a number
  of large-scale coronal disturbances, which may correspond to what we
  have generally known as "EIT waves." Although their nature is still
  actively debated, these disturbances usually accompany CMEs. In certain
  cases, the fronts of the disturbances may signify CME-related shock
  waves important for particle acceleration. Using the unprecedented
  temporal resolution and broad temperature coverage of the AIA, we have
  studied more than 100 such events. Here we discuss their kinematics
  characterized by faster fronts than EIT waves in Solar Cycle 23, and
  spatial relations with CMEs using STEREO data that provide triangulation
  of the fronts. We also try plasma diagnostic using images in different
  filters. Association of these disturbances with CMEs, flares and type
  II bursts is discussed on a statistical basis. Lastly, we explore the
  possible relation of the larger-scale coronal disturbances with SEP
  events observed at widely separate longitudes and their onset times.

---------------------------------------------------------
Title: Slow-Mode Oscillations of Hot Loops Excited at Flaring
    Footpoints
Authors: Wang, T.; Liu, W.; Ofman, L.; Davila, J.
2012ASPC..456..127W    Altcode: 2017arXiv170605427W
  The analysis of a hot loop oscillation event using SOHO/SUMER,
  GOES SXI, and RHESSI observations is presented. Damped Doppler shift
  oscillations were detected in the Fe xix line by SUMER, and interpreted
  as a fundamental standing slow mode. The evolution of soft X-ray
  emission from GOES/SXI and hard X-ray sources from RHESSI suggests
  that the oscillations of a large loop are triggered by a small flare,
  which may be produced by interaction (local reconnection) of this
  large loop with a small loop at its footpoint. This study provides
  clear evidence supporting our early conjecture that the slow-mode
  standing waves in hot coronal loops are excited by impulsive heating
  (small or microflares) at the loop's footpoint.

---------------------------------------------------------
Title: The Journey of Sungrazing Comet Lovejoy
Authors: Bryans, Paul; A'Hearn, M.; Battams, K.; Biesecker, D.;
   Bodewits, D.; Boice, D.; Brown, J.; Caspi, A.; Chodas, P.; Hudson,
   H.; Jia, Y.; Jones, G.; Keller, H. U.; Knight, M.; Linker, J.; Lisse,
   C.; Liu, W.; McIntosh, S.; Pesnell, W. D.; Raymond, J.; Saar, S.;
   Saint-Hilaire, P.; Schrijver, C.; Snow, M.; Tarbell, T.; Thompson,
   W.; Weissman, P.; Comet Lovejoy Collaboration Team
2012AAS...22052507B    Altcode:
  Comet Lovejoy (C/2011 W3) was the first sungrazing comet, observed
  by space-based instruments, to survive perihelion passage. First
  observed by ground-based telescopes several weeks prior to perihelion,
  its journey towards the Sun was subsequently recorded by several solar
  observatories, before being observed in the weeks after perihelion by
  a further array of space- and ground-based instruments. Such a surfeit
  of wide-ranging observations provides an unprecedented insight into
  both sungrazing comets themselves, and the solar atmosphere through
  which they pass. This paper will summarize what we have learnt from the
  observations thus far and offer some thoughts on what future sungrazing
  comets may reveal about comets, the Sun, and their interaction.

---------------------------------------------------------
Title: SDO/AIA Detection of Quasi-periodic Wave Trains Within Global
    EUV ("EIT") Waves and Their Coronal Seismology Implications
Authors: Liu, Wei; Ofman, L.; Aschwanden, M. J.; Nitta, N.; Schrijver,
   C. J.; Title, A. M.; Tarbell, T. D.
2012AAS...22051501L    Altcode:
  The nature of global EUV waves (so-called "EIT waves") has long
  been under debate because of instrumental limitations and projection
  effects when viewed on the solar disk. We present here high cadence
  SDO/AIA observations of global EUV waves occurring on the limb. We
  report newly discovered quasi-periodic wave trains located in the low
  corona within a broad, diffuse pulse of the global EUV wave ahead of
  the lateral CME front/flank. These waves coherently travel to large
  distances on the order of 1 solar radii with initial velocities up
  to 1400 km/s. They have dominant 1-3 minute periodicities that often
  match the X-ray pulsations of the accompanying flare, suggestive of
  a causal connection. In addition, recently discovered quasi-periodic
  fast propagating (QFP) waves of 1000-2000 km/s (Liu, Title, Zhao et
  al. 2011 ApJL) are found in the funnel of coronal loops rooted at the
  flare kernel. These waves are spatially confined within the CME bubble
  and rapidly disappear while approaching the CME front, suggestive
  of strong damping and/or dispersion. These observations provide new
  evidence of the fast-mode wave nature of the primary, fast component
  of a global EUV wave, running ahead of a secondary, slow component
  of CME-caused restructuring of the coronal magnetic field. We suggest
  that the two types of quasi-periodic waves are both integral parts of
  global coronal dynamics manifested as a CME/flare eruption, and they
  have important implications for global and local coronal seismology.

---------------------------------------------------------
Title: WISE Photometry of Young Stellar Object Candidates in the
    Canis Major Star-Forming Region
Authors: Padgett, Deborah; Liu, W.; Rebull, L.; Leisawitz, D.
2012AAS...22033403P    Altcode:
  We present WISE (Wide-field Infrared Survey Explorer) photometry
  of young stellar object candidates in the Canis Major clouds at a
  distance of 1 kpc. WISE has identified 682 objects with apparent 12
  and 22 micron excess emission in a 7 deg x 10 deg field around the
  the CMa R1 cloud. While a substantial fraction of these candidates
  are likely galaxies, AGB stars, and artifacts from confusion along
  the galactic plane, others are part of a spectacular cluster of
  YSOs imaged by WISE along a dark filament in the R1 cloud. Palomar
  Double Spectrograph observations of several sources in this cluster
  confirm their identity as young A and B stars with strong emission
  lines. In this contribution,we plot the optical - mid-infrared spectral
  energy distribution for the WISE YSO candidates and discuss potential
  contaminants to the sample. The data demonstrate the utility of WISE
  in performing wide-area surveys for young stellar objects.

---------------------------------------------------------
Title: SDO/AIA Observations of Sustained Coronal Condensation in
    Prominences as Return Flows of the Chromosphere-Corona Mass Cycle
Authors: Liu, Wei; Berger, T.; Low, B. C.
2012AAS...22020708L    Altcode:
  It has recently been proposed that prominences are manifestations
  of a magneto-thermal convection process that involves ever-present
  dynamic descents of cool material threads and upflows of hot bubbles
  (Berger et al. 2011 Nature). On global scales, prominences may play
  an important role as the return flows of the chromosphere-corona
  mass cycle, in which hot mass is originally transported upward
  through spicules. A critical step in this cycle is the condensation of
  million-degree coronal plasma into T&lt;10,000 K prominence material by
  radiative cooling instability. However, direct observation of coronal
  condensation has been difficult in the past, a situation recently
  changed. We present here the first example observed with SDO/AIA,
  in which hours of gradual cooling through multiple EUV channels (from
  2 MK to 80,000 K) in large-scale loops leads to eventual condensation
  at magnetic dips, where we find evidence of magnetic reconnection and
  subsequent outflows. A moderate-size prominence of 10^14 gram is then
  formed. Its mass is not static but maintained by a continual supply
  through condensation at a high rate of 10^10 gram/s against a comparable
  drainage through numerous vertical threads at less than free-fall
  speeds. Most of the total condensation of 10^15 gram, comparable
  to a CME mass and an order of magnitude more than the instantaneous
  mass of the prominence itself, is drained in merely one day. These
  new observations show that a macroscopically quiescent prominence is
  microscopically dynamic (Liu, Berger, Low 2012 ApJL), involving the
  passage of a significant mass that bears important implications for
  the chromosphere-corona mass cycle. This interpretation is further
  supported by the recent theoretical development on spontaneous formation
  of current sheets and cool condensations (Low, Berger, Casini, &amp;
  Liu, 2012 submitted to ApJ).

---------------------------------------------------------
Title: Coupling of Particle Acceleration and Atmospheric Dynamic
    Response to Impulsive Energy Release in Solar Flares
Authors: Liu, Wei; Petrosian, V.; Chen, Q.; Mariska, J.
2012AAS...22020419L    Altcode:
  In solar flares, acceleration and transport of high-energy particles
  and fluid dynamics of the atmospheric plasma are interrelated
  processes coupled in a circular chain. Chromospheric evaporation,
  for example, can alter the density and temperature distribution
  along the flare loop, in particular in the acceleration site near
  the loop-top source. This produces a feedback on particle collisional
  heating, and more importantly on the energy release and acceleration
  process. This in turn will change the heating of the chromosphere and
  mass flows in the corona. In recent years, there have been increasing
  theoretical and observational motivations to investigate these coupled
  processes together in a self-consistent manner. We present here combined
  Fokker-­Planck modeling of particles and hydrodynamic simulation of
  flare plasma. We extended our earlier hybrid simulation (Liu, Petrosian,
  Mariska 2009) by feeding the updated plasma density and temperature at
  the loop-top source to the stochastic acceleration process. We find
  that the density enhancement causes the ratio of the electron plasma
  frequency to gyro-frequency to increase. This can lead to the reduction
  of the efficiency of electron acceleration and thus the quenching
  or spectral softening of nonthermal hard X-ray tails observed during
  the late stages of flares. This also affects the relative production
  of energetic electrons vs. protons (Petrosian and Liu 2004). We will
  compare our results with recent observations from RHESSI, SDO, and
  Hinode. We will also discuss their implications for cyclic spectral
  hardening, quasi-periodic flare pulsations, and recently imaged
  super-fast quasi-periodic coronal waves originating from flare kernels.

---------------------------------------------------------
Title: Impulsively Driven Waves And Flows In Coronal Active Regions
Authors: Ofman, Leon; Wang, T.; Davila, J. M.; Liu, W.
2012AAS...22032204O    Altcode:
  Recent SDO/AIA and Hinode EIS observations indicate that both (super)
  fast and slow magnetosonic waves are present in active region (AR)
  magnetic structures. Evidence for fast (100-300 km/s) impulsive flows
  is found in spectroscopic and imaging observations of AR loops. The
  super-fast waves were observed in magnetic funnels of ARs. The
  observations suggest that waves and flow are produced by impulsive
  events, such as (micro) flares. We have performed three-dimensional
  magnetohydrodynamic (3D MHD) simulations of impulsively generated
  flows and waves in coronal loops of a model bi-polar active region
  (AR). The model AR is initiated with a dipole magnetic field and
  gravitationally stratified density, with impulsively driven flow at
  the coronal base of the AR in localized magnetic field structures. We
  model the excitation of the flows in hot (6MK) and cold (1MK) active
  region plasma, and find slow and fast magnetosonic waves produced by
  these events. We also find that high-density (compared to surrounding
  corona) loops are produced as a result of the upflows. We investigate
  the parametric dependence between the properties of the impulsive
  flows and the waves. The results of the 3D MHD modeling study supports
  the conjecture that slow magnetosonic waves are often produced by
  impulsive upflows along the magnetic field, and fast magnetosonic
  waves can result from impulsive transverse field line perturbations
  associated with reconnection events. The waves and flows can be used
  for diagnostic of AR structure and dynamics.

---------------------------------------------------------
Title: Some Like it Hot: the Trajectory of Sungrazing Comet C/2011 W3
    (Lovejoy) in the Solar Neighborhood.
Authors: Saint-Hilaire, Pascal; Chodas, P. W.; Battams, K.; Tarbell,
   T. D.; Shine, R. A.; Liu, W.; Thompson, W. T.; Comet Lovejoy
   Collaboration Team
2012AAS...22052107S    Altcode:
  Sungrazing comet Lovejoy (C/2011 W3) was a recent spectacle in the sky,
  observed from the ground and by a host of space-based instruments,
  including several solar observatories. It is the first sungrazing comet
  in recent memory to have survived perihelion (q 1.2 Rs). It is only
  the second sungrazer to have been observed in the Sun's low corona in
  the extreme ultra-violet (EUV), where a plethora of EUV observations
  were obtained by the SDO and STEREO spacecraft. Such an occurrence
  can be used to probe the solar corona and test our understanding
  of plasma and cometary physics. In this work, we use the best orbit
  elements currently available to plot the path of the comet's nucleus on
  solar EUV images from SDO/AIA, both STEREO/EUVIs, and yellow continuum
  (near the Na D lines) images from Hinode/SOT. We compare the predicted
  positions and timing of the comet's nucleus to the latter, while the
  SDO and STEREO EUV observations are used to estimate the distance at
  which the EUV tail appears behind the comet's nucleus.

---------------------------------------------------------
Title: Large-scale Coronal Disturbances As Observed By SDO AIA
Authors: Nitta, Nariaki; Schrijver, C.; title, A.; Liu, W.; Lemen, J.
2012AAS...22051502N    Altcode:
  With increasing solar activity, the Atmospheric Imaging Assembly
  (AIA) on the Solar Dynamics Observatory (SDO) has observed a number
  of large-scale coronal disturbances, which may correspond to what
  we have generally known as "EIT waves." Their nature is still
  actively debated. In certain cases, the fronts of the disturbances
  may signify CME-related shock waves that are important for particle
  acceleration. Using the unprecedented temporal resolution and broad
  temperature coverage of the AIA, we have studied more than 100 such
  events. Here we discuss their kinematics characterized by faster fronts
  than EIT waves in Solar Cycle 23, and spatial relations with CMEs
  using STEREO data that provide triangulation of the fronts. We also
  try plasma diagnostic using images in different filters. Association
  of these disturbances with other phenomena such as CMEs, flares and
  type II bursts, is discussed on a statistical basis.

---------------------------------------------------------
Title: Period doubling in magnetospheric convection cycle
Authors: Liu, W. William
2012JGRA..117.4206L    Altcode: 2012JGRA..11704206L
  A gedanken investigation is performed on magnetospheric complexity. In
  an attempt to separate complexities due to external (solar wind) and
  internal (magnetospheric) dynamics, we hold the solar wind condition
  constant and investigate how the open flux in the magnetosphere
  changes from one convection cycle to the next. The change of open
  flux is related to the time integral of the tail electric field. This
  field, in turn, is proportional to the product of the normal (x)
  and tangential (z) components of the tail magnetic field. As the
  magnetosphere evolves, the magnetic components typically vary
  in opposite directions. We show that this competition leads to a
  magnetic flux cycle described by the classical logistic equation
  x<SUB>n+1</SUB> = r(1 - x<SUB>n</SUB>)x<SUB>n</SUB>, where x is a
  linear function of open flux, the much researched route to chaos through
  period-doubling. The result could provide a possible explanation of the
  steady magnetospheric convection, sawtooth events, and other observed
  manifestations of nonlinearity.

---------------------------------------------------------
Title: Explanatory Supplement to the WISE All-Sky Data Release
    Products
Authors: Cutri, R. M.; Wright, E. L.; Conrow, T.; Bauer, J.; Benford,
   D.; Brandenburg, H.; Dailey, J.; Eisenhardt, P. R. M.; Evans, T.;
   Fajardo-Acosta, S.; Fowler, J.; Gelino, C.; Grillmair, C.; Harbut,
   M.; Hoffman, D.; Jarrett, T.; Kirkpatrick, J. D.; Leisawitz, D.;
   Liu, W.; Mainzer, A.; Marsh, K.; Masci, F.; McCallon, H.; Padgett,
   D.; Ressler, M. E.; Royer, D.; Skrutskie, M. F.; Stanford, S. A.;
   Wyatt, P. L.; Tholen, D.; Tsai, C. W.; Wachter, S.; Wheelock, S. L.;
   Yan, L.; Alles, R.; Beck, R.; Grav, T.; Masiero, J.; McCollum, B.;
   McGehee, P.; Papin, M.; Wittman, M.
2012wise.rept....1C    Altcode:
  The Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010)
  surveyed the entire sky at 3.4, 4.6, 12 and 22 microns in 2010,
  achieving 5-sigma point source sensitivities per band better than
  0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic. The
  WISE All-Sky Data Release, conducted on March 14, 2012, incorporates
  all data taken during the full cryogenic mission phase, 7 January 2010
  to 6 August 2010, that were processed with improved calibrations and
  reduction algorithms. Release data products include: (1) an Atlas
  of 18,240 match-filtered, calibrated and coadded image sets; (2)
  a Source Catalog containing positions and four-band photometry for
  over 563 million objects, and (3) an Explanatory Supplement. Ancillary
  products include a Reject Table that contains 284 million detections
  that were not selected for the Source Catalog because they are low
  signal-to-noise ratio or spurious detections of image artifacts, an
  archive of over 1.5 million sets of calibrated WISE Single-exposure
  images, and a database of 9.4 billion source extractions from those
  single-images, and moving object tracklets identified by the NEOWISE
  program (Mainzer et al. 2011). The WISE All-Sky Data Release products
  supersede those from the WISE Preliminary Data Release (Cutri et
  al. 2011). <P />The Explanatory Supplement to the WISE All-Sky Data
  Release Products is a general guide for users of the WISE data. The
  Supplement contains an overview of the WISE mission, facilities, and
  operations, a detailed description of WISE data processing algorithms,
  a guide to the content and formats of the image and tabular data
  products, and cautionary notes that describe known limitations of the
  All-Sky Release products. Instructions for accessing the WISE data
  products via the services of the NASA/IPAC Infrared Science Archive
  are provided. The Supplement also provides analyses of the achieved sky
  coverage, photometric and astrometric characteristics and completeness
  and reliability of the All-Sky Release data products. <P />The WISE
  All-Sky Release Explanatory Supplement is an on-line document that is
  updated frequently to provide the most current information for users of
  the WISE data products. The Explanatory Supplement is maintained at: <P
  />http://wise2.ipac.caltech.edu/docs/release/allsky/expsup/index.html <P
  />WISE is a joint project of the University of California, Los Angeles
  and the Jet Propulsion Laboratory/California Institute of Technology,
  funded by the National Aeronautics and Space Administration. NEOWISE
  is a project of the Jet Propulsion Laboratory/California Institute of
  Technology, funded by the Planetary Science Division of the National
  Aeronautics and Space Administration.

---------------------------------------------------------
Title: The Hydromagnetic Nature of Quiescent Prominences
Authors: Low, B. C.; Berger, T.; Casini, R.; Liu, W.
2012decs.confE..84L    Altcode:
  High-resolution observations of quiescent prominences with Hinode
  and SDO have revealed within their interiors the ever-¬present
  descent at less than free-fall speeds of cool, vertical dense
  filaments interspersed among upward, narrow streams at comparable
  speeds of heated, low-density plasma. We address the physical nature
  of this dynamical state. Despite the high magnetic Reynolds numbers
  characterizing this hydromagnetic environment, magnetic reconnection
  takes place via spontaneous formation and dissipation of current sheets
  by the coupled effects of highly-anisotropic thermal conduction,
  gravity, optically-thin radiation, heating, and high electrical
  conductivity. In this interesting new version of the theory of Parker
  (1994, Spontaneous current sheets in magnetic fields, Cambridge U
  Press), pervasive reconnections produce a perennial local descent of
  dense condensations under gravity along newly reconnected magnetic field
  lines and a concurrent turbulent rise of buoyant pockets of heated
  magnetized plasma through the large-scale magnetic structure. This
  mechanism may explain the massive downward drainage through a quiescent
  prominence observed recently (Liu et al. 2012 ApJ 745, L21) and, in
  the broader context, relate the quiescent prominence to the surrounding
  chromosphere/corona as a novel, large-scale, magneto-thermal convective
  phenomenon (Berger et al. 2011, Nature 472, 197).

---------------------------------------------------------
Title: SDO/AIA Observations of Sustained Coronal Condensation and Mass
    Drainage in Prominences as Return Flows of the Chromosphere-Corona
    Mass Cycle
Authors: Liu, Wei; Berger, Thomas; Low, B. C.
2012decs.confE..90L    Altcode:
  It has recently been proposed that prominences are manifestations
  of a magneto-thermal convection process that involves ever-present
  dynamic descents of cool material threads and upflows of hot bubbles
  (Berger et al. 2011 Nature). On global scales, prominences may play
  an important role as the return flows of the chromosphere-corona mass
  cycle, in which hot mass is originally transported upward through
  spicules. A critical step in this cycle is the condensation of
  million-degree coronal plasma into T&lt;10,000 K prominence material
  by radiative cooling instability. However, direct observation of
  coronal condensation has been difficult in the past, a situation
  recently changed with the launch of the Hinode/SOT and SDO/AIA. We
  present here the first example observed with SDO/AIA, in which hours of
  gradual cooling through multiple EUV channels (from 2 MK to 80,000 K)
  in large-scale loops leads to eventual condensation at magnetic dips,
  forming a moderate-size prominence of 10^14 gram. The prominence
  mass is not static but maintained by a continual supply through
  condensation at a high rate of 10^10 gram/s against a comparable
  drainage through numerous vertical threads at less than free-fall
  speeds. Most of the total condensation of 10^15 gram, comparable
  to a CME mass and an order of magnitude more than the instantaneous
  mass of the prominence itself, is drained in merely one day. These
  new observations show that a macroscopically quiescent prominence
  is microscopically dynamic, involving the passage of a significant
  mass that bears important implications for the chromosphere-corona
  mass cycle. This interpretation is further supported by the recent
  theoretical development on spontaneous formation of current sheets
  and cool condensations (Low, Berger, Casini, &amp; Liu, this meeting).

---------------------------------------------------------
Title: Modeling waves, flows, and instabilities produced by impulsive
    events in coronal active regions
Authors: Ofman, L.; Liu, W.; Wang, T. J.; Davila, J. M.; Thompson,
   B. J.
2012decs.confE..73O    Altcode:
  Recent high-resolution observations by SDO/AIA combined with spectral
  data from Hinode provide insights into the properties of MHD waves,
  flows, and instabilities in coronal active region plasma and
  their connection with impulsive energy release. Shear flow driven
  instabilities, such as the Kelvin-Helmholtz (KH) instability were
  only recently detected in detail in the corona. I will present recent
  results of 3D MHD models of slow and fast magnetosonic waves in active
  regions excited by jets and quasi-periodic flows driven by micro-flares
  at loops' footpoints. I will discuss models of super-fast magnetosonic
  waves detected recently by SDO/AIA. I will also discuss models of global
  (EIT) waves, and KH instabilities driven by CMEs. The relations between
  waves, flows, instabilities, and impulsive events such as flares and
  CMEs are becoming apparent thanks to the combination of observational
  data analysis and the 3D MHD modeling. Understanding these relations
  is useful for coronal seismology and for tracing the flow of energy
  from the transition region to the corona.

---------------------------------------------------------
Title: Herschel Observations of Debris Disks from WISE
Authors: Padgett, D. L.; Stapelfeldt, K. R.; Liu, W.; Leisawitz,
   D. T.; Fajardo-Acosta, S.
2012faph.confE..44P    Altcode:
  The Wide Field Infrared Survey Explorer (WISE) has just completed a
  sensitive all-sky survey in photometric bands at 3.4, 4.6, 12, and 22
  microns. We report on a study of main sequence Hipparcos and Tycho
  catalog stars within 120 pc with WISE 22 micron emission in excess
  of photospheric levels. This warm excess emission traces material in
  the circumstellar region likely to host terrestrial planets and is
  preferentially found in young systems with ages &lt; 1 Gyr. Nearly a
  hundred of the WISE new warm debris disk candidates detected among FGK
  stars are being observed by Herschel/PACS to characterize circumstellar
  dust. Preliminary results indicate 70 micron detection rates in excess
  of 80% for these targets, suggesting that most of these systems have
  both warm and cool dust in analogy to our asteroid and Kuiper belts. In
  this contribution, we will discuss the WISE debris disk survey and
  latest results from Herschel observations of these sources.

---------------------------------------------------------
Title: SDO/AIA Observations of Various Coronal EUV Waves Associated
    with Flares/CMEs and Their Coronal Seismology Implications
Authors: Liu, Wei; Ofman, Leon; Aschwanden, Markus J.; Nitta, Nariaki;
   Zhao, Junwei; Title, Alan M.
2012decs.confE..87L    Altcode:
  MHD waves can be used as diagnostic tools of coronal seismology to
  decipher otherwise elusive critical physical parameters of the solar
  corona, such as the magnetic field strength and plasma density. They
  are analogous to acoustic waves used in helioseismology, but with
  complexities arising from the magnetic field and nonlinearity. Recent
  high cadence, high resolution, full-disk imaging observations from
  SDO/AIA have opened a new chapter in understanding these waves. Various
  types of EUV waves associated with flares/CMEs have been discovered
  or observed in unprecedented detail. In this presentation, we will
  review such new AIA observations, focusing on the following topics and
  their interrelationships: (1) quasi-periodic fast waves traveling along
  coronal funnels within CME bubbles at speeds up to 2000 km/s, associated
  with flare pulsations at similar frequencies; (2) quasi-periodic wave
  trains within broad, diffuse pulses of global EUV waves (so-called
  EIT waves) running ahead of CME fronts; (3) interactions of global EUV
  waves with local coronal structures on their paths, such as flux-rope
  coronal cavities and their embedded filaments (kink oscillations)
  and coronal holes/active regions (deflections). We will discuss the
  implications of these observations on coronal seismology, on their roles
  in transporting energy through different parts of the solar atmosphere,
  and on understanding their associated eruptive flares/CMEs.

---------------------------------------------------------
Title: SDO/AIA Observations of Secondary Waves Generated by
    Interaction of the 2011 June 7 Global EUV Wave with Solar Coronal
    Structures
Authors: Li, Ting; Zhang, Jun; Yang, Shuhong; Liu, Wei
2012ApJ...746...13L    Altcode: 2011arXiv1111.5202L
  We present Solar Dynamics Observatory/Atmospheric Imaging Assembly
  observations of the interaction of a global EUV wave on 2011 June
  7 with active regions (ARs), coronal holes (CHs), and coronal bright
  structures. The primary global wave has a three-dimensional dome shape,
  with propagation speeds ranging from 430 to 780 km s<SUP>-1</SUP> in
  different directions. The primary coronal wave runs in front of the
  expanding loops involved in the coronal mass ejection (CME) and its
  propagation speeds are approximately constant within 10-20 minutes. Upon
  arrival at an AR on its path, the primary EUV wave apparently disappears
  and a secondary wave rapidly reemerges within 75 Mm of the AR boundary
  at a similar speed. When the EUV wave encounters a coronal bright
  structure, an additional wave front appears there and propagates in
  front of it at a velocity nearly a factor of two faster. Reflected
  waves from a polar CH and a coronal bright structure are observed and
  propagate fractionally slower than the primary waves. Some of these
  phenomena can be equally explained by either a wave or a non-wave
  model alone. However, taken together, these observations provide new
  evidence for the multitudes of global EUV waves, in which a true MHD
  fast-mode wave or shock propagates in front of an expanding CME bubble.

---------------------------------------------------------
Title: First SDO/AIA Observation of Solar Prominence Formation
Following an Eruption: Magnetic Dips and Sustained Condensation
    and Drainage
Authors: Liu, Wei; Berger, Thomas E.; Low, B. C.
2012ApJ...745L..21L    Altcode:
  Imaging solar coronal condensation forming prominences was difficult
  in the past, a situation recently changed by Hinode and the Solar
  Dynamics Observatory (SDO). We present the first example observed with
  the SDO/Atmospheric Imaging Assembly, in which material gradually cools
  through multiple EUV channels in a transequatorial loop system that
  confines an earlier eruption. Nine hours later, this leads to eventual
  condensation at the dips of these loops, forming a moderate-size
  prominence of ~10<SUP>14</SUP> g, to be compared to the characteristic
  10<SUP>15</SUP> g mass of a coronal mass ejection (CME). The prominence
  mass is not static but maintained by condensation at a high estimated
  rate of 10<SUP>10</SUP> g s<SUP>-1</SUP> against a comparable, sustained
  drainage through numerous vertical downflow threads, such that 96% of
  the total condensation (~10<SUP>15</SUP> g) is drained in approximately
  one day. The mass condensation and drainage rates temporally correlate
  with the total prominence mass. The downflow velocity has a narrow
  Gaussian distribution with a mean of 30 km s<SUP>-1</SUP>, while the
  downward acceleration distribution has an exponential drop with a
  mean of ~1/6 g <SUB>⊙</SUB>, indicating a significant canceling of
  gravity, possibly by the Lorentz force. Our observations show that
  a macroscopically quiescent prominence is microscopically dynamic,
  involving the passage of a significant mass through it, maintained
  by a continual mass supply against a comparable mass drainage, which
  bears important implications for CME initiation mechanisms in which
  mass unloading is important.

---------------------------------------------------------
Title: New determination of the astrophysical <SUP>13</SUP>C(
    p, γ) <SUP>14</SUP>N S(E) factors and reaction rates via the
    <SUP>13</SUP>C(<SUP>7</SUP>Li, <SUP>6</SUP>He) <SUP>14</SUP>N reaction
Authors: Li, Y. J.; Li, Z. H.; Li, E. T.; Bai, X. X.; Su, J.; Guo,
   B.; Wang, B. X.; Yan, S. Q.; Zeng, S.; Li, Z. C.; Liu, J. C.; Liu,
   X.; Jin, S. J.; Wang, Y. B.; Zhang, L. Y.; Yu, X. Q.; Li, L.; Lian,
   G.; Fan, Q. W.; Liu, W. P.
2012EPJA...48...13L    Altcode:
  The <SUP>13</SUP>C(<SUP>7</SUP>Li, <SUP>6</SUP>He) <SUP>14</SUP>
  N<SUB>0,1</SUB> reactions were measured at E (<SUP>7</SUP>Li) = 34 MeV
  with the Q3D magnetic spectrometer of the HI-13 tandem accelerator, and
  the first peaks of the angular distributions were obtained for the first
  time. The <SUP>14</SUP>N<SUB>0,1</SUB> proton spectroscopic factors were
  extracted to be 0.67±0.09 and 0.73±0.10 , respectively. Using the
  <SUP>13</SUP>C( p, γ) <SUP>14</SUP>N direct capture S <SUB>dc</SUB>(
  E) factors derived by the spectroscopic factors, the direct measurement
  data for both 1<SUP>-</SUP> and 0<SUP>-</SUP> resonances were well
  fitted via updating the resonance parameters, and then the total
  astrophysical <SUP>13</SUP>C( p, γ) <SUP>14</SUP>N S( E) factors
  and reaction rates were determined at stellar energies. The present
  work offers an independent examination to the existing results of the
  <SUP>13</SUP> C( p, γ) <SUP>14</SUP>N reaction.

---------------------------------------------------------
Title: Measurement of reaction, decay of astrophysical interest and
    progress of RI beam facilities
Authors: Liu, W.; BRIF Collaboration; Nuclear Astrophysics
   Collaboration
2012nuco.confE.170L    Altcode: 2012PoS...146E.170L
  No abstract at ADS

---------------------------------------------------------
Title: Kinematics and amplitude evolution of global coronal extreme
    ultraviolet waves
Authors: Li, Ting; Zhang, Jun; Yang, Shu-Hong; Liu, Wei
2012RAA....12..104L    Altcode:
  With the observations of the Solar-Terrestrial Relations Observatory
  (STEREO) and the Solar Dynamics Observatory (SDO), we analyze in
  detail the kinematics of global coronal waves together with their
  intensity amplitudes (so-called “perturbation profiles"). We use
  a semi-automatic method to investigate the perturbation profiles of
  coronal waves. The location and amplitude of the coronal waves are
  calculated over a 30° sector on the sphere, where the wave signal is
  strongest. The position with the strongest perturbation at each time
  is considered as the location of the wave front. In all four events,
  the wave velocities vary with time for most of their lifetime, up to 15
  min, while in the event observed by the Atmospheric Imaging Assembly
  there is an additional early phase with a much higher velocity. The
  velocity varies greatly between different waves from 216 to 440 km
  s<SUP>-1</SUP>. The velocity of the two waves initially increases,
  subsequently decreases, and then increases again. Two other waves show a
  deceleration followed by an acceleration. Three categories of amplitude
  evolution of global coronal waves are found for the four events. The
  first is that the amplitude only shows a decrease. The second is
  that the amplitude initially increases and then decreases, and the
  third is that the amplitude shows an orderly increase, a decrease,
  an increase again and then a decrease. All the extreme ultraviolet
  waves show a decrease in amplitude while propagating farther away,
  probably because the driver of the global coronal wave (coronal mass
  ejection) is moving farther away from the solar surface.

---------------------------------------------------------
Title: Study of the primordial Lithium abundance at CIAE
Authors: Li, Z. H.; Li, E. T.; Su, J.; Guo, B.; Liu, W. P.; Li, Y. J.;
   Chen, Y. S.; Hou, S. Q.; Bai, X. X.; Yan, S. Q.; Want, Y. B.; Want,
   B. X.; Zeng, S.; Lian, G.; Liu, X.; Jin, S. J.
2012nuco.confE.209L    Altcode: 2012PoS...146E.209L
  No abstract at ADS

---------------------------------------------------------
Title: New Young Star Candidates in the Taurus-Auriga Region as
    Selected from WISE
Authors: Rebull, Luisa M.; Koenig, X.; Padgett, D.; Terebey, S.;
   McGehee, P.; Hillenbrand, L.; Knapp, G.; Leisawitz, D.; Liu, W.;
   Noriega-Crespo, A.; Ressler, M.; Stapelfeldt, K.; Fajardo-Acosta,
   S.; Mainzer, A.
2012AAS...21942505R    Altcode:
  The Taurus Molecular Cloud subtends a large solid angle on the sky, in
  excess of 250 square degrees. The search for legitimate Taurus members
  to date has been limited by sky coverage as well as the challenge
  of distinguishing members from field interlopers. The Wide-field
  Infrared Survey Explorer (WISE) has recently observed the entire sky,
  and we take advantage of the opportunity to search for young stellar
  object (YSO) candidate Taurus members from a 260 square degree region
  designed to encompass previously-identified Taurus members. We use
  near- and mid-infrared colors to select objects with apparent infrared
  excesses and incorporate other catalogs of ancillary data to present:
  a list of rediscovered Taurus YSOs with infrared excesses (taken to
  be due to circumstellar disks), a list of rejected YSO candidates
  (largely galaxies), and a list of 94 surviving candidate new YSO-like
  Taurus members. There is likely to be contamination lingering in this
  candidate list, and follow-up spectra are warranted.

---------------------------------------------------------
Title: A Risk Assessment Model and Method of Major Aerospace Projects
Authors: Jin, B.; Liu, W.; Chen, F.; Li, F.
2012ESASP.699E..35J    Altcode:
  A "five-claw" model which is based on the idea of risk profile in NASA,
  common risk sources of equipment development in GJB 5852-2006 and
  "nine-new" analysis method in CASC is put forward. The "five-claw"
  risk assessment model uses design &amp; test, manufacturing, basic
  parts &amp; general parts to describe aerospace projects' risk. In
  order to assess the extent of a risk described by this new model,
  a semi-quantitative method is put forward. It could avoid lacking
  objectivity of qualitative method and the difficulty in data-obtaining
  of quantitative method. Although the model and method present in
  this paper may not be fully practical in major aerospace projects,
  it just provides a new idea for risk assessment during the development
  of major aerospace projects

---------------------------------------------------------
Title: Destruction of Sun-Grazing Comet C/2011 N3 (SOHO) Within the
    Low Solar Corona
Authors: Schrijver, C. J.; Brown, J. C.; Battams, K.; Saint-Hilaire,
   P.; Liu, W.; Hudson, H.; Pesnell, W. D.
2012Sci...335..324S    Altcode:
  Observations of comets in Sun-grazing orbits that survive solar
  insolation long enough to penetrate into the Sun's inner corona provide
  information on the solar atmosphere and magnetic field as well as on
  the makeup of the comet. On 6 July 2011, the Solar Dynamics Observatory
  (SDO) observed the demise of comet C/2011 N3 (SOHO) within the low solar
  corona in five wavelength bands in the extreme ultraviolet (EUV). The
  comet penetrated to within 0.146 solar radius (~100,000 kilometers)
  of the solar surface before its EUV signal disappeared. Before that,
  material released into the coma - at first seen in absorption - formed
  a variable EUV-bright tail. During the final 10 minutes of observation
  by SDO's Atmospheric Imaging Assembly, ~6 × 10^8 to 6 × 10^10 grams
  of total mass was lost (corresponding to an effective nucleus diameter
  of ~10 to 50 meters), as estimated from the tail's deceleration due to
  interaction with the surrounding coronal material; the EUV absorption
  by the comet and the brightness of the tail suggest that the mass was
  at the high end of this range. These observations provide evidence
  that the nucleus had broken up into a family of fragments, resulting
  in accelerated sublimation in the Sun's intense radiation field.

---------------------------------------------------------
Title: SDO/AIA Observations of Quasi-periodic Fast (~1000 km/s)
    Propagating (QFP) Waves as Evidence of Fast-mode Magnetosonic Waves
in the Low Corona: Statistics and Implications
Authors: Liu, W.; Ofman, L.; Title, A. M.; Zhao, J.; Aschwanden, M. J.
2011AGUFMSH33A2043L    Altcode:
  Recent EUV imaging observations from SDO/AIA led to the discovery of
  quasi-periodic fast (~2000 km/s) propagating (QFP) waves in active
  regions (Liu et al. 2011). They were interpreted as fast-mode
  magnetosonic waves and reproduced in 3D MHD simulations (Ofman
  et al. 2011). Since then, we have extended our study to a sample
  of more than a dozen such waves observed during the SDO mission
  (2010/04-now). We will present the statistical properties of these waves
  including: (1) Their projected speeds measured in the plane of the sky
  are about 400-2200 km/s, which, as the lower limits of their true speeds
  in 3D space, fall in the expected range of coronal Alfven or fast-mode
  speeds. (2) They usually originate near flare kernels, often in the wake
  of a coronal mass ejection, and propagate in narrow funnels of coronal
  loops that serve as waveguides. (3) These waves are launched repeatedly
  with quasi-periodicities in the 30-200 seconds range, often lasting
  for more than one hour; some frequencies coincide with those of the
  quasi-periodic pulsations (QPPs) in the accompanying flare, suggestive
  a common excitation mechanism. We obtained the k-omega diagrams and
  dispersion relations of these waves using Fourier analysis. We estimate
  their energy fluxes and discuss their contribution to coronal heating
  as well as their diagnostic potential for coronal seismology.

---------------------------------------------------------
Title: The EUV Emission in Comet-Solar Corona Interactions
Authors: Bryans, P.; Pesnell, W. D.; Schrijver, C. J.; Brown, J. C.;
   Battams, K.; Saint-Hilaire, P.; Liu, W.; Hudson, H. S.
2011AGUFMSH34B..05B    Altcode:
  The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory
  (SDO) viewed a comet as it passed through the solar corona on 2011 July
  5. This was the first sighting of a comet by a EUV telescope. For 20
  minutes, enhanced emission in several of the AIA wavelength bands marked
  the path of the comet. We explain this EUV emission by considering
  the evolution of the cometary atmosphere as it interacts with the
  ambient solar atmosphere. Water ice in the comet rapidly sublimates
  as it approaches the Sun. This water vapor is then photodissociated,
  primarily by Ly-α, by the solar radiation field to create atomic H and
  O. Other molecules present in the comet also evaporate and dissociate
  to give atomic Fe and other metals. Subsequent ionization of these
  atoms can be achieved by a number of means, including photoionization,
  electron impact, and charge exchange with coronal protons and other
  highly-charged species. Finally, particles from the cometary atmosphere
  are thermalized to the background temperature of the corona. Each step
  could cause emission in the AIA bandpasses. We will report here on
  their relative contribution to the emission seen in the AIA telescopes.

---------------------------------------------------------
Title: Investigation of ULF waves in space and on the ground
Authors: Sarris, T. E.; Liu, W.; Li, X.; Argyriadis, E.
2011AGUFMSM51B2080S    Altcode:
  In this study we compare features of magnetospheric Ultra-Low
  Frequency waves as they are observed on the ground and in space. In
  particular, the characteristics that we investigate include the waves'
  azimuthal mode number, using spacecraft conjunctions and azimuthally
  aligned magnetometer stations; the wave amplitudes and their spatial
  variations in space and on the ground; their occurence distribution
  in terms of latitudinal and local time extent, as they are seen by
  ground magnetometer chains and by multiple spacecraft in different
  locations in the magnetosphere; and their polarization. We comment
  on the characteristics that are mostly altered by the ionosphere
  and on the implications in using ground measurements in models of
  radial diffusion, which require the above inputs to approximate the
  drift-resonant interraction of high-energy particles with ULF waves.

---------------------------------------------------------
Title: Measurable realistic image-based 3D mapping
Authors: Liu, W.; Wang, J.; Wang, J. J.; Ding, W.; Almagbile, A.
2011ArFKT..22..297L    Altcode:
  Maps with 3D visual models are becoming a remarkable feature of 3D map
  services. High-resolution image data is obtained for the construction
  of 3D visualized models.The3D map not only provides the capabilities
  of 3D measurements and knowledge mining, but also provides the
  virtual experienceof places of interest, such as demonstrated in
  the Google Earth. Applications of 3D maps are expanding into the
  areas of architecture, property management, and urban environment
  monitoring. However, the reconstruction of high quality 3D models is
  time consuming, and requires robust hardware and powerful software to
  handle the enormous amount of data. This is especially for automatic
  implementation of 3D models and the representation of complicated
  surfacesthat still need improvements with in the visualisation
  techniques. The shortcoming of 3D model-based maps is the limitation of
  detailed coverage since a user can only view and measure objects that
  are already modelled in the virtual environment. This paper proposes and
  demonstrates a 3D map concept that is realistic and image-based, that
  enables geometric measurements and geo-location services. Additionally,
  image-based 3D maps provide more detailed information of the real world
  than 3D model-based maps. The image-based 3D maps use geo-referenced
  stereo images or panoramic images. The geometric relationships between
  objects in the images can be resolved from the geometric model of stereo
  images. The panoramic function makes 3D maps more interactive with
  users but also creates an interesting immersive circumstance. Actually,
  unmeasurable image-based 3D maps already exist, such as Google street
  view, but only provide virtual experiences in terms of photos. The
  topographic and terrain attributes, such as shapes and heights though
  are omitted. This paper also discusses the potential for using a low
  cost land Mobile Mapping System (MMS) to implement realistic image
  3D mapping, and evaluates the positioning accuracy that a measureable
  realistic image-based (MRI) system can produce. The major contribution
  here is the implementation of measurable images on 3D maps to obtain
  various measurements from real scenes.

---------------------------------------------------------
Title: Investigation on a dayside poloidal ULF wave event on 29
    May 2007
Authors: Liu, W.; Sarris, T. E.; Li, X.; Zong, Q.; Ergun, R. E.;
   Angelopoulos, V.; Glassmeier, K.
2011AGUFMSM13B2070L    Altcode:
  We investigate a strong poloidal ultralow frequency wave event in
  the noon sector observed by THEMIS and LANL satellites on 29 May
  2007. From 07:00 to 10:00 UT, five THEMIS satellites that were lined up
  in similar outbound orbits consecutively observed narrow-band poloidal
  pulsations from 10 to 4 mHz. The wave activity covered a broad region
  from 09:00 to 13:30 LT azimuthally and 5 to 9.5 RE radially with an
  azimuthal mode number around 8. The radial extent and power of the wave
  decreased with time from 07:00 to 08:30 UT, suggesting a decay process
  with a time scale of hours. In the region outside the plasmapause,
  the wave power was observed to decrease then increase from 08:00 to
  09:00 UT with a rapid temporal variation. The decrease in wave power,
  which suggests fast decay (within one hour), might be related to the
  evolution of the plasmasphere. The increase could be related to the
  regeneration by the surface wave at the plasmapause. We suggest that
  a coupling between the surface wave and the resonance of the field
  line around the plasmapause takes place when the density inside the
  plasmapause is twice of the density outside the plasmapause.

---------------------------------------------------------
Title: Large-scale Coronal Propagating Fronts During the Rising
    Phase of Solar Cycle 24
Authors: Nitta, N. V.; Liu, W.; Schrijver, C. J.; Title, A. M.; Lemen,
   J. R.
2011AGUFMSH23A1941N    Altcode:
  With increasing solar activity, the AIA on SDO has observed a number
  of large-scale coronal propagating fronts, which are often called
  "EIT waves." Although their nature is still actively debated,
  these propagating fronts usually accompany CMEs, and, in certain
  cases, may signify CME-related shock waves important for particle
  acceleration. Using the unprecedented temporal resolution and broad
  temperature coverage of the AIA, it is possible to characterize
  the propagating fronts in the corona far better than before, as
  demonstrated in the literature for a yet small number of cases. We
  study the properties of more than 40 propagating fronts as observed
  by AIA, and discuss the key properties for them to be associated with
  other phenomena such as type II radio bursts, flares, CMEs, ICMEs,
  and SEP events. We make use of data, both remote-sensing and in-situ,
  from STEREO which provides two additional vantage points, to make the
  associations more solid. For the associated phenomena, their basic
  properties are correlated with those of the propagating fronts. We
  also revisit the association of EIT waves with other phenomena during
  the similar phase of Solar Cycle 23 and discuss possible differences
  in terms of global magnetic field. Understanding their relation with
  other phenomena, we can have a more complete picture of the coronal
  propagating fronts in the context of CME acceleration and deceleration.

---------------------------------------------------------
Title: Quantifying Radial Diffusion of Radiation Belt Electrons Based
    on Global MHD Simulation Validated by GOES and THEMIS Measurements
Authors: Tu, W.; Elkington, S. R.; Li, X.; Liu, W.
2011AGUFMSM21C..08T    Altcode:
  Radial diffusion is one of the most important acceleration mechanisms
  for radiation belt electrons, which is due to the drift-resonant
  interactions with large-scale fluctuations of the magnetosphere's
  magnetic and electric fields (Pc4 and Pc5 ranges of ULF waves). A key
  step in radial diffusion simulations is to quantify the radial diffusion
  coefficient, which is related to the power spectral density and global
  mode structure of the ULF waves. However, difficulties in determining
  the global properties of ULF waves have guided researchers towards
  specifying empirical forms of the diffusion coefficient, introducing
  additional uncertainties in the radiation belt studies. In order to
  quantify the radial diffusion, we run the global MHD simulations
  to obtain the mode structure and power spectrum of the ULF waves
  and validate the simulation results with available satellite
  measurements, such as GOES and THEMIS measurements. The calculated
  diffusion coefficient is shown to be dominated by the contribution
  from magnetic field perturbations, and much less from the electric
  field perturbations. Fast diffusion is found to generally occur when
  solar wind dynamic pressure is high or nightside geomagnetic activity
  is strong and with faster diffusion at higher L regions.

---------------------------------------------------------
Title: VizieR Online Data Catalog: New young star candidates in
    Taurus-Auriga (Rebull+, 2011)
Authors: Rebull, L. M.; Koenig, X. P.; Padgett, D. L.; Terebey, S.;
   McGehee, P. M.; Hillenbrand, L. A.; Knapp, G. R.; Leisawitz, D.;
   Liu, W.; Noriega-Crespo, A.; Ressler, M. E.; Stapelfeldt, K. R.;
   Fajardo-Acosta, S.; Mainzer, A.
2011yCat..21960004R    Altcode:
  In the context of Rebull et al. (2010ApJS..186..259R), we assembled
  a substantial multi-wavelength database, spanning Sloan u through
  Spitzer/MIPS 160um (with some X-rays) for point sources throughout
  the Taurus region. We use that catalog as the core for our analysis
  here, updating it with confirmed Taurus members from, e.g., Kenyon
  et al. (2008hsf1.book..405K) and Luhman et al. (2010ApJS..186..111L)
  outside of our original Spitzer map. We have also searched SIMBAD (and
  literature references therein) for known galaxies and other contaminants
  in this vicinity. Our Taurus Spitzer Survey spanned ~44deg<SUP>2</SUP>
  (figure 1). WISE data acquisition and reduction are discussed in Wright
  et al. (2010AJ....140.1868W), Jarrett et al. (2011, ApJ, submitted),
  and in the Explanatory Supplement to the WISE Preliminary Data Release
  Products. There are four WISE bands, with central wavelengths at 3.4,
  4.6, 12, and 22um, and a spatial resolution of 6" (12" at 22um). <P
  />(3 data files).

---------------------------------------------------------
Title: Modeling Super-fast Magnetosonic Waves Observed by SDO in
    Active Region Funnels
Authors: Ofman, L.; Liu, W.; Title, A.; Aschwanden, M.
2011ApJ...740L..33O    Altcode:
  Recently, quasi-periodic, rapidly propagating waves have been observed
  in extreme ultraviolet by the Solar Dynamics Observatory/Atmospheric
  Imaging Assembly (AIA) instrument in about 10 flare/coronal mass
  ejection (CME) events thus far. A typical example is the 2010 August 1
  C3.2 flare/CME event that exhibited arc-shaped wave trains propagating
  in an active region (AR) magnetic funnel with ~5% intensity variations
  at speeds in the range of 1000-2000 km s<SUP>-1</SUP>. The fast
  temporal cadence and high sensitivity of AIA enabled the detection
  of these waves. We identify them as fast magnetosonic waves driven
  quasi-periodically at the base of the flaring region and develop
  a three-dimensional MHD model of the event. For the initial state
  we utilize the dipole magnetic field to model the AR and include
  gravitationally stratified density at coronal temperature. At the
  coronal base of the AR, we excite the fast magnetosonic wave by
  periodic velocity pulsations in the photospheric plane confined to a
  funnel of magnetic field lines. The excited fast magnetosonic waves
  have similar amplitude, wavelength, and propagation speeds as the
  observed wave trains. Based on the simulation results, we discuss the
  possible excitation mechanism of the waves, their dynamical properties,
  and the use of the observations for coronal MHD seismology.

---------------------------------------------------------
Title: Spatial structure and temporal evolution of a dayside poloidal
    ULF wave event
Authors: Liu, W.; Sarris, T. E.; Li, X.; Zong, Q. -G.; Ergun, R.;
   Angelopoulos, V.; Glassmeier, K. H.
2011GeoRL..3819104L    Altcode:
  We investigate a strong poloidal ultralow frequency wave event in
  the noon sector observed by THEMIS and LANL satellites on 29 May
  2007. From 07:00 to 10:00 UT, the five THEMIS satellites that were
  lined up in similar outbound orbits consecutively observed narrow-band
  poloidal pulsations from 10 to 4 mHz. The wave activity covered a broad
  region from 09:00 to 13:30 LT azimuthally and 5 to 9.5 R<SUB>E</SUB>
  radially. The radial extent and power of the wave decreased with
  time from 07:00 to 08:30 UT, suggesting a decay process with a time
  scale of hours. In the region outside the plasmapause, the wave power
  was observed to decrease then increase from 08:00 to 09:00 UT with a
  rapid temporal variation. The decrease in wave power, which suggests
  fast decay (within one hour), might be related to the evolution of
  the plasmasphere. The subsequent increase could possibly be related
  to a regeneration process by a surface wave at the plasmapause. We
  suggest that a coupling between the surface wave and the resonance
  of the field line around the plasmapause takes place when the density
  inside the plasmapause is twice the density outside the plasmapause.

---------------------------------------------------------
Title: Coronal Seismology in the SDO Era: AIA Observations of Various
    Coronal Waves Associated with CMEs/Flares
Authors: Liu, Wei; Ofman, Leon; Aschwanden, Markus J.; Nitta, Nariaki;
   Zhao, Junwei; Title, Alan M.
2011sdmi.confE..49L    Altcode:
  MHD waves, as critical diagnostic tools of coronal seismology, can be
  used to decipher otherwise elusive physical parameters of the solar
  corona, such as the magnetic field strength and plasma density. They
  are analogous to acoustic waves used in helioseismology. Recent high
  cadence, high resolution, full-disk imaging observations from SDO/AIA
  have opened a new chapter in understanding these waves. Various types
  of waves associated with flares and/or CMEs have been discovered. In
  this presentation, we will review such new AIA observations, focusing
  on the following topics: (1) fine structures in CME-related global EUV
  waves (so-called EIT waves), including a diffuse pulse superimposed
  with multiple sharp fronts or "ripples" (Liu et al. 2010, ApJL); (2)
  quasi-periodic fast waves traveling in coronal funnels at speeds up to
  2000 km/s and associated with flares pulsating at similar frequencies
  (Liu et al. 2011, ApJL); (3) interaction of global EUV waves with local
  coronal structures on their paths, such as flux-rope coronal cavities
  (triggered kink oscillations, Liu et al. in preparation) and coronal
  holes/active regions (deflection). We will discuss the implications
  of these observations on coronal seismology and on understanding their
  associated flares and CMEs. We also anticipate to exchange ideas with
  helioseismologists at this workshop, in a hope to bring together coronal
  seismology and helioseismology techniques to advance our understanding
  of solar oscillations from the interior to the upper atmosphere.

---------------------------------------------------------
Title: Analysis of Land Water Storage in Southwest China Based on
    GRACE Data
Authors: Liu, Wei; Miao, Yuan-Xing
2011ChA&A..35..421L    Altcode:
  The inversion of the variation in the land water storage in Southwest
  China is carried out by taking advantage of the data obtained by the
  earth gravity satellite GRACE (Gravity Recovery and Climate Experiment)
  for 64 months from January 2005 to April 2010. The result shows that
  by selecting an appropriate Gauss radius ( R = 600 km) and taking the
  average gravitational field of the adopted data as the back-ground
  gravitational field, the land water storage in Southwest China inverted
  on the basis of the GRACE data reflects the drought in Southwest China
  at the beginning of 2010 very well.

---------------------------------------------------------
Title: Improving the <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl Reaction
    Rate for Models of Classical Nova Explosions
Authors: Parikh, A.; Faestermann, Th.; Krücken, R.; Bildstein, V.;
   Bishop, S.; Eppinger, K.; Herlitzius, C.; Lepyoshkina, O.; Maierbeck,
   P.; Seiler, D.; Wimmer, K.; Hertenberger, R.; Wirth, H. -F.; Fallis,
   J.; Hager, U.; Hutcheon, D.; Ruiz, Ch.; Buchmann, L.; Ottewell, D.;
   Freeman, B.; Wrede, Ch.; García, A.; Delbridge, B.; Knecht, A.;
   Sallaska, A.; Chen, A. A.; Clark, J. A.; Deibel, C. M.; Fulton, B.;
   Laird, A.; Greife, U.; Guo, B.; Li, E.; Li, Z.; Lian, G.; Wang, Y.;
   Liu, W.; Parker, P. D.; Setoodehnia, K.
2011AIPC.1377..188P    Altcode:
  Reduced uncertainty in the thermonuclear rate of the
  <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl reaction would help to improve
  our understanding of nucleosynthesis in classical nova explosions. At
  present, models are generally in concordance with observations that
  nuclei up to roughly the calcium region may be produced in these
  explosive phenomena; better knowledge of this rate would help with
  the quantitative interpretation of nova observations over the S-Ca
  mass region, and contribute towards the firm establishment of a
  nucleosynthetic endpoint. As well, models find that the ejecta of
  nova explosions on massive oxygen-neon white dwarfs may contain
  as much as 150 times the solar abundance of <SUP>33</SUP>S. This
  characteristic isotopic signature of a nova explosion could possibly
  be observed through the analysis of microscopic grains formed in the
  environment surrounding a nova and later embedded within primitive
  meteorites. An improved <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl rate
  (the principal destruction mechanism for <SUP>33</SUP>S in novae)
  would help to ensure a robust model prediction for the amount of
  <SUP>33</SUP>S that may be produced. Finally, constraining this
  rate could confirm or rule out the decay of an isomeric state of
  <SUP>34</SUP>Cl (Ex = 146 keV, t<SUB>1/2</SUB> = 32 m) as a source
  for observable gamma-rays from novae. We have performed several
  complementary experiments dedicated to improving our knowledge of the
  <SUP>33</SUP>S(p,γ)<SUP>34</SUP>Cl rate, using both indirect methods
  (measurement of the <SUP>34</SUP>S(<SUP>3</SUP>He,t)<SUP>34</SUP>Cl
  and <SUP>33</SUP>S(<SUP>3</SUP>He,d)<SUP>34</SUP>Cl reactions with the
  Munich Q3D spectrograph) and direct methods (in normal kinematics at
  CENPA, University of Washington, and in inverse kinematics with the
  DRAGON recoil mass separator at TRIUMF). Our results will be used
  with nova models to facilitate comparisons of model predictions with
  present and future nova observables.

---------------------------------------------------------
Title: On the progenitors of millisecond pulsars by the recycling
    evolutionary channel
Authors: Liu, Wei-Min; Chen, Wen-Cong
2011MNRAS.416.2285L    Altcode: 2011arXiv1106.1567L; 2011MNRAS.tmp.1198L
  The recycling model suggested that low-mass X-ray binaries (LMXBs)
  could evolve into binary millisecond pulsars (BMSPs). In this work,
  we attempt to investigate the progenitor properties of BMSPs formed by
  the recycling evolutionary channel, and if submillisecond pulsars can
  be produced by this channel. Using Eggleton's stellar evolution code,
  considering that the dead pulsars can be spun up to a short spin period
  by the accreting material and angular momentum from the donor star,
  we have calculated the evolution of close binaries consisting of a
  neutron star (NS) and a low-mass main-sequence donor star, and the
  spin evolution of NSs. In the calculation, some physical processes,
  such as the thermal and viscous instability of an accretion disc,
  propeller effect and magnetic braking, are included. Our calculated
  results indicate that all LMXBs with a low-mass donor star of 1.0-2.0
  M<SUB>⊙</SUB> and a short orbital period (≲ 3-4 d) can form
  millisecond pulsars with a spin period less than 10 ms. However, it
  is difficult to produce submillisecond pulsars by this evolutionary
  channel. In addition, our evolutionary scenario cannot account for
  the existence of BMSPs with a long orbital period (P<SUB>orb</SUB>≳
  70-80 d).

---------------------------------------------------------
Title: Implications of X-ray Observations for Electron Acceleration
    and Propagation in Solar Flares
Authors: Holman, G. D.; Aschwanden, M. J.; Aurass, H.; Battaglia, M.;
   Grigis, P. C.; Kontar, E. P.; Liu, W.; Saint-Hilaire, P.; Zharkova,
   V. V.
2011SSRv..159..107H    Altcode: 2011SSRv..tmp..162H; 2011SSRv..tmp..242H; 2011SSRv..tmp..260H;
   2011SSRv..tmp...86H; 2011arXiv1109.6496H
  High-energy X-rays and γ-rays from solar flares were discovered
  just over fifty years ago. Since that time, the standard for
  the interpretation of spatially integrated flare X-ray spectra
  at energies above several tens of keV has been the collisional
  thick-target model. After the launch of the Reuven Ramaty High
  Energy Solar Spectroscopic Imager ( RHESSI) in early 2002, X-ray
  spectra and images have been of sufficient quality to allow a greater
  focus on the energetic electrons responsible for the X-ray emission,
  including their origin and their interactions with the flare plasma
  and magnetic field. The result has been new insights into the flaring
  process, as well as more quantitative models for both electron
  acceleration and propagation, and for the flare environment with
  which the electrons interact. In this article we review our current
  understanding of electron acceleration, energy loss, and propagation
  in flares. Implications of these new results for the collisional
  thick-target model, for general flare models, and for future flare
  studies are discussed.

---------------------------------------------------------
Title: An Observational Overview of Solar Flares
Authors: Fletcher, L.; Dennis, B. R.; Hudson, H. S.; Krucker, S.;
   Phillips, K.; Veronig, A.; Battaglia, M.; Bone, L.; Caspi, A.; Chen,
   Q.; Gallagher, P.; Grigis, P. T.; Ji, H.; Liu, W.; Milligan, R. O.;
   Temmer, M.
2011SSRv..159...19F    Altcode: 2011SSRv..tmp..261F; 2011arXiv1109.5932F
  We present an overview of solar flares and associated phenomena,
  drawing upon a wide range of observational data primarily from the
  RHESSI era. Following an introductory discussion and overview of
  the status of observational capabilities, the article is split into
  topical sections which deal with different areas of flare phenomena
  (footpoints and ribbons, coronal sources, relationship to coronal mass
  ejections) and their interconnections. We also discuss flare soft X-ray
  spectroscopy and the energetics of the process. The emphasis is to
  describe the observations from multiple points of view, while bearing
  in mind the models that link them to each other and to theory. The
  present theoretical and observational understanding of solar flares is
  far from complete, so we conclude with a brief discussion of models,
  and a list of missing but important observations.

---------------------------------------------------------
Title: Current progress of nuclear astrophysical reaction and decay
    study at CIAE
Authors: Liu, W. P.; Li, Z. H.; Guo, B.; Wang, Y. B.; Su, J.; Bai,
   X. X.; Lian, G.; Wang, B. X.; Yan, S. Q.; Zeng, S.; Li, Y. J.; Li,
   E. T.; Jin, S. J.; Liu, X.
2011JPhCS.312d2013L    Altcode:
  Presented here was current progress of the study of nuclear
  astrophysical reaction and decay at CIAE. We studied astrophysical
  <SUP>12</SUP>N(p,γ)<SUP>13</SUP>O reaction through the measurement
  of the <SUP>12</SUP>N(d,n)<SUP>13</SUP>O angular distribution
  in inverse kinematics. Our result is in agreement with that from
  the <SUP>14</SUP>N(<SUP>12</SUP>N,<SUP>13</SUP>O)<SUP>13</SUP>C
  reaction and two shell model calculations. We also measured
  the angular distributions of single neutron transfer reaction of
  <SUP>7</SUP>Li(<SUP>6</SUP>Li,<SUP>7</SUP>Li)<SUP>6</SUP>Li, and derived
  the reaction cross section for <SUP>6</SUP>Li(n,γ)<SUP>7</SUP>Li by
  using the present spectroscopic factor. The astrophysical reaction
  rate is found to be higher by a factor of 1.7 than the value adopted
  in previous reaction network calculations. In addition, half-life of
  <SUP>147</SUP>Sm in metal samarium and Sm<SUB>2</SUB>O<SUB>3</SUB>
  was measured. No significant change has been observed within the
  experimental uncertainty.

---------------------------------------------------------
Title: New Young Star Candidates in the Taurus-Auriga Region as
    Selected from the Wide-Field Infrared Survey Explorer
Authors: Rebull, L. M.; Koenig, X. P.; Padgett, D. L.; Terebey, S.;
   McGehee, P. M.; Hillenbrand, L. A.; Knapp, G. R.; Leisawitz, D.;
   Liu, W.; Noriega-Crespo, A.; Ressler, M. E.; Stapelfeldt, K. R.;
   Fajardo-Acosta, S.; Mainzer, A.
2011ApJS..196....4R    Altcode: 2011arXiv1106.5080R
  The Taurus Molecular Cloud subtends a large solid angle on the sky, in
  excess of 250 deg<SUP>2</SUP>. The search for legitimate Taurus members
  to date has been limited by sky coverage as well as the challenge
  of distinguishing members from field interlopers. The Wide-field
  Infrared Survey Explorer has recently observed the entire sky, and we
  take advantage of the opportunity to search for young stellar object
  (YSO) candidate Taurus members from a ~260 deg<SUP>2</SUP> region
  designed to encompass previously identified Taurus members. We use
  near- and mid-infrared colors to select objects with apparent infrared
  excesses and incorporate other catalogs of ancillary data to present
  a list of rediscovered Taurus YSOs with infrared excesses (taken to
  be due to circumstellar disks), a list of rejected YSO candidates
  (largely galaxies), and a list of 94 surviving candidate new YSO-like
  Taurus members. There is likely to be contamination lingering in this
  candidate list, and follow-up spectra are warranted.

---------------------------------------------------------
Title: Direct Imaging of Quasi-periodic Fast Propagating Waves of
    ~2000 km s<SUP>-1</SUP> in the Low Solar Corona by the Solar Dynamics
    Observatory Atmospheric Imaging Assembly
Authors: Liu, Wei; Title, Alan M.; Zhao, Junwei; Ofman, Leon;
   Schrijver, Carolus J.; Aschwanden, Markus J.; De Pontieu, Bart;
   Tarbell, Theodore D.
2011ApJ...736L..13L    Altcode: 2011arXiv1106.3150L
  Quasi-periodic propagating fast mode magnetosonic waves in the solar
  corona were difficult to observe in the past due to relatively low
  instrument cadences. We report here evidence of such waves directly
  imaged in EUV by the new Atmospheric Imaging Assembly instrument
  on board the Solar Dynamics Observatory. In the 2010 August 1 C3.2
  flare/coronal mass ejection event, we find arc-shaped wave trains of
  1%-5% intensity variations (lifetime ~200 s) that emanate near the
  flare kernel and propagate outward up to ~400 Mm along a funnel of
  coronal loops. Sinusoidal fits to a typical wave train indicate a phase
  velocity of 2200 ± 130 km s<SUP>-1</SUP>. Similar waves propagating
  in opposite directions are observed in closed loops between two flare
  ribbons. In the k-ω diagram of the Fourier wave power, we find a
  bright ridge that represents the dispersion relation and can be well
  fitted with a straight line passing through the origin. This k-ω
  ridge shows a broad frequency distribution with power peaks at 5.5,
  14.5, and 25.1 mHz. The strongest signal at 5.5 mHz (period 181 s)
  temporally coincides with quasi-periodic pulsations of the flare,
  suggesting a common origin. The instantaneous wave energy flux
  of (0.1-2.6) × 10<SUP>7</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>
  estimated at the coronal base is comparable to the steady-state heating
  requirement of active region loops.

---------------------------------------------------------
Title: Multi-instrument observations of soft electron precipitation
    and its association with magnetospheric flows
Authors: Liang, Jun; Spanswick, E.; Nicolls, M. J.; Donovan, E. F.;
   Lummerzheim, D.; Liu, W. W.
2011JGRA..116.6201L    Altcode:
  We present a multi-instrument study on the variations of optical
  auroras and ionospheric electron densities during an interval of a
  series of fast earthward flows in the magnetotail on 3 March 2009. The
  flow-related auroral signatures include intermittent higher-latitude
  (&gt;68° magnetic latitude) intensifications manifested in green and
  blue line auroras and more latitudinally extended red line auroral
  intensifications and expansions. During the same interval the Poker
  Flat incoherent scatter radar (PFISR) detected F region ionospheric
  electron density enhancements which, together with the red line
  auroral intensifications, give evidence for soft electron (&lt;1 keV)
  precipitation associated with fast magnetospheric flow activity. We
  demonstrated the southward motion of ionospheric electron density
  patches in correspondence to individual earthward flow bursts and
  auroral activations. By virtue of the multibeam technique of PFISR we
  construct the altitudinal profile of the density patches and estimate
  that the characteristic energies of the precipitating electrons were
  on order of a few hundred eV, comparable to the observed electron
  temperature in the near-Earth central plasma sheet (CPS). We propose
  that the fast flows give rise to enhanced ELF wave activity, which
  causes strong pitch angle diffusion of the soft electron population
  in the CPS via wave-particle interactions. The precipitation may be
  further aided with a moderate field-aligned potential drop comparable
  to or smaller than the CPS electron temperature. When the flows
  penetrate into the inner plasma sheet, the adiabatic drift motion of
  soft electrons may lead to a decreasing trend of electron energy with
  decreasing radial distance, which is manifested in PFISR observations
  as an ascending trend of the altitude range of the density patches
  toward the equatorward auroral border.

---------------------------------------------------------
Title: SDO/AIA Observations of a Global EUV Disturbance Traveling
into a Coronal Cavity and Its Subsequent Oscillations: New Evidence
    of Fast Mode MHD Waves
Authors: Liu, Wei; Aschwanden, M. J.; Ofman, L.; Nitta, N. V.; Tarbell,
   T. D.
2011SPD....42.0906L    Altcode: 2011BAAS..43S.0906L
  We report new SDO/AIA observations of a global EUV disturbance
  that propagates at 600 km/s and sweeps through a coronal cavity,
  instigating its bodily transverse oscillations. The high temporal
  resolution and large FOV of AIA allow us to clearly see, for the first
  time, the timing coincidence between the onsets of the oscillations
  and the arrival of the disturbance at increasing distances covering
  300 Mm in the neighborhood of the cavity. There is a time delay of
  the oscillations from the near side to the far side of the cavity,
  which is consistent with the travel time of the global perturbation. In
  addition, we find a fine structure consisting of evenly spaced pulses
  of periods 100-120 s within the global disturbance. In contrast, the
  CME loop expansion falls behind the global disturbance at a smaller
  velocity of 200 km/s. These observations suggests that this global
  disturbance is a real fast mode MHD wave that continues propagating
  into the cavity, rather than an apparent wave caused by CME expulsion
  that is not expected to penetrate through a topological separatrix,
  including the flux rope cavity boundary here. The cavity and its
  hosted prominence have oscillation amplitudes of 20 km/s and periods
  of 20-30 minutes. Such unusually long periods, compared with a few
  minutes commonly observed in coronal loops, likely reflect kink mode
  oscillations of the long cavity flux rope of a large length (a fraction
  of the solar radius).

---------------------------------------------------------
Title: Particle energization in 3D magnetic reconnection of
    relativistic pair plasmas
Authors: Liu, Wei; Li, Hui; Yin, Lin; Albright, B. J.; Bowers, K. J.;
   Liang, Edison P.
2011PhPl...18e2105L    Altcode: 2010arXiv1005.2435L
  We present large scale 3D particle-in-cell simulations to examine
  particle energization in magnetic reconnection of relativistic
  electron-positron (pair) plasmas. The initial configuration is set
  up as a relativistic Harris equilibrium without a guide field. These
  simulations are large enough to accommodate a sufficient number of
  tearing and kink modes. Contrary to the non-relativistic limit, the
  linear tearing instability is faster than the linear kink instability,
  at least in our specific parameters. We find that the magnetic
  energy dissipation is first facilitated by the tearing instability
  and followed by the secondary kink instability. Particles are mostly
  energized inside the magnetic islands during the tearing stage due
  to the spatially varying electric fields produced by the outflows
  from reconnection. Secondary kink instability leads to additional
  particle acceleration. Accelerated particles are, however, observed to
  be thermalized quickly. The large amplitude of the vertical magnetic
  field resulting from the tearing modes by the secondary kink modes
  further help thermalizing the non-thermal particles generated from
  the secondary kink instability. Implications of these results for
  astrophysics are briefly discussed.

---------------------------------------------------------
Title: SDO/AIA Observations of Coronal Condensation Leading to
    Prominence Formation
Authors: Liu, Wei; Berger, T.; Low, B. C.; Casini, R.
2011SPD....42.2119L    Altcode: 2011BAAS..43S.2119L
  Coronal condensation takes place when million degree coronal plasma
  undergoes radiative cooling instability. Direct observation of coronal
  condensation in prominences has been difficult in the past, but with the
  launch of the Hinode/SOT and SDO/AIA instruments, numerous observations
  of plasma condensing "out of nowhere" high up in quiescent prominences
  have been captured. We present here one such event seen with SDO/AIA. On
  25-Nov-2010, a prominence above the southwest limb is swept away by
  a nearby eruption, and for next a few hours there is no visible 304
  A material in the local corona. Then, a portion of the coronal loops
  at the same location progressively sags and forms a local dip, where
  the first sign of new, cool material appears, 7.5 hours after the
  eruption. This is a clear indication of coronal condensation, and the
  gradual sag of the loops is likely a result of increasing weight of
  the condensed material that has been accumulated at the dip. Similar
  condensation occurs nearby at a larger rate and leads to the formation
  of a moderate-size prominence. The estimated prominence mass increases
  linearly for about 7 hours at a rate of 2.6e10 grams/sec and reaches
  approximately 6e14 grams. Simultaneously, the prominence drains through
  vertical flows of approximately 32 km/s, bringing the mass back to the
  chromosphere. We estimate the mass drain rate to be 2.7e10 grams/sec,
  which, together with the estimated mass accumulation rate, implies a
  coronal condensation rate of approximately 5.3e10 grams/sec. This study
  can provide critical information about the coupling between condensation
  energetics and MHD, prominence mass cycles, and coronal mass ejections
  initiated by loss of anchoring prominence mass (e.g., Low 2001).

---------------------------------------------------------
Title: Heating of Flare Loops During a Two-ribbon Flare on 2005 May 13
Authors: Qiu, Jiong; Liu, W.; Longcope, D. W.
2011SPD....42.1205Q    Altcode: 2011BAAS..43S.1205Q
  Many eruptive flares exhibit two extended ribbons in the
  lower-atmosphere outlining the feet of the post-flare coronal
  arcade. High-cadence high-resolution UV observations by TRACE reveal
  that a flare ribbon consists of small patches sequentially brightened
  along the ribbon, suggesting that reconnection takes place sequentially
  forming individual post-flare loops along the arcade, as often seen in
  coronal observations in the EUV wavelengths. These reconnection events
  and formation of new loops continue into the decay phase. Our recent
  study (Qiu et al. 2010) further shows that the spatially resolved UV
  brightness at the foot-points of individual loops grows rapidly on
  timescales of 1 minute, followed by a long decay on timescales of more
  than 10 minutes. The rapid rise of UV radiation is correlated with
  the hard X-ray light curve during the impulsive phase, hence is most
  likely a direct response of instantaneous heating in the reconnection
  formed flux tubes. In this study, we utilize the spatially resolved UV
  brightness time profiles to reconstruct instantaneous heating functions
  of individual flux tubes, and compute evolution of each flux tube using
  the EBTEL model (Klimchuk et al. 2008). To build the heating function,
  we take into account the scaling between the total UV peak count rate,
  the hard X-ray energy flux derived from RHESSI spectral analysis during
  the impulsive phase, and as well the reconnection rate that persists
  from the pre-impulsive phase to the decay phase. The sum of the computed
  coronal radiation in all the flux tubes compares favorably with the
  gross coronal radiation observed by GOES. This study presents the
  first effort to constrain heating functions of flare loops directly
  using all available observables, and provides a method to examine
  physics of heating discrete flux tubes formed by reconnection events
  throughout the flare. The work is supported by NSF grant ATM-0748428.

---------------------------------------------------------
Title: Astrophysical Rates for the <SUP>6</SUP>He(p, γ)<SUP>7</SUP>Li
    Reaction
Authors: Li, Er-Tao; Li, Zhi-Hong; Su, Jun; Guo, Bing; Li, Yun-Ju;
   Yan, Sheng-Quan; Bai, Xi-Xiang; Wang, You-Bao; Wang, Bao-Xiang; Lian,
   Gang; Zeng, Sheng; Fang, Xiao; Zhao, Wei-Juan; Liu, Wei-Ping
2011ChPhL..28e2102L    Altcode:
  Angular distribution of the <SUP>6</SUP>He(d,n)<SUP>7</SUP>Li reaction
  at E<SUB>c.m.</SUB>=9.1 MeV is measured in inverse kinematics for
  the first time. The proton spectroscopic factors for the ground
  and first excited states of <SUP>7</SUP>Li are derived by using the
  distorted wave Born approximation analysis. The astrophysical rates
  of <SUP>6</SUP>He(p, γ)<SUP>7</SUP>Li reaction are then deduced and
  fitted with an expression of REACLIB.

---------------------------------------------------------
Title: Preliminary Experimental Result of Magnetic Reconnection in
    Laboratory Plasma
Authors: Zhang, S. B.; Xie, J. L.; Hu, G. H.; Li, H.; Huang, G. L.;
   Liu, W. D.
2011AcASn..52..199Z    Altcode:
  Magnetic reconnection is one of the most important physical processes
  in astrophysical plasmas. Lots of theoretical works, numerical
  simulations and observations have been done. Some experimental
  programs have been activated to investigate the basic mechanisms of
  magnetic reconnection. In order to investigate the electron dynamic
  near the electron diffusion region in magnetic reconnection process,
  an upgrade is accomplished in the LMP (Linear magnetic plasmas) device
  at University of Science and Technology of China. The magnetic field
  of reconnection is produced by passing two identical currents axially
  through two copper plates. Magnetic field and parallel electric field
  are measured by magnetic probes and emissive probes, respectively. The
  existence of a large electric field related to the reconnection process
  is verified. The plasma is driven by electric field and magnetic
  field, so the magnetic reconnection appears. The magnitude of axial
  current is found to scale with the number of passing particles. In
  the configuration of current bars, passing particles are even more and
  our measured axial current is about 10 A. Magnetic flux doesn't pile
  up because of the parameter region in our case, which is consistent
  with the result of numerical simulation.

---------------------------------------------------------
Title: Direct Imaging by SDO/AIA of Quasi-periodic Propagating Fast
    Mode Magnetosonic Waves of  2000 km/s in the Solar Corona
Authors: Liu, Wei; Title, A. M.; Zhao, J.; Ofman, L.; Schrijver,
   C. J.; Aschwanden, M. J.; De Pontieu, B.; Tarbell, T. D.
2011SPD....42.2114L    Altcode: 2011BAAS..43S.2114L
  Quasi-periodic, propagating fast mode magnetosonic waves in the
  corona were difficult to observe in the past due to relatively low
  instrument cadences. We report here unprecedented evidence of such
  waves directly imaged in EUV by the new SDO/AIA instrument. In the 2010
  August 1 C3.2 flare/CME event, we find arc-shaped wave trains of 1-5%
  intensity variations emanating near the flare kernel and propagating
  outward along a funnel of coronal loops. Sinusoidal fits to a typical
  wave train indicate a phase velocity of 2350 +/- 210 km/s. Similar
  waves propagating in opposite directions are observed in closed loops
  between two flare ribbons. In the k-omega diagram of the Fourier wave
  power, we find a bright ridge that represents the dispersion relation
  and can be well fitted with a straight line passing through the
  origin, giving an equal phase and group velocity of 1630 +/- 760 km/s
  averaged over the event. This k-omega ridge shows a broad frequency
  distribution with prominent power at four non-harmonic frequencies,
  5.5, 14.5, 25.1, and 37.9 mHz, among which the 14.5 mHz (period:
  69 s) signal is the strongest. The signal at 5.5 mHz (period: 181 s,
  same as chromospheric 3-minute oscillations) temporally coincides with
  flare pulsations, suggesting a common origin of possibly quasi-periodic
  magnetic reconnection. The instantaneous wave energy flux of (0.1-2.6)e7
  ergs/cm<SUP>2</SUP>/s estimated at the coronal base is comparable to
  the steady-state heating requirement of active region loops.

---------------------------------------------------------
Title: Modeling Fast Magnetosonic Waves Observed by SDO in Active
    region Funnels
Authors: Ofman, Leon; Liu, W.; Title, A.; Aschwanden, M.
2011SPD....42.2104O    Altcode: 2011BAAS..43S.2104O
  Recently, quasi-periodic, propagating waves have been observed in EUV by
  the SDO/AIA instrument in about 10 flare/CME events thus far. A typical
  example is the waves associated with the 2010 August 1 C3.2 flare/CME
  that exhibited arc-shaped wave trains propagating in an active region
  magnetic funnel with 5% intensity variations at speeds in the range
  of 1000-2000 km/s. The fast temporal cadence and high sensitivity of
  AIA enabled the detection of these waves. We identify them as fast
  magnetosonic waves driven quasi-periodically at the base of the flaring
  region, and develop a three-dimensional MHD model of the event. For
  the initial state we utilize the dipole magnetic field to model the
  active region, and include gravitationally stratified density at coronal
  temperature. At the coronal base of the active region we excite the fast
  magnetosonic wave by periodic velocity pulsations in the photospheric
  plane confined to the funnel of magnetic field line. The excited fast
  magnetosonic waves have similar amplitude, wavelength and propagation
  speeds as the observed wave trains. Based on the simulation results, we
  discuss the possible excitation mechanism of the waves, their dynamical
  properties, and the use of the event for coronal MHD seismology.

---------------------------------------------------------
Title: Heating of Flare Loops During a Two-ribbon Flare
Authors: Qiu, Jiong; Liu, W.; Longcope, D. W.
2011SPD....42.2221Q    Altcode: 2011BAAS..43S.2221Q
  Many eruptive flares exhibit two extended ribbons in the
  lower-atmosphere outlining the feet of the post-flare coronal
  arcade. High-cadence high-resolution UV observations by TRACE reveal
  that the flare ribbon consists of small patches sequentially brightened
  along the ribbon, suggesting that reconnection takes place sequentially
  forming individual post-flare loops along the arcade, as often seen in
  coronal observations in the EUV wavelengths. These reconnection events
  and formation of new loops continue well into the decay phase. Our
  recent study (Qiu et al. 2010) further shows that the spatially resolved
  UV brightness at the foot-points of individual loops grows rapidly
  on timescales of 1 minutes, followed by a long decay on timescales of
  more than 10 minutes. The rapid rise of UV radiation is correlated with
  the hard X-ray light curve during the impulsive phase, hence is most
  likely a direct response of instantaneous heating in the reconnection
  formed flux tubes. In this study, we utilize the spatially resolved UV
  brightness time profiles to reconstruct instantaneous heating functions
  of individual flux tubes, and compute evolution of each flux tube using
  the EBTEL model (Klimchuk et al. 2008). To build the heating function,
  we take into account the scaling between the total UV peak count rate,
  the hard X-ray energy flux derived from RHESSI spectral analysis during
  the impulsive phase, and as well the reconnection rate that persists
  from the pre-impulsive phase to the decay phase. The sum of the computed
  coronal radiation in all the flux tubes compares favorably with the
  gross coronal radiation observed by GOES. This study presents the
  first effort to constrain heating functions of flare loops directly
  using all available observables, and provides a method to examine
  physics of heating discrete flux tubes formed by reconnection events
  throughout the flare. This work is supported by NSF grant ATM-0748428.

---------------------------------------------------------
Title: RHESSI and SDO Observation Of HXR and UV/EUV Emissions in
    the 2011 March 7 Solar Flare
Authors: Chen, Qingrong; Petrosian, V.; Liu, W.
2011SPD....42.2231C    Altcode: 2011BAAS..43S.2231C
  We present analysis of the RHESSI and SDO observation of a very unusual
  M3.7 class solar flare on 2011 March 7 from the active region 11164,
  which was also detected by the Fermi Large Area Telescope above 100 MeV
  at gamma-rays and NoRP at microwaves. This flare was accompanied by a
  relatively strong CME and solar energetic particles. <P />During the
  flare, hard X-ray emission up to 300 keV was detected by RHESSI. The
  HXR images at 12-300 keV in the impulsive phase exhibit two footpoint
  sources with an unusually large separation of more than 120 arcsec and
  a thermal loop below 18 keV connecting the two footpoints. On the other
  hand, the SDO/AIA UV and EUV images indicate that the spatial structure
  of the flare is much more complicated than the above HXR picture. The UV
  continuum images at 1600 and 1700 angstrom show three elongated ribbons,
  the outer two being brightest and coincident with the HXR footpoints and
  the middle one without any detectable cospatial HXR source. Furthermore,
  the EUV images show a few arcade systems successively developing during
  the flare, while there are no clear EUV loops seen to connect the two
  HXR footpoints. <P />We will examine the magnetic configuration within
  the flaring regions using the RHESSI, SDO/AIA and SDO/HMI magnetogram
  data, and investigate the relation between UV ribbon brightening and
  electron heating in this flare. The relation between the HXR and EUV
  emission and other observations will be analyzed and described.

---------------------------------------------------------
Title: Slow-Mode Oscillations of Hot Coronal Loops Excited at
    Flaring Footpoints
Authors: Wang, Tongjiang; Liu, W.; Ofman, L.; Davila, J. M.
2011SPD....42.2214W    Altcode: 2011BAAS..43S.2214W
  A large number of strongly damped oscillations in hot coronal loops
  have been observed by SOHO/SUMER in the past decade in Doppler shifts
  of flaring (&gt;6 MK) lines (Fe XIX and Fe XXI). These oscillations
  with periods on the order of 10-30 min were interpreted as fundamental
  standing slow modes. They often manifest features such as recurrence
  and association with a flow (100-300 km/s) pulse preceding to the
  oscillation, which suggests that they are likely driven by microflares
  at the footpoints. With coordinated RHESSI observations, we have found
  a dozen such events supporting this conjecture. A typical event is
  presetned here. By analyzing RHESSI hard X-ray and GOES/SXI soft
  X-ray emissions as well as SUMER Doppler shifts, we identify the
  flare that triggers the loop oscillations. From RHESSI spectra, we
  measure physical parameters such as temperature, emission measure,
  and thermal/non-thermal energy contents as functions of time. We
  discuss the wave excitation mechanism based on these observations. Our
  results provide important observational constraints that can be used
  for improving theoretical models of magnetosonic wave excitation,
  and for coronal seismology.

---------------------------------------------------------
Title: Explanatory Supplement to the WISE Preliminary Data Release
    Products
Authors: Cutri, R. M.; Wright, E. L.; Conrow, T.; Bauer, J.; Benford,
   D.; Brandenburg, H.; Dailey, J.; Eisenhardt, P. R. M.; Evans, T.;
   Fajardo-Acosta, S.; Fowler, J.; Gelino, C.; Grillmair, C.; Harbut,
   M.; Hoffman, D.; Jarrett, T.; Kirkpatrick, J. D.; Liu, W.; Mainzer,
   A.; Marsh, K.; Masci, F.; McCallon, H.; Padgett, D.; Ressler, M. E.;
   Royer, D.; Skrutskie, M. F.; Stanford, S. A.; Wyatt, P. L.; Tholen,
   D.; Tsai, C. W.; Wachter, S.; Wheelock, S. L.; Yan, L.; Alles, R.;
   Beck, R.; Grav, T.; Masiero, J.; McCollum, B.; McGehee, P.; Wittman, M.
2011wise.rept....1C    Altcode:
  The Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010)
  surveyed the entire sky at 3.4, 4.6, 12 and 22 microns in 2010,
  achieving 5-sigma point source sensitivities per band better than
  0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic. The WISE
  Preliminary Data Release, conducted on April 14, 2011, incorporates data
  covering the first ~57% of the sky surveyed that were processed with
  initial calibrations and reduction algorithms. Release data products
  include: (1) an Atlas of 10,464 sets of calibrated, coadded images,
  depth-of-coverage and uncertainty maps in the four WISE bands, (2)
  a Source Catalog containing positions and four-band photometry for 257
  million objects, and (3) an Explanatory Supplement. Ancillary products
  include an archive of 754,000 sets of calibrated WISE single-exposure
  images, uncertainty and bit-mask maps, and a database of 2.2 billion
  source extractions made from the single-exposure images, and moving
  object tracklets identified by the NEOWISE program (Mainzer et
  al. 2011). <P />The Explanatory Supplement to the WISE Preliminary Data
  Release Products is a general guide for users of the WISE data. The
  Supplement contains an overview of the WISE mission, facilities,
  and operations, a description of the contents and formats of the WISE
  image and tabular data products, and cautionary notes that describe
  known limitations of the Preliminary Release products. Instructions
  for accessing the WISE data products via the services of the NASA/IPAC
  Infrared Science Archive are provided. Detailed descriptions of the
  data processing system and algorithms used to ingest and convert
  raw WISE data to the calibrated data products are presented,
  along with assessments of the achieved sky coverage, photometric
  and astrometric characteristics and completeness and reliability
  of the Preliminary Release data products. <P />The WISE Preliminary
  Release Explanatory Supplement is an on-line document that is updated
  frequently to provide the most current information for users of the
  WISE data products. The Explanatory Supplement is maintained at: <P
  />http://wise2.ipac.caltech.edu/docs/release/prelim/expsup/wise_prelrel_toc.html
  <P />WISE is a joint project of the University of California,
  Los Angeles and the Jet Propulsion Laboratory/California
  Institute of Technology, funded by the National Aeronautics and
  Space Administration. NEOWISE is a project of the Jet Propulsion
  Laboratory/California Institute of Technology, funded by the Planetary
  Science Division of the National Aeronautics and Space Administration.

---------------------------------------------------------
Title: Multispacecraft observations of a foreshock-induced
    magnetopause disturbance exhibiting distinct plasma flows and an
    intense density compression
Authors: Turner, D. L.; Eriksson, S.; Phan, T. D.; Angelopoulos, V.;
   Tu, W.; Liu, W.; Li, X.; Teh, W. -L.; McFadden, J. P.; Glassmeier,
   K. -H.
2011JGRA..116.4230T    Altcode:
  Large-scale magnetopause disturbances can result from several different
  types of events, including those resulting from phenomena in the
  foreshock region. In this observational report, we present multipoint
  THEMIS observations of a magnetopause disturbance along the dawnside,
  equatorial flank that exhibits distinct flows in the magnetospheric
  plasma and an abnormally strong compression of the plasma density
  within it, which peaks at &gt;7X the density of the near-Earth solar
  wind. We find that the fastest ion and electron flows are related
  to two different processes, the ion flows resulting from plasma
  being displaced around the disturbance and field-aligned electron
  flows, possibly related to magnetic reconnection. Interestingly, the
  magnetospheric plasma flows around the disturbance are very similar
  to those previously reported around flux transfer events, but we
  conclude that the disturbance is most likely the result of regions of
  compressed and rarified plasma density in the sheath resulting from
  a foreshock cavity. We present simple schematics of this foreshock
  cavity and its leading-edge compression region that explain many
  of the observed features and discuss possibilities for the intense
  density enhancement. Using the simultaneous THEMIS observations from
  the magnetosphere, magnetosheath, and solar wind, we propose that
  the abnormal density enhancement was the result of a combination
  of compression effects due to the magnetosheath and the cavity's
  leading-edge compression region coupled with some complex interaction
  near the magnetopause along the event's distinct boundary layer.

---------------------------------------------------------
Title: Discovery of Panguite, a New Ultra-Refractory Titania Mineral
    in Allende
Authors: Ma, C.; Tschauner, O.; Beckett, J. R.; Kiefer, B.; Rossman,
   G. R.; Liu, W.
2011LPI....42.1276M    Altcode:
  We report here the discovery of panguite (Ti4+,Al,Sc,Mg,Zr,Ca)1.8O3,
  a new titania mineral in Allende, and discuss implications of this
  phase for processes very early in the history of our solar system.

---------------------------------------------------------
Title: The Analysis of the Southwestern Landwater Storage Based on
    GRACE Data
Authors: Liu, W.; Miao, Y. X.
2011AcASn..52..145L    Altcode:
  Based on the 64-month data of GRACE (Gravity Recovery and Climate
  Experiment) from January 2005 to April 2010, the inversion of the
  landwater storage in the southwest China is carried out in this
  paper. GRACE is a near polar orbiting satellite, so the subsatellite
  points become dense with increasing latitude, and thus the region
  with a higher latitude has a higher spatial resolution. By repeated
  calculations and comparison, it is found that with appropriate
  Gaussian radius (R=600 km) in the southwest China and taking the
  monthly average gravitational field as the background gravitational
  field, the landwater storage estimated from GRACE data well reflects
  the climate change and the drought in early 2010.

---------------------------------------------------------
Title: Formation and disruption of current filaments in a flow-driven
    turbulent magnetosphere
Authors: Liu, W. W.; Morales, L. F.; Uritsky, V. M.; Charbonneau, P.
2011JGRA..116.3213L    Altcode: 2010arXiv1008.2938L
  Recent observations have established that the magnetosphere is a system
  of natural complexity. The coexistence of multiscale structures such as
  auroral arcs, turbulent convective flows, and scale-free distributions
  of energy perturbations has lacked a unified explanation, although there
  is strong reason to believe that they all stem from a common base of
  physics. In this paper we show that a slow but turbulent convection
  leads to the formation of multiscale current filaments reminiscent of
  auroral arcs. The process involves an interplay between random shuffling
  of field lines and dissipation of magnetic energy on sub-MHD scales. As
  the filament system reaches a critical level of complexity, local
  current disruption can trigger avalanches of energy release of varying
  sizes, leading to scale-free distributions over energy perturbation,
  power, and event duration. A long-term memory effect is observed whereby
  the filament system replicates itself after each avalanche. The results
  support the view that that the classical and inverse cascades operate
  simultaneously in the magnetosphere. In the former, the high Reynolds
  number plasma flow disintegrates into turbulence through successive
  breakdowns; in the latter, the interactions of small-scale flow eddies
  with the magnetic field can self-organize into elongated current
  filaments and large-scale energy avalanches mimicking the substorm.

---------------------------------------------------------
Title: Chromospheric Jet and Growing "Loop" Observed by Hinode: New
    Evidence of Fan-spine Magnetic Topology Resulting from Flux Emergence
Authors: Liu, Wei; Berger, Thomas E.; Title, Alan M.; Tarbell,
   Theodore D.; Low, B. C.
2011ApJ...728..103L    Altcode: 2010arXiv1012.1897L
  We present observations of a chromospheric jet and growing "loop" system
  that show new evidence of a fan-spine topology resulting from magnetic
  flux emergence. This event, occurring in an equatorial coronal hole on
  2007 February 9, was observed by the Hinode Solar Optical Telescope in
  the Ca II H line in unprecedented detail. The predecessor of the jet is
  a bundle of fine material threads that extend above the chromosphere and
  appear to rotate about the bundle axis at ~50 km s<SUP>-1</SUP> (period
  lsim200 s). These rotations or transverse oscillations propagate upward
  at velocities up to 786 km s<SUP>-1</SUP>. The bundle first slowly and
  then rapidly swings up, with the transition occurring at the onset of an
  A4.9 flare. A loop expands simultaneously in these two phases (velocity:
  16-135 km s<SUP>-1</SUP>). Near the peak of the flare, the loop appears
  to rupture; simultaneous upward ejecta and mass downflows faster than
  free-fall appear in one of the loop legs. The material bundle then
  swings back in a whip-like manner and develops into a collimated jet,
  which is orientated along the inferred open-field lines with transverse
  oscillations continuing at slower rates. Some material falls back along
  smooth streamlines, showing no more oscillations. At low altitudes, the
  streamlines bifurcate at presumably a magnetic null point and bypass
  an inferred dome, depicting an inverted-Y geometry. These streamlines
  closely match in space the late Ca II H loop and X-ray flare loop. These
  observations are consistent with the model that flux emergence in an
  open-field region leads to magnetic reconnection, forming a jet and
  fan-spine topology. We propose that the material bundle and collimated
  jet represent the outer spine in quasi-static and eruptive stages,
  respectively, and the growing loop is a two-dimensional projection of
  the three-dimensional fan surface.

---------------------------------------------------------
Title: Warm Debris Disk Candidates from the Wide-field Infrared
    Survey Explorer (WISE)
Authors: Padgett, Deborah; Liu, W.; Stapelfeldt, K.; Fajardo-Acosta,
   S.; Leisawitz, D.
2011AAS...21733305P    Altcode: 2011BAAS...4333305P
  The Wide Field Infrared Survey Explorer (WISE) has just completed
  a sensitive all-sky survey in photometric bands at 3.4, 4.6, 12,
  and 22 microns. We report on a preliminary investigation of main
  sequence Hipparcos catalog stars with 22 micron emission in excess
  of photospheric levels. This warm excess emission traces material in
  the circumstellar region likely to host terrestrial planets and is
  preferentially found in young systems with ages &lt; 1 Gyr. Nearly a
  hundred new warm debris disk candidates are detected among FGK stars
  within 100 pc and M stars as close as 12 pc, as well as numerous new
  A star disks. We are in the process of obtaining spectra to determine
  spectral types and activity level of these stars and have proposed
  observations to characterize the dust, multiplicity, and substellar
  companions of these systems. In this contribution, we will discuss
  source selection methods and individual examples from among the WISE
  debris disk candidates.

---------------------------------------------------------
Title: Advances in Coordinated Sun-Earth System Science Through
    Interdisciplinary Initiatives and International Programs
Authors: Fichtner, Horst; Liu, W. William
2011sswh.book..341F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Quantum tunnelling of higher-dimensional Kerr-anti-de Sitter
    black holes beyond semi-classical approximation
Authors: Liu, Wei-Wei; Luo, Zhi-Quan; Yang, Juan; Bian, Gang
2011ChPhC..35...22L    Altcode:
  Based on the theory of Klein-Gordon scalar field particles, the Hawking
  radiation of a higher-dimensional Kerr-anti-de Sitter black hole with
  one rotational parameter is investigated using the beyond semi-classical
  approximation method. The corrections of quantum tunnelling probability,
  Hawking temperature and Bekenstein-Hawking entropy are also included.

---------------------------------------------------------
Title: Remote-Sensing Radial Plasma Flows in the Magnetotail Using
    Multiscale Vector Field Techniques
Authors: Uritsky, V. M.; Spanswick, E. L.; Donovan, E. F.; Liang,
   J.; Birn, J.; Knudsen, D. J.; Liu, W.
2010AGUFMSM41A1833U    Altcode:
  Fast radial plasma flows and the associated traveling magnetic
  structures are commonly observed in the magnetotail plasma sheet,
  for example, outside the reconnection diffusion region. In this talk,
  we present a new methodology for analyzing anisotropic multiscale
  signatures of velocity shears, turbulence, and transient vortex
  structures generated by such bursty bulk flows. We generalize the
  higher-order structure function analysis to transient anisotropic
  spatially localized topological features often seen in velocity
  and magnetic fields around the flows. The technique is illustrated
  using the results from a 3-dimensional MHD simulation (J. Birn et
  al, 2009) as well as in situ observations. The time evolution of the
  longitudinal and transverse scaling indices computed using our algorithm
  shows a distinct reproducible pattern of temporary isotropization
  (partly-developed intermittent turbulence) during the passage times
  of the flows, followed by a strongly anisotropic transient behavior
  dominated by large-scale velocity shears. This pattern can be observed
  at a significant azimuthal distance from the flow channel (e.g., several
  times the width scale of the fast flow). We also present multi-spectral
  auroral observations from time periods associated with magnetotail
  equatorial flow channels. We analyze (with similar techniques) the
  auroral response in the regions spanning the ionospheric projection of
  the structured velocity fields. These result are compared to “quiet
  times” where no flow channels are detectable in the magnetotail. The
  results show that the proposed methodology can be used to quantify
  multiscale plasma sheet response to various types of fast convective
  plasma transport in conjunction with ground-based measurements,
  and to clarify the physical origin of eddy plasma dynamics driven by
  these events.

---------------------------------------------------------
Title: Solar wind influence on Pc4 and Pc5 ULF wave activity in the
    inner magnetosphere
Authors: Liu, W.; Sarris, T. E.; Li, X.; Ergun, R.; Angelopoulos,
   V.; Bonnell, J.; Glassmeier, K. H.
2010JGRA..11512201L    Altcode:
  Abundant evidence has shown that ULF wave activity measured at
  geosynchronous orbit is well correlated with solar wind parameters,
  such as the solar wind velocity and dynamic pressure. However, many
  of the past studies were based on magnetic field measurements near the
  equatorial plane and thus could not unambiguously describe ULF waves,
  as magnetic field oscillations in the fundamental toroidal mode have a
  node at the magnetic equator. In this study, we use, for the first time,
  simultaneous electric and magnetic field measurements by Time History
  of Events and Macroscale Interactions during Substorms satellites
  throughout the inner magnetosphere to statistically examine the
  correlation between ULF wave activity in the inner magnetosphere and
  the solar wind parameters: velocity, dynamic pressure, and variation
  in dynamic pressure. On the basis of electric field observations from
  August 2007 to May 2009, we found that, among the three parameters,
  the solar wind velocity has the strongest correlation with the daily
  averaged Pc4 and 5 wave magnitude in 4 ∼ 9 R<SUB>E</SUB>. For example,
  the correlation coefficient of δE<SUB>r</SUB> (the square root of
  the integrated power spectral density of the radial component of the
  electric field) in the Pc5 frequency range with the solar wind dynamic
  pressure is 0.35; with the dynamic pressure variation, it is 0.42;
  and with the solar wind velocity, it is 0.55. However, using only
  magnetic field observations, the variation in dynamic pressure is
  best correlated, with correlation coefficients of δB<SUB>r</SUB>
  (the square root of the integrated power spectral density of the
  radial component of the magnetic field) with the dynamic pressure
  being 0.59, with the dynamic pressure variation being 0.63 and with
  the solar wind velocity being 0.53. We suggest that this difference
  arises because toroidal and poloidal mode pulsations are not detected
  with the same effectiveness in the electric field and the magnetic
  field near the magnetic equator and/or because of the presence of
  broadband ULF noise. We further suggest that either directly measured
  or flow-derived electric field measurements are better suited in the
  study of the relationship between wave power of fundamental field line
  resonance (i.e., in Pc5 frequency range) and solar wind conditions.

---------------------------------------------------------
Title: Multipoint Observation of Fast Mode Waves Trapped in the
    Dayside Plasmasphere
Authors: Takahashi, K.; Bonnell, J. W.; Glassmeier, K.; Angelopoulos,
   V.; Singer, H. J.; Chi, P. J.; Denton, R. E.; Nishimura, Y.; Lee,
   D.; Nose, M.; Liu, W.
2010AGUFMSM22A..05T    Altcode:
  Multipoint observations of a dayside Pc4 pulsation event provide
  evidence of fast mode waves trapped in the plasmasphere (plasmaspheric
  cavity mode or virtual resonance). Time History of Events and Macroscale
  Interactions during Substorms (THEMIS)-A, the primary source of data
  for the present study, was moving outward near noon and detected
  poloidal oscillations, characterized by the azimuthal electric field
  component Ey and the radial and compressional magnetic field components
  Bx and Bz. The structure of the plasmasphere was constructed from the
  mass density radial profile estimated from the frequency of toroidal
  standing Alfvén waves observed at this spacecraft. The outer edge of
  the plasmapause (the maximum of the equatorial Alfvén velocity VAeq)
  was located at L ~ 7, and the minimum of VAeq was located at L ~ 4,
  forming a potential-well structure required for mode trapping. Relative
  to the ground magnetic pulsations observed in the H component at a
  low-latitude station (L = 1.5), the Ey component exhibited a broad
  amplitude maximum around L ~ 3.5 and maintained a nearly constant
  phase from L = 2 to L = 5. In contrast, the Bz component exhibited an
  amplitude minimum and switched its phase by 180° at L = 3.8. This
  radial mode structure is consistent with theoretical models of mode
  trapping. Also, the Ey and Bz components oscillated ±90° out of phase,
  as is expected for radially standing waves.

---------------------------------------------------------
Title: First SDO/AIA Observations of Global Coronal EUV "Waves":
    Multiple Components and "Ripples"
Authors: Liu, W.; Nitta, N. V.; Schrijver, C. J.; Title, A. M.;
   Tarbell, T. D.
2010AGUFMSH13A..07L    Altcode:
  Global coronal EUV disturbances (so-called "EIT waves") are useful
  diagnostics for physical conditions on the Sun. Major drawbacks that
  hindered our understanding of this phenomenon were previous instruments'
  single view point, low cadence (e.g., 12 minutes of EIT), and limited
  wavelength coverage. The Atmospheric Imaging Assembly (AIA) on board
  the Solar Dynamics Observatory (SDO) observes the full-sun corona
  at 10 EUV and UV wavelengths, covering a wide range of temperatures,
  with high resolution (1.4") and cadence (up to 12 s). It thus offers a
  great chance to end the decade long debate on the nature of global EUV
  "waves". We present here the first AIA observations of such phenomenon
  on 2010 April 8 revealed in unprecedented detail and discuss their
  physical implications. The disturbance exhibits two components: one
  weak, diffuse pulse superimposed by multiple strong, sharp fronts,
  which again have slow and fast components. The disturbance originates
  in front of erupting coronal loops and the slow sharp front undergoes
  acceleration, both implying the disturbance being driven by the
  coronal mass ejection (CME). Even at a 20 s cadence, the diffuse pulse
  propagates at a surprisingly constant velocity of ~200 km/s, weakly
  dependent on direction. The fast sharp front overtakes the slow front,
  producing multiple "ripples" and steepening of the local pulse, and both
  fronts propagate independently afterwards. These resemble the nature
  of real waves. Unexpectedly, the amplitude and FWHM of the diffuse
  pulse decreases linearly with distance. The diffuse pulse appears as
  emission enhancement at hotter 193 Å but reduction at cooler 171 Å,
  suggestive of heating, while the sharp fronts appear as enhancement at
  both wavelengths, indicating density increase. As evidence for both
  wave and non-wave models of "EIT waves" has been found, we suggest
  that a hybrid model combining both mechanisms (e.g., Cohen et al. 2010)
  may best explaine the data. In addition to the global EUV disturbance,
  we found fast (600-1100 km/s) features repeated at 100 s intervals
  as tentative evidence of fast mode MHD waves. Discoveries of the fast
  features, multiple ripples, and two-component fronts were made possible
  for the first time thanks to AIA's high cadences and sensitivities.

---------------------------------------------------------
Title: THEMIS measurements of the spatial structure and temporal
    evolution of a dayside poloidal ULF wave event
Authors: Liu, W.; Sarris, T. E.; Li, X.; Ergun, R. E.; Angelopoulos,
   V.; Glassmeier, K.
2010AGUFMSM11B1739L    Altcode:
  In this work, we investigate a strong poloidal ULF wave event in the
  noon sector observed by THEMIS during its coast phase on May 29th,
  2007. In this event, five THEMIS probes were lined up in the same
  outbound path, and consecutively observed narrow-band ULF pulsations
  in the Pc4 and Pc5 frequency range from 0700UT to 1200UT. This
  configuration allows us to investigate the spatial and temporal
  characteristics of the ULF wave activity. The oscillation is strongest
  in the radial component of the magnetic field and extended in the
  region from 5 to 9.5 Re at discrete L shells around 1200 LT. The
  peak frequency of the pulsation decreases with increasing L shell
  from 10mHz to 4mHz. In the region outside the plasmapause, the wave
  power decreases and then increases, showing a temporal evolution that
  appears to be related to the evolution of the plasmasphere. We will
  also discuss the possible excitation mechanism of this poloidal ULF
  wave with simultaneous observations of WIND satellite in the solar
  wind and of Cluster satellites in the magnetosheath. The solar wind
  velocity is relatively steady and there is no sudden impulse of the
  solar wind dynamic pressure during this time period. Cluster observe
  narrow band fluctuations in the number density of the sheath plasma. The
  frequencies of these fluctuations are similar to the frequencies of
  some of the narrow-band poloidal pulsations as observed by THEMIS. This
  correlation seems to support the idea that density fluctuations in
  the upstream might be responsible for the generation of the poloidal
  ULF wave at certain location where the local field line resonance
  frequency matches some of the driving frequencies.

---------------------------------------------------------
Title: Dual scaling for self-organized critical models of the
    magnetosphere
Authors: VallièRes-Nollet, M. -A.; Charbonneau, P.; Uritsky, V.;
   Donovan, E.; Liu, W.
2010JGRA..11512217V    Altcode:
  The central plasma sheet is a complex magnetized plasma structure
  located in the equatorial plane of the magnetotail from where
  substorms are believed to originate. Dynamically, it may behave
  like a self-organized critical (SOC) system, driven by the slow
  energy input of the solar wind. The power law distributions for the
  sizes, energies, and durations of substorms that are reflected in
  observations can be reproduced using such SOC models. However, the
  expected scale invariance does not seem to hold for all scale ranges
  and observables. Recent observations of all-sky auroras have suggested
  a dual regime, where small and large events scale as different power
  laws, the smaller events having a steeper slope. On the other hand,
  scale-dependent substorm behavior can materialize as a consequence of
  an energy loading-unloading cycle. Accordingly, we designed a 2-D SOC
  model subject to global deterministic driving and a nonconservative
  redistribution law. This model can reproduce the coexistence of two
  scaling regimes, with the second regime appearing as a consequence
  of the enhanced spatial development of avalanches caused by a higher
  spatial intermittency in the energy gradients. Thresholded interevent
  waiting time statistics showed a well-defined peak with an exponential
  tail, consistent with observations and the expected dynamics of a
  loading-unloading cycle. Finally, we show that the coherency index
  extracted from the simulations decreases prior to large avalanches, as
  is in fact observed in auroral arcs. This suggests that the coherency
  index may be a useful substorm predictor.

---------------------------------------------------------
Title: An Alternative View of the "Masuda" Flare
Authors: Nitta, Nariaki V.; Freeland, Samuel L.; Liu, Wei
2010ApJ...725L..28N    Altcode:
  The limb flare on 1992 January 13, the so-called Masuda flare,
  has stimulated scientists to refine theory of solar flares based on
  two-dimensional magnetic reconnection. This is primarily because of
  the hard X-ray (HXR) source seen above the clearly defined flare loop,
  and the outward motions in soft X-rays (SXRs) interpreted as "plasmoid"
  ejections. We have revisited Yohkoh HXR and SXR data for this and other
  limb flares and found that the Masuda flare is still unique in terms of
  the location and spectral properties of the coronal HXR source. However,
  the outward motions in SXR outside the flare loop may not be as simply
  characterized as plasmoid ejections as in other flares, nor are they
  particularly fast. The motions appear complex partly because we also see
  trans-equatorial loops in motion, one of whose legs anchors close to the
  main flare loop. It is possible that these large-scale loops represent
  post-flare loops, and that the flare may also be explained in terms of
  three-dimensional quadrupolar reconnection, similar to those flares
  where a pair of two loops exchange their footpoints through magnetic
  reconnection. It appears that expansion and brightening of large-scale
  loops offset from the main flare loop are not common, possibly providing
  a reason for the unusual coronal HXR source in the Masuda flare.

---------------------------------------------------------
Title: Multiscale Anisotropy and Instabilities in a Thin Electron
Current Sheet: Simulation Results and Measurement Recommendations
Authors: Khazanov, I. G.; Uritsky, V. M.; Singh, N.; Donovan, E. F.;
   Liu, W.
2010AGUFMSM51C1833K    Altcode:
  Magnetic reconnection is a fundamental plasma process involving
  nonlinear interactions of vastly separated spatial scales, ranging from
  the large-scale magnetic field geometry enabling the formation of the
  global X-line, to the microscopic plasma properties at ion and electron
  gyroscales controlling fast energy conversion of the reconnecting
  flux and providing physical conditions for particle acceleration
  and heating. In this talk, we investigate simulation outputs from a
  3-dimensional electromagnetic particle-in-cell code (Singh et al., 2006)
  with the objective to understand magnetic signatures of the transient
  multiscale dynamics in the electron diffusion region. The simulation
  reproduces the formation of a thin embedded electron current layer
  in a reversed magnetic field configuration, followed the development
  of electron tearing mode and an explosive electrostatic instability
  leading to reconnection. We use higher-order anisotropic structure
  function (SF) analysis as a tool to quantify topological changes
  of the magnetic field inside and outside of the simulated thin
  electron current layer. The results show temporal evolution of the
  longitudinal and transverse intermittency indices (net deviation of
  the SF exponents form the fully developed turbulent state) suggesting a
  formation of anisotropic magnetic field structures during the tearing
  mode growth. This anisotropy decreases once the instability becomes
  explosive. The estimated growth time of 60-70 electron plasma periods
  of the transverse SF index is in an agreement with the theoretical
  prediction for the electron tearing mode instability. The results
  obtained shed new light on the forces and interactions governing
  time evolution of the multiscale magnetic field topology accompanying
  tearing mode growth at different stages of the initial instability,
  and provide important clues for monitoring reconnection onset events
  using multiscale in situ measurements conducted at various distances
  from the neutral sheet.

---------------------------------------------------------
Title: Multi-point measurements of the spatial extent and azimuthal
    mode number of ULF waves
Authors: Sarris, T. E.; Li, X.; Liu, W.
2010AGUFMSM11B1745S    Altcode:
  Magnetospheric ULF (Ultra-Low Frequency) waves have frequencies in
  the mHz range, comparable with the drift frequency of high-energy
  particles, with which they are believed to resonantly interact. A
  critical parameter in this interaction is the azimuthal mode number of
  the waves, which determines the resonant condition for drift-resonant
  acceleration, and also the spatial extent of the waves. In this study
  we investigate the spatial extent using multi-point measurements
  in the magnetosphere and on the ground and we compare different
  measurement techniques for estimating the azimuthal mode number, such
  as by using azimuthally displaced satellites in the magnetosphere,
  by using longitudinally aligned magnetometers on the ground and by
  studying signatures of energetic particle flux modulations. Case
  studies are presented and compared.

---------------------------------------------------------
Title: First SDO AIA Observations of a Global Coronal EUV "Wave":
    Multiple Components and "Ripples"
Authors: Liu, Wei; Nitta, Nariaki V.; Schrijver, Carolus J.; Title,
   Alan M.; Tarbell, Theodore D.
2010ApJ...723L..53L    Altcode: 2012arXiv1201.0815L
  We present the first Solar Dynamics Observatory Atmospheric Imaging
  Assembly (AIA) observations of a global coronal EUV disturbance
  (so-called "EIT wave") revealed in unprecedented detail. The disturbance
  observed on 2010 April 8 exhibits two components: one diffuse pulse
  superimposed, on which are multiple sharp fronts that have slow and
  fast components. The disturbance originates in front of erupting coronal
  loops and some sharp fronts undergo accelerations, both effects implying
  that the disturbance is driven by a coronal mass ejection. The diffuse
  pulse, propagating at a uniform velocity of 204-238 km s<SUP>-1</SUP>
  with very little angular dependence within its extent in the south,
  maintains its coherence and stable profile for ~30 minutes. Its arrival
  at increasing distances coincides with the onsets of loop expansions and
  the slow sharp front. The fast sharp front overtakes the slow front,
  producing multiple "ripples" and steepening the local pulse, and both
  fronts propagate independently afterward. This behavior resembles
  the nature of real waves. Unexpectedly, the amplitude and FWHM of
  the diffuse pulse decrease linearly with distance. A hybrid model,
  combining both wave and non-wave components, can explain many, but
  not all, of the observations. Discoveries of the two-component fronts
  and multiple ripples were made possible for the first time thanks to
  AIA's high cadences (&lt;=20 s) and high signal-to-noise ratio.

---------------------------------------------------------
Title: Helium-star evolutionary channel to super-Chandrasekhar mass
    type Ia supernovae
Authors: Liu, W. -M.; Chen, W. -C.; Wang, B.; Han, Z. W.
2010A&A...523A...3L    Altcode: 2010arXiv1007.4751L
  The recent discovery of several overluminous type Ia supernovae
  (SNe Ia) indicates that the explosive masses of white dwarfs may
  significantly exceed the canonical Chandrasekhar-mass limit. Rapid
  differential rotation may support these massive white dwarfs
  (WDs). Based on the single-degenerate scenario and assuming that the
  WDs would differentially rotate when the accretion rate dot{M} &gt;
  3 × 10<SUP>-7</SUP> M<SUB>⊙</SUB> yr<SUP>-1</SUP>, we performed
  the numerical calculations for 1000 binary systems consisting of a He
  star and a CO WD with Eggleton's stellar evolution code. We present the
  initial parameters in the orbital period - helium star-mass plane (for
  WD masses of 1.0 M<SUB>⊙</SUB> and 1.2 M<SUB>⊙</SUB>, respectively),
  which lead to super-Chandrasekhar mass SNe Ia. Our results indicate that
  for an initially massive WD of 1.2 M<SUB>⊙</SUB>, a large number of
  SNe Ia may result from super-Chandrasekhar mass WDs. The highest mass
  of the WD at the moment of the SNe Ia explosion is 1.81 M_⊙, but
  very massive (&gt;1.85 M<SUB>⊙</SUB>) WDs cannot be formed. However,
  when the initial mass of WDs is 1.0 M<SUB>⊙</SUB>, the explosive
  masses of SNe Ia are nearly uniform, which is consistent with the
  rareness of super-Chandrasekhar mass SNe Ia in observations.

---------------------------------------------------------
Title: The littlest Higgs model with T-parity and some lepton flavor
    violation decay processes
Authors: Yue, Chongxing; Ma, Wei; Zhang, Tingting; Liu, Wei; Liu,
   Jinyan
2010SCPMA..53.1968Y    Altcode: 2010ScChG..53.1968Y
  The new particles predicted by the littlest Higgs model with T-parity
  (called LHT model) can induce the lepton flavor violation (LFV)
  couplings at the one-loop level, which can add contributions to some
  LFV processes. Taking into account the constraints of the experimental
  data on the relevant free parameters, we calculate the branching
  ratios of the LFV decay processes Z → lbar l' and τ <SUP>-</SUP>
  → µ<SUP>-</SUP> P <SUB>1</SUB> P <SUB>2</SUB> with P <SUB>1</SUB>
  P <SUB>2</SUB> = π <SUP>+</SUP> π <SUP>-</SUP>, K <SUP>+</SUP> K
  <SUP>-</SUP>, and K <SUP>0</SUP> bar K^0 in the context of this new
  physics model. We find that the LHT model can indeed make significant
  contributions to some of these LFV decay processes. The Z factory
  option for the future high energy e <SUP>+</SUP> e <SUP>-</SUP>
  collider experiments will give severe constraints on the LHT model.

---------------------------------------------------------
Title: A transient narrow poleward extrusion from the diffuse aurora
    and the concurrent magnetotail activity
Authors: Lui, A. T. Y.; Spanswick, E.; Donovan, E. F.; Liang, J.;
   Liu, W. W.; Le Contel, O.; Zong, Q. -G.
2010JGRA..11510210L    Altcode:
  We report observation of a transient narrow auroral feature extruding
  from the poleward boundary of the diffuse aurora on March 19, 2009. It
  moved westward and poleward initially to form part of a vortex pattern,
  followed by its equatorward-dawnward retreat later. During this
  auroral activity, THEMIS satellites, projected near the same magnetic
  local time of the auroral feature, detected appreciable plasma flows,
  increase in the ratio of the ion energy over the electron energy,
  and some enhancements of electrostatic waves. The plasma flows were
  initially duskward-earthward and changed to duskward-tailward later. The
  overall development of the observed plasma flow pattern was detected
  during the equatorward-dawnward retreat of the auroral feature when
  the Alfvén transit time between the magnetotail and the ionosphere
  is taken into account. This suggests that THEMIS satellites remotely
  sensed a counter-clockwise flow vortex (viewed from above the equatorial
  plane) in the magnetotail with decreasing strength. We suggest that the
  process generating the auroral feature is related to the flow vortex
  in association with the depletion of the electron energy relative
  to the ion energy and wave-particle interaction. An estimate of the
  possible associated current density is made. We provide reasoning for
  this auroral feature to be an auroral streamer and not a “failed”
  transpolar arc.

---------------------------------------------------------
Title: Record warming in the South Pacific and western Antarctica
    associated with the strong central-Pacific El Niño in 2009-10
Authors: Lee, Tong; Hobbs, William R.; Willis, Joshua K.; Halkides,
   Daria; Fukumori, Ichiro; Armstrong, Edward M.; Hayashi, Akiko K.;
   Liu, W. Timothy; Patzert, William; Wang, Ou
2010GeoRL..3719704L    Altcode:
  Satellite data for the past three decades reveal a record-high
  sea surface temperature (SST) anomaly within a large mid-latitude
  region of the south-central Pacific (SCP) during the mature phase
  of the 2009-10 El Niño, with a peak magnitude that is 5 times
  the standard deviation of local SST anomaly and is warmer than the
  concurrent tropical-Pacific SST anomaly. The SCP oceanic warming was
  confined to the upper 50 meters and is associated with an extreme and
  persistent anticyclone. Wind changes associated with the anticyclone
  caused the oceanic warming with surface heat flux and ocean processes
  playing equally important roles. The anticyclone diverted circumpolar
  westerlies and warm air towards Antarctica. Austral-summer SST in
  the Bellingshausen Sea also reached a three-decade high. The extreme
  atmospheric and oceanic anomalies in the South Pacific may have been
  fueled by the 2009-10 El Niño because of its record-high SST anomaly
  in the central-equatorial Pacific.

---------------------------------------------------------
Title: 返回舱动态稳定性分析及被动控制方法研究
Authors: 赵, 海洋; 杨, 小亮; 刘, 伟
2010SSPMA..40.1156.    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Influence of super-strong magnetic field on the electron
    chemical potential and β decay in the stellar surroundings
Authors: Liu, Wei-Wei; Luo, Zhi-Quan; Zhang, Jie; Gao, Jie; Bian, Gang
2010ChPhC..34.1090L    Altcode:
  In this paper, considering the quantum effect of electrons in a
  super-strong magnetic field, the influence of a super-strong magnetic
  field on the chemical potential of a non-zero temperature electron is
  analyzed, the rates of β decay under the super-strong magnetic field
  are studied, and then we compare them with the case without a magnetic
  field. Here, the nucleus <SUP>63</SUP>Co is investigated in detail as
  an example. The results show that a magnetic field that is less than
  10<SUP>10</SUP> T has little effect on the electron chemical potential
  and β decay rates, but the super-strong magnetic field that is greater
  than 10<SUP>10</SUP> T depresses the electron chemical potential and
  improves the β decay rates clearly.

---------------------------------------------------------
Title: An in situ XAS study of copper(I) transport as hydrosulfide
complexes in hydrothermal solutions (25-592 °C, 180-600 bar):
    Speciation and solubility in vapor and liquid phases
Authors: Etschmann, B. E.; Liu, W.; Testemale, D.; Müller, H.; Rae,
   N. A.; Proux, O.; Hazemann, J. L.; Brugger, J.
2010GeCoA..74.4723E    Altcode:
  Chloride and hydrosulfide are the principal ligands assumed to govern
  transport of copper in hydrothermal fluids. Existing solubility
  experiments suggest that Cu(I)-hydrosulfide complexes are dominant
  compared to chloride complexes at low salinities in alkaline solutions
  (H <SUB>2</SUB>S <SUB>(aq)</SUB>/HS <SUP>-</SUP> pH buffer), and
  may be important in transporting Cu in low density magmatic vapors,
  potentially controlling the liquid-vapor partitioning of Cu. This
  study provides the first in situ evidence of the solubility of copper
  sulfides and the nature and structure of the predominant Cu species in
  sulfur-containing fluids at temperatures up to 592 °C and pressures of
  180-600 bar. XANES and EXAFS data show that at elevated T (⩾200 °C),
  Cu solubility occurs via a linear Cu complex. At 428 °C in alkaline
  solutions, Cu is coordinated by two sulfur atoms in a distorted linear
  coordination (angle ∼150-160°). This geometry is consistent with the
  species Cu(HS)2- predicted by earlier solubility studies. In addition,
  in situ measurements of the solubility of chalcocite in 2 m NaHS
  solutions performed in this study are in remarkably good agreement
  with the solubilities calculated using available thermodynamic data
  for Cu(I)-hydrosulfide complexes, also supporting the interpretation
  of speciation in these studies and validating the extrapolation of
  low- T thermodynamic properties for Cu(HS)2- to high P- T. Data on
  phase separation for the 2 m NaHS solution show that while significant
  amounts of copper can be partitioned into the vapor phase, there is no
  indication for preferential partitioning of Cu into the vapor. This
  is consistent with recent partitioning experiments conducted in
  autoclaves by Pokrovski et al. (2008a) and Simon et al. (2006). XANES
  data suggest that the species present in the low density phase is very
  similar to that present in the high density liquid, i.e., Cu(HS)2-,
  although Cu(HS)(H <SUB>2</SUB>S) <SUP>0</SUP> cannot be excluded on
  the basis of XAS data.

---------------------------------------------------------
Title: THEMIS observations of the spatial extent and pressure-pulse
    excitation of field line resonances
Authors: Sarris, T. E.; Liu, W.; Li, X.; Kabin, K.; Talaat, E. R.;
   Rankin, R.; Angelopoulos, V.; Bonnell, J.; Glassmeier, K. -H.
2010GeoRL..3715104S    Altcode:
  We present a case study of Field Line Resonances (FLRs) in the dayside
  magnetosphere, observed in both electric and magnetic field components
  at multiple L-shells near the equator. The event measured by the five
  THEMIS probes and the nearby GOES and Geotail satellites provides
  a unique opportunity to differentiate between temporal and spatial
  characteristics of FLRs. Narrow-band FLRs were excited globally
  at different frequencies matching the local field line resonant
  frequency. In conjunction with a sharp increase in the upstream solar
  wind density, prompt intensification of the FLR power was observed
  at different L-shells, simultaneously at different frequencies and
  amplitudes.

---------------------------------------------------------
Title: The Fomalhaut debris disk seen from every angle with
    interferometry
Authors: Absil, O.; Mennesson, B.; Le Bouquin, J. -B.; Augereau,
   J. -C.; Millan-Gabet, R.; Colavita, M.; Hinz, P.; Liu, W.; Serabyn, G.
2010SPIE.7734E..17A    Altcode: 2010SPIE.7734E..34A
  In this paper, we present the results of three different studies of the
  Fomalhaut debris disk with infrared interferometry. First, VLTI/AMBER
  measurements are used to determine the position angle of the slightly
  oblate rapidly rotating photosphere by means of differential phase
  measurements across the Br-gamma photospheric line. This measurement
  allows us to confirm that the debris disk is located in the equatorial
  plane of its host star. Second, we use VLTI/VINCI to search for
  resolved near-infrared emission around the stellar photosphere, which
  would correspond to the presence of large amounts of hot dust grains
  located between the sublimation radius and the habitable zone. Our
  observations reveal a small excess of 0.88%+/-0.12% in K band relative
  to the photospheric flux. Finally, we use the Keck Interferometer Nuller
  in order to derive additional constraints on the nature of the resolved
  infrared emission. Our observations suggest a marginal detection of a
  circumstellar excess at 10 μm, which we use together with the VINCI
  detection to model the circumstellar emission. Preliminary results
  from this modeling effort are discussed.

---------------------------------------------------------
Title: Neutron Spectroscopic Factors of <SUP>7</SUP>Li and
    Astrophysical <SUP>6</SUP>Li(n,γ)<SUP>7</SUP>Li Reaction Rates
Authors: Su, Jun; Li, Zhi-Hong; Guo, Bing; Bai, Xi-Xiang; Li,
   Zhi-Chang; Liu, Jian-Cheng; Wang, You-Bao; Lian, Gang; Zeng, Sheng;
   Wang, Bao-Xiang; Yan, Sheng-Quan; Li, Yun-Ju; Li, Er-Tao; Fan, Qi-Wen;
   Liu, Wei-Ping
2010ChPhL..27e2101S    Altcode: 2010arXiv1001.4329S
  Angular distributions of the <SUP>7</SUP>Li(<SUP>6</SUP>Li,
  <SUP>6</SUP>Li)<SUP>7</SUP>Li elastic scattering
  and the <SUP>7</SUP>Li(<SUP>6</SUP>Li,
  <SUP>7</SUP>Li<SUB>g.s.</SUB>)<SUP>6</SUP>Li,
  <SUP>7</SUP>Li(<SUP>6</SUP>Li,
  <SUP>7</SUP>Li<SUB>0.48</SUB>)<SUP>6</SUP>Li transfer reactions
  at E<SUB>c.m.</SUB> = 23.7 MeV are measured with the Q3D magnetic
  spectrograph. The optical potential of <SUP>6</SUP>Li + <SUP>7</SUP>Li
  is obtained by fitting the elastic scattering differential cross
  sections. Based on the distorted wave Born approximation (DWBA)
  analysis, spectroscopic factors of <SUP>7</SUP>Li = <SUP>6</SUP>Li
  otimes n are determined to be 0.73 ± 0.05 and 0.90 ± 0.09 for the
  ground and first exited states in <SUP>7</SUP>Li, respectively. Using
  the spectroscopic factors, the cross sections of the <SUP>6</SUP>Li(n,
  γ<SUB>0, 1</SUB>)<SUP>7</SUP>Li direct neutron capture reactions and
  the astrophysical <SUP>6</SUP>Li(n, γ)<SUP>7</SUP>Li reaction rates
  are derived.

---------------------------------------------------------
Title: New Insights to Global Coronal EUV Waves: First Double
    Quadrature Observations by SDO/AIA and STEREO/EUVI
Authors: Liu, Wei; Nitta, N. V.; Schrijver, C. J.; Title, A. M.
2010AAS...21640230L    Altcode:
  Global coronal EUV waves are useful diagnostic tools for physical
  conditions on the Sun. Major drawbacks that hindered our understanding
  of EUV waves were previous instruments' low cadence (e.g., 12
  minutes for SoHO/EIT) and limited spatial resolution and wavelength
  coverage. The Atmospheric Imaging Assembly (AIA) on board the recently
  launched Solar Dynamics Observatory (SDO), joined by the STEREO EUV
  Imager (EUVI), offers a great chance to end the decade long debate
  on the nature of global EUV waves. AIA observes the corona at 10 EUV
  and UV wavelengths, covering a wide range of temperatures. It has high
  resolution (0.6") and cadence (20 s, 7 times faster than EUVI). These
  capabilities allow us to study the thermal structure and kinematics
  of EUV waves in unprecedented detail. We present here the first AIA
  observations of an EUV wave occurring on 2010 April 8. AIA observed
  this event on the solar disk, while the STEREO Ahead (A) and Behind
  (B) spacecraft, which were 67 degree ahead and 72 degree behind the
  Earth, respectively, provided side views of both the EUV wave and the
  halo coronal mass ejection (seen by SoHO/LASCO) near the limb. This
  formed a double quadrature configuration with great advantages to
  infer the 3D structure. Initial analysis indicates that this wave
  exhibited strong anisotropy, propagating primarily toward the south,
  on the same side of the erupting loop system. We will examine its
  spatial and temporal relationship with the erupting loop and CME and
  discuss physical implications.

---------------------------------------------------------
Title: Direct Imaging of an Emerging Flux Rope and a Resulting
    Chromospheric Jet Observed by Hinode
Authors: Liu, Wei; Berger, T.; Title, A. M.; Tarbell, T. D.; DeRosa, M.
2010AAS...21640307L    Altcode: 2010BAAS...41R.878L
  Magnetic flux emergence has been traditionally observed on the disk by
  identifying changes in magnetograms. Observations near the limb offer
  an alternative perspective and allow direct imaging of emerging flux
  ropes. We present Hinode/SOT Ca II H observations of such an event in
  an equatorial coronal hole on 2007 February 9. The precursor of the
  event was a bundle of fine material threads that extended at an oblique
  angle above the chromosphere and appeared to rotate about a common
  axis. This bundle first slowly and then rapidly swung up, accompanied
  by a loop that appeared at the base of the bundle and expanded at
  comparable rates. During the first (slow rise) stage, the apex of the
  loop ascended at 16 km/s, a velocity similar to that of H-alpha arch
  filaments (e.g., Chou &amp; Zirin) and of emerging flux ropes expanding
  into the corona as found in MHD simulations (e.g., Fan &amp; Gibson;
  Martinez-Sykora). The second stage started at the onset of a GOES A5
  flare and the loop expansion accelerated, reaching a velocity of 130
  km/s when the loop appeared to rupture near the peak of the flare. The
  material bundle then swung back in a whiplike manner and developed into
  a collimated jet, exhibiting oscillatory transverse motions across its
  axis, as expected from unwinding twists. Some jet material fell back
  along smooth streamlines, which bypass an unseen dome and presumably
  a null point in the low corona, depicting an inverted-Y shape. Some
  of these observations resemble the model (e.g., Uchida &amp; Shibata)
  of the emergence of a twisted flux rope into an open field region that
  leads to reconnection and formation of a jet. Some observations are,
  however, not predicted in previous models and we will discuss their
  implications.

---------------------------------------------------------
Title: Energetics in Two-ribbon Flares
Authors: Qiu, Jiong; Liu, W.; Hill, N.; Kazachenko, M.
2010AAS...21632101Q    Altcode: 2010BAAS...41..911Q
  We conduct a semi-quantitative analysis of two-ribbon flares to relate
  the pattern of magnetic reconnection and energetics during the flare. We
  establish a correlation between UV emission and &gt;30 keV hard X-ray
  emission, so that evolution of the flare morphology illustrated in
  high resolution UV images is used to infer non-thermal particle
  precipitation. In the few two-ribbon flares under investigation,
  the flare UV ribbons exhibit apparent motion both parallel with
  and perpendicular to the magnetic polarity inversion line of the
  active region. We note that the perpendicular spread of the UV ribbon
  dominates the peak phase of hard X-rays, when the parallel motion is
  nearly halted. With a local 2.5D assumption, we decompose the magnetic
  reconnection rate into two parts ψ<SUB>||</SUB> and ψ<SUB>perp</SUB>,
  ψ<SUB>||</SUB> being related to the parallel expansion of the UV
  ribbon, and ψ<SUB>perp</SUB> being related to the perpendicular
  expansion of the UV ribbon. It is found that non-thermal energy
  release is strongly correlated with ψ<SUB>perp</SUB>. We explore
  an empirical scaling law between non-thermal energy release and the
  pattern of magnetic reconnection. This work is supported by the NSF
  grant ATM-0748428, NASA grant NNX08AE44G, and NSF REU grant ATM-0552958.

---------------------------------------------------------
Title: Indirect measurement of nuclear reactions of astrophysical
    interest
Authors: Liu, W. P.; Li, Z. H.; Bai, X. X.; Wang, Y. B.; Guo, B.;
   Lian, G.; Su, J.; Zeng, S.; Wang, B. X.; Yan, S. Q.; Li, Y. J.; Li,
   E. T.; Jin, S. J.
2010AIPC.1235..322L    Altcode:
  Systematic indirect measurements of nuclear astrophysical
  reactions using the unstable ion beam facility GIRAFFE in CIAE
  were performed. We have measured the angular distributions of
  transfer reactions, such as <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li,
  <SUP>8</SUP>Li(d,n)<SUP>9</SUP>Be and <SUP>8</SUP>Li(p,d)<SUP>7</SUP>Li
  in inverse kinematics, and derived the astrophysical S-factors
  or reaction rates for <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li and
  <SUP>8</SUP>Li(p,γ)<SUP>9</SUP>Be by using asymptotic normalization
  coefficient (ANC) or spectroscopic factor methods.

---------------------------------------------------------
Title: Salinity Variations in Water Column due to Outflows Estimated
    by Multi-Sensor Remote Sensing
Authors: Yan, Xiao-Hai; Jo, Young-Heon; Liu, W. Timothy; Dai, Minhan
2010aogs...18..109Y    Altcode:
  The following sections are included: <P />* Introduction <P />*
  Theoretical Background, Methodology, Data and Error Analysis <P />*
  Results <P />* River discharge <P />* Amazon river discharge * Yangtze
  river discharge * Mediterranean eddy and outflow <P />* Conclusions
  <P />* Acknowledgments <P />* References

---------------------------------------------------------
Title: Electrostatic field and ion temperature drop in thin current
sheets: A theory
Authors: Liu, W. W.; Liang, J.; Donovan, E. F.
2010JGRA..115.3211L    Altcode: 2010JGRA..11503211L
  The observational evidence presented by Liang et al. (2009) showed
  that a neutral sheet-pointing electrostatic field frequently arises in
  the late growth-phase current sheet in the magnetotail. In this paper,
  we elaborate on the suggestion that this electric field is associated
  with the thinning of the current sheet to the ion scale at which
  the electron and ion current sheets begin to separate. The attendant
  effect of a decreasing ion temperature, also interpreted in terms of
  a thinning current sheet, suggests that a cold plasma population is
  involved. We review existing theories of “charged” Harris sheet
  that can produce electrostatic fields and show that they cannot explain
  the observations for various reasons. A particular problem is the over
  shielding of the electrostatic field by the cold population embedding
  the current sheet. We argue that this problem stems from not treating
  the cold plasma as a separate population from the hot plasma forming
  the thin current sheet (TCS). We show that if the cold population is
  treated as external to the TCS and behaving in a largely MHD manner,
  the resultant solution yields an electrostatic field and ion temperature
  drop consistent with the observations.

---------------------------------------------------------
Title: Lithium induced nuclear reactions of astrophysical interest
Authors: Liu, W. P.; Li, Z. H.; Bai, X. X.; Wang, Y. B.; Lian, G.; Guo,
   B.; Su, J.; Zeng, S.; Wang, B. X.; Yan, S. Q.; Li, Y. J.; Li, E. T.
2010NuPhA.834..651L    Altcode:
  Systematic studies of nuclear astrophysical reactions induced by lithium
  isotopes using the unstable ion beam facility GIRAFFE in CIAE were
  performed. We have measured the angular distributions of some single
  nucleon transfer reactions, such as <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li,
  <SUP>8</SUP>Li(d,n)<SUP>9</SUP>Be and <SUP>8</SUP>Li(p,d)<SUP>7</SUP>Li
  in inverse kinematics, and derived the astrophysical S-factors
  or reaction rates for <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li and
  <SUP>8</SUP>Li(p,γ)<SUP>9</SUP>Be by using asymptotic normalization
  coefficient (ANC) or spectroscopic factor.

---------------------------------------------------------
Title: <SUP>2</SUP>H(<SUP>6</SUP>He,<SUP>7</SUP>Li)n,
    <SUP>12</SUP>C(<SUP>7</SUP>Li, <SUP>6</SUP>He)<SUP>13</SUP>N reactions
    and <SUP>12</SUP>C(p,γ)<SUP>13</SUP>N astrophysical S(E) factors
Authors: Li, Z. H.; Su, J.; Guo, B.; Li, E. T.; Li, Z. C.; Bai, X. X.;
   Li, Y. J.; Liu, J. C.; Yan, S. Q.; Wang, B. X.; Wang, Y. B.; Lian,
   G.; Zeng, S.; Fang, X.; Liu, W. P.; Chen, Y. S.; Shu, N. C.; Fan, Q. W.
2010NuPhA.834..661L    Altcode:
  Angular distributions of <SUP>2</SUP>H(<SUP>6</SUP>He,<SUP>7</SUP>Li)n
  and <SUP>12</SUP>C(<SUP>7</SUP>Li,<SUP>6</SUP>He)<SUP>13</SUP>N
  reactions were measured at the HI-13 tandem accelerator,
  Beijing. Asymptotic normalization coefficient (ANC) of <SUP>13</SUP>N
  → <SUP>12</SUP>C + p was derived to be 1.64±0.11 fm<SUP>-1</SUP>
  through distorted wave Born approximation (DWBA) analysis, which was
  then used to deduce the astrophysical S(E) factors for direct capture
  in <SUP>12</SUP>C(p,γ)<SUP>13</SUP>N at energies of astrophysical
  relevance.

---------------------------------------------------------
Title: The 33S(p,γ)34Cl reaction in classical nova explosions
Authors: Parikh, A.; Faestermann, T.; Krücken, R.; Bildstein, V.;
   Bishop, S.; Eppinger, K.; Herlitzius, C.; Lepyoshkina, O.; Maierbeck,
   P.; Seiler, D.; Wimmer, K.; Hertenberger, R.; Wirth, H. F.; Fallis,
   J.; Hager, U.; Hutcheon, D. A.; Ruiz, C.; Buchmann, L.; Ottewell,
   D.; Freeman, B.; Wrede, C.; Garcia, A.; Delbridge, B.; Knecht, A.;
   Sallaska, A.; Chen, A.; Clark, J. A.; Deibel, C.; Fulton, B. R.;
   Laird, A.; Greife, U.; Guo, B.; Li, E.; Li, Z.; Lian, G.; Wang, Y.;
   Liu, W.; Parker, P.; Setoodehnia, K.
2010nuco.confE..52P    Altcode: 2010PoS...100E..52P
  No abstract at ADS

---------------------------------------------------------
Title: System-level musings about system-level science (Invited)
Authors: Liu, W.
2009AGUFMSM11D..01L    Altcode:
  In teleology, a system has a purpose. In physics, a system has a
  tendency. For example, a mechanical system has a tendency to lower
  its potential energy. A thermodynamic system has a tendency to
  increase its entropy. Therefore, if geospace is seen as a system,
  what is its tendency? Surprisingly or not, there is no simple answer
  to this question. Or, to flip the statement, the answer is complex,
  or complexity. We can understand generally why complexity arises,
  as the geospace boundary is open to influences from the solar wind
  and Earth’s atmosphere and components of the system couple to
  each other in a myriad of ways to make the systemic behavior highly
  nonlinear. But this still begs the question: What is the system-level
  approach to geospace science? A reductionist view might assert that
  as our understanding of a component or subsystem progresses to a
  certain point, we can couple some together to understand the system
  on a higher level. However, in practice, a subsystem can almost never
  been observed in isolation with others. Even if such is possible,
  there is no guarantee that the subsystem behavior will not change
  when coupled to others. Hence, there is no guarantee that a subsystem,
  such as the ring current, has an innate and intrinsic behavior like a
  hydrogen atom. An absolutist conclusion from this logic can be sobering,
  as one would have to trace a flash of aurora to the nucleosynthesis
  in the solar core. The practical answer, however, is more promising;
  it is a mix of the common sense we call reductionism and awareness
  that, especially when strongly coupled, subsystems can experience
  behavioral changes, breakdowns, and catastrophes. If the stock answer
  to the systemic tendency of geospace is complexity, the objective of
  the system-level approach to geospace science is to define, measure,
  and understand this complexity. I will use the example of magnetotail
  dynamics to illuminate some key points in this talk.

---------------------------------------------------------
Title: Motion of Auroral Features and Plasmasheet Flow
Authors: Spanswick, E. L.; Donovan, E. F.; Lui, A.; Kepko, E. L.;
   Liang, J.; Liu, W.
2009AGUFMSM53D..06S    Altcode:
  The aurora is often interpreted as a projection of large scale dynamics
  occurring in the central plasma sheet. This is only one mechanism
  for driving changes in auroral structure and luminosity and we do not
  know when (and to what extent) magnetotail processes determine auroral
  morphology. What specific auroral features are directly driven by and/or
  related to individual magnetospheric processes? Using data from the
  THEMIS white light and NORSTAR multi-spectral imagers we investigate
  the relationship between plasma sheet flow and the motion of auroral
  features. We use data from a twenty day period, starting in late March
  2009, when the NORSTAR imagers operated in a high resolution mode
  capturing the red-line aurora at a six second cadence (synchronized
  with the THEMIS ASI array). Concurrent THEMIS spacecraft observations
  are used as a measure of local plasma sheet flow. We present results
  from the survey of optical and spacecraft data and discuss the possible
  connection between auroral and magnetospheric motion.

---------------------------------------------------------
Title: An Intriguing Chromospheric Jet Observed by Hinode: Fine
    Structure Kinematics and Evidence of Unwinding Twists
Authors: Liu, Wei; Berger, Thomas E.; Title, Alan M.; Tarbell,
   Theodore D.
2009ApJ...707L..37L    Altcode: 2009arXiv0910.5186L
  We report a chromospheric jet lasting for more than 1 hr observed by
  the Hinode Solar Optical Telescope in unprecedented detail. The ejection
  occurred in three episodes separated by 12-14 minutes, with the amount
  and velocity of material decreasing with time. The upward velocities
  range from 438 to 33 km\nolimits s\nolimits ^{-1}, while the downward
  velocities of the material falling back have smaller values (mean:
  -56 km\nolimits s\nolimits ^{-1}) and a narrower distribution (standard
  deviation: 14 km\nolimits s\nolimits ^{-1}). The average acceleration
  inferred from parabolic spacetime tracks is 141 m\nolimits s^{-2}, a
  fraction of the solar gravitational acceleration. The jet consists of
  fine threads (0farcs5-2” wide), which exhibit coherent, oscillatory
  transverse motions perpendicular to the jet axis and about a common
  equilibrium position. These motions propagate upward along the jet,
  with the maximum phase speed of 744 ± 11 km\nolimits s\nolimits ^{-1}
  at the leading front of the jet. The transverse oscillation velocities
  range from 151 to 26 km\nolimits s\nolimits ^{-1}, amplitudes from
  6.0 to 1.9 Mm\nolimits, and periods from 250 to 536 s\nolimits. The
  oscillations slow down with time and cease when the material starts to
  fall back. The falling material travels along almost straight lines in
  the original direction of ascent, showing no transverse motions. These
  observations are consistent with the scenario that the jet involves
  untwisting helical threads, which rotate about the axis of a single
  large cylinder and shed magnetic helicity into the upper atmosphere.

---------------------------------------------------------
Title: Electric and magnetic field observations of Pc4 and Pc5
pulsations in the inner magnetosphere: A statistical study
Authors: Liu, W.; Sarris, T. E.; Li, X.; Elkington, S. R.; Ergun,
   R.; Angelopoulos, V.; Bonnell, J.; Glassmeier, K. H.
2009JGRA..11412206L    Altcode:
  Ultralow frequency (ULF) waves in the Pc4 and Pc5 bands are ubiquitous
  in the inner magnetosphere and have significant influence on energetic
  particle transport. Investigating the source and characteristics of
  ULF waves also helps us better understand the interaction processes
  between the solar wind and the magnetosphere. However, owing to the
  limitation in instrumentation and spatial coverage, the distribution
  of ULF waves in local time and L shell in the inner magnetosphere has
  not been completely studied. The recent Time History of Events and
  Macroscale Interactions During Substorms (THEMIS) mission provides
  unique opportunities to investigate the spatial distribution of ULF
  pulsations across different L shells with full local time coverage in
  the inner magnetosphere during solar minimum, with both electric and
  magnetic field measurements. Pc4 and Pc5 pulsations in the electric
  field observations are identified throughout 13 months of measurements,
  covering 24 h in local time. The pulsations are characterized as either
  toroidal or poloidal (including compressional) mode, depending on
  the polarization of the electric field. Subsequently, the pulsations'
  occurrence rate and wave power distributions in radial distance and
  local time are recorded. While the distributions of both Pc4 and Pc5
  events vary greatly with radial distance and local time, Pc4 events are
  more frequently observed in the inner region around 5-6 R<SUB>E</SUB>
  and Pc5 events are more frequently observed in the outer region around
  7-9 R<SUB>E</SUB>, which suggests that the field line resonance is
  an important source of the ULF waves. In the flank regions, the wave
  power is dominated by the toroidal mode, likely associated with the
  Kelvin-Helmholtz (KH) instability. In the noon sector, the Pc5 ULF
  wave power is dominated by the poloidal mode, likely associated with
  the solar wind dynamic pressure disturbance. The KH instability plays
  an important role, suggested by our observations, during the solar
  minimum when the solar wind dynamic pressure is relatively weak. We
  also find that the contributions to the Pc5 ULF wave power from the
  external sources are larger than the contributions from the internal
  sources. These statistical results are important in characterizing
  Pc4 and Pc5 waves and also important for any efforts to model the
  transport of energetic particles in the magnetosphere.

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Title: PFSIR observations of equatorward-expanding ionospheric
    F-region patch and its association with the flow and auroral
    activities
Authors: Liang, J.; Spanswick, E. L.; Nicolls, M. J.; Donovan, E. F.;
   Lummerzheim, D.; Liu, W.
2009AGUFMSM53D..08L    Altcode:
  We present an event study with conjunctive THEMIS and PFISR observations
  on March 3, 2009, 10-12 UT. During this event interval mid-tail probe
  THEMIS-C detected a series of fast earthward flows. Correspondingly,
  ground-based optical observations revealed strong red-line (630nm)
  emission intensifications and equatorward-moving auroral structures,
  but they were not accompanied by a substorm expansion. Using the
  Poker Flat incoherent radar (PFISR) observations we are able to
  fully explore the 4-D (time, latitude, longitude, and altitude)
  properties of the ionospheric electron density profile for this
  event. We found that localized density enhancements (patches) appeared
  with the start of the flow and auroral activities, and then expanded
  progressively equatorward. The patches were limited within roughly
  the same latitudinal/latitudinal range of a moving auroral arc,
  and existed dominantly in F-region (~150-300 km), suggesting that
  the precipitating particles generating the patches were relatively
  soft in energy (&lt;1keV), similar to that responsible for the
  red-line auroral emissions. More interestingly, when the patches
  extended further equatorward they were substantially elevated in
  altitudes. Synthesizing all observations we discuss the possible
  particle sources and mechanisms, both magnetospheric and ionospheric,
  that lead to the of the observed F-region patch dynamics.

---------------------------------------------------------
Title: Solar wind influence on Pc4 and Pc5 ULF wave activity in the
    inner magnetosphere
Authors: Liu, W.; Sarris, T. E.; Li, X.; Ergun, R. E.; Angelopoulos,
   V.; Bonnell, J. W.; Glassmeier, K.
2009AGUFMSM11A1569L    Altcode:
  Abundant evidences have previously been shown that the ULF wave
  activities measured at geosynchronous orbit are well correlated with
  solar wind parameters, such as solar wind dynamic pressure. However,
  these studies, based only magnetic field measurements near the
  equatorial plane, cannot determine the actual ULF wave power
  because magnetic field oscillation in torodial mode has a node
  at the equator. In this study, we use both electric and magnetic
  field measurements by THEMIS satellites in the inner magnetosphere
  to statistically examine the correlation between the overall
  ULF wave activities in the inner magnetosphere and the solar wind
  parameters. Based on the electric field observations from July 2007 to
  May 2009, a strong correlation has been found between the daily averaged
  integral Pc4&amp;5 wave power in 4~9 Re and the solar wind velocity;
  the correlation with solar wind dynamic pressure is not as obvious. The
  THEMIS magnetic field measurements show that the correlation coefficient
  decreases with solar velocity but increases with dynamic pressure, in
  contrast to the results based on the electric field measurements. We
  suggest that the difference is due to the detection of different
  ULF mode pulsations (toridal and poloidal) and that electric field
  measurements near the equator are critical to investigate Pc4 and Pc5
  ULF wave activities.

---------------------------------------------------------
Title: Low-frequency waves in auroral arcs: optical echo of
    magnetotail dynamics (Invited)
Authors: Uritsky, V. M.; Liang, J.; Donovan, E. F.; Spanswick, E. L.;
   Knudsen, D. J.; Liu, W.
2009AGUFMSM52B..03U    Altcode:
  We report new results of our analysis of longitudinally propagating
  low-frequency (period 0.5 - 2.0 min) wave oscillations in optical
  auroral arcs, with the emphasis on the underlying physics. Several
  alternative wave mechanisms are considered, including a variety of
  wave modes in the ionosphere and the auroral acceleration region,
  field line resonances, and plasma waves in the magnetotail. A
  representative set of well-documented episodes of wave activity
  recorded by ground-based and in situ THEMIS instruments is studied
  in this context. Our analysis rules out three of the four wave
  locations listed above. The ionospheric origin of the arc wave is
  unlikely considering the measured phase velocities which require
  unrealistically strong convection electric fields. The acceleration
  region is able to produce fast-traveling localized auroral features
  such as folds and rays, but not for the observed range of wavelengths
  (up to ~400 km in the ionospheric frame), and not for the observed
  propagation direction (predominantly westward at both southern
  and northern edges of pre-midnight arcs). It is noteworthy that the
  majority of wave events are not accompanied by field line resonances,
  indicating that this effect is not the primary cause of the arc wave,
  contrary to some recent claims. The only interpretation consistent
  with our quantitative analysis of the relevant data tests is that the
  arc waves are a manifestation of an azimuthally propagating wave in
  the magnetotail. We present several examples of a nearly one-to-one
  correspondence between low-frequency tail waves (e.g. flapping motion)
  and the auroral arc waves, the parameters of the optical wave being
  consistent with theoretical predictions for drift wave oscillations in
  a thin current sheet. Although the detailed physical picture of the
  underlying magnetosphere -ionosphere interaction is still lacking,
  our results strongly suggest that further investigation of optical
  arc waves will provide a valuable piece of information on spatial
  propagation of plasma instabilities associated with substorm growth and
  expansion phases as well as other magnetospheric conditions. Detrended
  ewogram representation (MLON vs UT, color-coded optical intensity)
  of a longitudinally propagating arc wave prior to 8:04 03/03/08
  substorm onset observed by the Fort Simpson ASI. Parameters of several
  representative pre-onset arc wave events. Letters N and S correspond to
  northern and southern arcs in double-arc systems. Numbers in brackets
  are expected magnetotail values from T89 mapping.

---------------------------------------------------------
Title: Fine Structures and Kinematics of an Intriguing Chromospheric
    Jet Observed by Hinode Solar Optical Telescope
Authors: Liu, W.; Berger, T. E.; Title, A. M.; Tarbell, T. D.
2009AGUFMSH51A1266L    Altcode:
  Transient, small-scale ejections of plasma from the lower atmosphere
  are common manifestations of solar activity. Hinode, with its superior
  resolutions, has spurred renewed interest in solar jets since its
  launch. Here we report a chromospheric jet lasting for more than 1
  hr on 2007 February 9 observed by the Hinode Solar Optical Telescope
  (SOT) in unprecedented detail. SOT Ca II H passband observations
  at high resolution of 0.2 arcsecond and cadence of 8 s allowed us to
  investigate the fine structures and kinematics of the jet. The ejection
  occurred in three episodes, rather than continuously, with the amount
  and velocity of material decreasing with time. The upward velocities
  along the jet range from ~440 to ~30 km/s, while the downward velocities
  of the material falling back have much smaller values (mean: -60 km/s)
  and a narrower distribution. Some tracks in the space-time plot clearly
  show parabolic shapes and the inferred acceleration is a fraction of
  the solar gravitational acceleration. The jet consists of fine threads
  (0.5-2 arcsecond wide), which exhibit coherent, oscillatory transverse
  motions perpendicular to the jet axis and about a common equilibrium
  position. These motions propagate upward, with the maximum phase speed
  of ~740 km/s found at the leading front of the jet. The transverse
  oscillation velocities range from 150 to 30 km/s, amplitudes from 6 to 2
  Mm, and periods from 250 to 550 s. The oscillations slow down with time
  and cease when the material starts to fall back. The falling material
  travels along almost straight lines in the original direction of ascent,
  showing no transverse motions. These observations are consistent with
  the models suggested by Shibata &amp; Uchida (1985) and Canfield et
  al. (1996). In this scenario, the jet involves untwisting helical
  threads, which rotate about the axis of a single large cylinder and
  shed magnetic helicity into the upper atmosphere. Implications of this
  event in the context of multiwavelength data in H-alpha, EUV, and X-rays
  will be discussed. A chromospheric jet observed by Hinode SOT in the
  Ca II H passband (T=1-2×10 4 K). Note the helical-like fine threads.

---------------------------------------------------------
Title: When the rubber hits the road: turbulence and intermittencies
    in Earth’s magnetosphere (Invited)
Authors: Liu, W.; Uritsky, V. M.; Charbonneau, P.; Valliere-Nollet,
   M.; Morales, L. F.
2009AGUFMSM41C..02L    Altcode:
  The theory of MHD turbulence has a long history of development, but its
  application to actual physical systems has not been as widespread as
  the omnipresence of turbulent phenomena in these systems. The reasons
  can be many. For example, the geometry, constitution, coupling, and
  boundary conditions in an actual system may place it well beyond the
  limit of the current theory. Or our measurement capability has not
  progressed to the point that the salient theoretical predictions
  can be reliably tested. In our view, however, the most pertinent
  reason is the specialist’s unfamiliarity with and reluctance to
  use the ‘generalist’ approach of complexity and turbulence, and
  the generalist’s lack of attention to the particulars of specific
  systems. Clearly, a closer dialogue between the two communities holds
  significant promise for further advances. In this talk, complexity
  and turbulence observed in Earth’s magnetosphere are reviewed. A
  distinguishing characteristic of magnetospheric processes is strong
  intermittency in global episodes and ever-present turbulence on
  local scales. We explore the suggestion that avalanches of localized
  turbulence are responsible for global dynamics. Some new theoretical
  advances in elaborating this concept are discussed.

---------------------------------------------------------
Title: Go With the Flow: The Reductionist View of Geospace at the
    System Level (Invited)
Authors: Liemohn, M. W.; Brandt, P. C.; Denton, M. H.; Donovan, E. F.;
   Frey, H. U.; Lester, M.; Liu, W.; Milan, S. E.; Ostgaard, N.; Palmroth,
   M. M.; Ridley, A. J.; Uritsky, V. M.; Zhang, X.
2009AGUFMSM11D..02L    Altcode:
  A typical approach to understanding geospace is to solve the
  first-principles equations for the motion of particles and for the
  electric and magnetic fields within the region of interest. This is the
  reductionist approach to space physics and has been the primary (and
  highly successful) methodology of our field for many decades. When only
  a small part of geospace of being investigated, then the researcher
  must assume boundary conditions for those plasma and field regions
  not being solved by the equation set. For many problems, this is
  entirely acceptable and such an approach has delivered excellent
  scientific results that have significantly advanced understanding of
  geospace. For some problems, though, this boundary condition approach is
  insufficient. That is, the population or region of interest can modify
  the boundary conditions through some system-level feedback mechanism
  of geospace. These feedbacks invariably relate to the flow of mass and
  energy through the system. The simplified regional model is no longer
  adequate for this problem and a larger-scale system-level approach
  is warranted. This presentation discusses a number of system-level
  problems that require full tracking of these mass and energy flows
  through the geospace system. This reductionist view of system-level
  science is then compared with analysis of emergent phenomena and the
  study of the geospace system’s natural complexity. The presentation
  concludes with ideas of how these two views of system-level science
  could, and in many ways should, be used together.

---------------------------------------------------------
Title: Combined Fokker-Planck Modeling of Particle
    Acceleration/Transport and Hydrodynamic Simulation of Atmospheric
    Response in Solar Flares
Authors: Petrosian, V.; Liu, W.; Mariska, J. T.
2009AGUFMSH21C..04P    Altcode:
  Acceleration and transport of high-energy particles and fluid dynamics
  of atmospheric plasma are interrelated aspects of solar flares, but for
  simplicity they were artificially separated in the past. We present
  here self-consistently combined Fokker-Planck modeling of particles
  and hydrodynamic simulation of flare plasma. Energetic electrons are
  modeled with the Stanford unified code of acceleration, transport,
  and radiation, while plasma is modeled with the NRL flux tube code
  (Mariska et al. 1989). We calculated the collisional heating rate
  directly from the particle transport code, which is more accurate
  than those in previous studies based on approximate analytical
  solutions. We used a more realistic spectrum of injected electrons
  provided by the stochastic acceleration model of Petrosian &amp; Liu
  (2004), which has a smooth transition from a quasi-thermal background
  at low energies to a nonthermal tail at high energies. The inclusion of
  low-energy electrons results in relatively more heating in the corona
  (vs. chromosphere) and thus a larger downward heat conduction flux. The
  interplay of electron heating, conduction, and radiative loss leads to
  stronger chromospheric evaporation than obtained in previous studies,
  which had a deficit in low-energy electrons due to an arbitrarily
  assumed low-energy cutoff. The energy and spatial distributions of
  energetic electrons and bremsstrahlung photons bear signatures of the
  changing density distribution caused by chromospheric evaporation. In
  particular, the density jump at the evaporation front gives rise to
  enhanced X-ray emission, which could be responsible for the X-ray
  sources moving along flare loops observed by RHESSI (Sui et al. 2006,
  ApJL 645; Liu et al. 2006, ApJ 649). Various energy contents from the
  simulations can be used to test the empirical Neupert effect. This
  technique can also be applied to investigate a variety of high-energy
  processes in solar, space, and astrophysical plasmas, such as planetary
  auroras. Geometry of the model flare loop assumed in this study.

---------------------------------------------------------
Title: An Active Auroral Streamer And The Concurrent Magnetotail
    Activity
Authors: Lui, A.; Spanswick, E. L.; Donovan, E. F.; Liang, J.; Liu,
   W.; Uritsky, V. M.; McFadden, J. P.; Larson, D. E.
2009AGUFMSM53D..02L    Altcode:
  We report the observations of an active auroral streamer and the
  concurrent activity in the magnetotail monitored by the five THEMIS
  satellites. The auroral streamer was a low intensity feature obtained
  by the Rankin Inlet EMCCD ASI. It emerged from the diffuse aurora,
  advancing poleward and then retreating equatorward. This occurred during
  a major THEMIS tail conjunction period and the ground projections of
  THEMIS satellites were near the MLT of the auroral streamer. During
  this interval, tailward plasma flows were observed by the five THEMIS
  satellites, followed by earthward plasma flows by four of them. These
  plasma flows were mostly field-aligned and had low speeds of 40-100
  km/s. The possible connection between the ground auroral activity and
  the magnetotail activity will be discussed

---------------------------------------------------------
Title: THEMIS Observations of Field Line Resonance Excitation in
    Responce to a Solar Wind Pressure Pulse
Authors: Sarris, T. E.; Liu, W.; Li, X.; Kabin, K.; Angelopoulos,
   V.; Bonnell, J. W.; Glassmeier, K.
2009AGUFMSM31B1534S    Altcode:
  The THEMIS multi-probe mission performs electric and magnetic field
  measurements with identical instrumentation at different locations,
  providing unique opportunities to differentiate between temporal and
  spatial characteristics of Field Line Resonances (FLRs) and to identify
  their extent in the Earth magnetosphere. In the case study presented,
  narrow-band FLRs are observed to be excited globally at different
  frequencies that match the local field line resonant frequency; for
  one instance where the intensification of the FLR power coincides
  with a solar wind pressure pulse, we are able to conclusively and
  definitively identify the excitation mechanism, and we thus consider
  this instance to be a proof that FLRs can be excited globally at the
  local FLR frequency by a solar wind pressure pulse.

---------------------------------------------------------
Title: Using Optical and Riometer Observations to Study the
    Relationship Between the Spatio-temporal Evolution of Magnetic Field
    Topology and Dispersionless Electron Injection
Authors: Donovan, E.; Spanswick, E.; Liang, J.; Jackel, B. J.; Liu,
   W.; Kabin, K.; Rankin, R.
2009AGUFMSM41A1680D    Altcode:
  In an electron injection, inner central plasma sheet fluxes of energetic
  electrons increase dramatically around the time of a substorm expansion
  phase onset. If the injection is dispersionless, then the increase is
  simultaneous across a broad range of energies. It is widely accepted
  that the Dispersionless Injection (DI) is observed in the region of
  space and at the time of the dipolarization. Recent observational
  studies of various signatures of DI and other onset related phenomena
  have led to a number of conclusions about the spatio-temporal evolution
  of DI. These include the fact that DI begins on field lines threading
  the transition region between dipolar and stretched magnetic field
  topologies and subsequently expands both tailward and earthward, and
  that DI begins in a radially narrow and azimuthally extended region. In
  this paper, we present observations of proton and electron aurora,
  riometer absorption, and in situ high-energy electron fluxes, all from
  the minutes around substorm expansion phase onset. We describe how
  these observations corroborate the idea that DI begins in the region
  of transition between dipolar and tail-like topologies, and further
  how they support the hypothesis that in the last few minutes of the
  growth phase the transition region is radially narrow, that after
  onset the narrow transition retreats tailward, and that this retreat
  is the tailward expansion of the DI. We assert that these results set
  the quantitative stage for numerical simulations that can be used to
  explore the physical mechanism responsible for DI.

---------------------------------------------------------
Title: How well can satellite data characterize the water cycle of
    the Madden-Julian Oscillation?
Authors: Waliser, Duane E.; Tian, Baijun; Xie, Xiaosu; Liu, W. Timothy;
   Schwartz, Michael J.; Fetzer, Eric J.
2009GeoRL..3621803W    Altcode:
  Most characterizations of the Madden-Julian Oscillation (MJO) have
  focused on its convection and circulation features, ocean interactions,
  and weather and climate impacts. The water cycle of the MJO has
  yet to be examined or quantified despite it offering an additional
  constraint on model representations of the MJO, which are still woefully
  poor. Recent satellite products now make it possible to characterize the
  MJO water cycle from observations. These include water vapor profiles,
  column water vapor, cloud ice profiles, total cloud liquid, rainfall,
  surface evaporation and column moisture convergence. From these,
  we quantify the water budget for disturbed and suppressed phases of
  the MJO. The column-integrated results indicate that precipitation is
  nearly balanced with moisture convergence, with variations in surface
  evaporation being an order of magnitude smaller. However, residuals
  in the column-integrated budget are relatively large, indicating the
  need for improved satellite retrievals and/or the necessity of using
  model-based assimilation products.

---------------------------------------------------------
Title: Longitudinally propagating arc wave in the pre-onset optical
    aurora
Authors: Uritsky, V. M.; Liang, J.; Donovan, E.; Spanswick, E.;
   Knudsen, D.; Liu, W.; Bonnell, J.; Glassmeier, K. H.
2009GeoRL..3621103U    Altcode:
  We present the first systematic observational evidence for a traveling
  periodic structure in the pre-onset optical aurora - the longitudinally
  propagating arc wave (LPAW) - associated with flapping oscillations
  in the magnetotail. The LPAW is characterized by azimuthally
  moving intensity enhancements inside auroral arcs as seen by THEMIS
  ground-based all-sky imagers. It travels westward in the pre-midnight
  auroral sector during the 10-20 minutes preceding auroral breakup with
  a velocity of 2-10 km/s, time period 40-110 s, and wavelength 250-420
  km. Magnetically conjugate measurements by THEMIS satellites show low
  frequency plasma oscillations consistent with the parameters of the arc
  wave in the course of current sheet thinning. When mapped into tail,
  wavelength (4800-9400 km) and velocity (70-190 km/s) of the LPAW are
  compatible with observations and theoretical predictions for current
  sheet flapping motions. Our results strongly suggest that LPAW is an
  auroral footprint of the drift wave mode (kink, sausage, ballooning,
  etc.) in a stretched magnetotail.

---------------------------------------------------------
Title: 3D Magnetic Reconnection of Relativistic Pair Plasmas
Authors: Liu, Wei; Yin, Lin; Albright, Brian; Bowers, Kevin; Li, Hui;
   Liang, Edison
2009APS..DPPNM9008L    Altcode:
  Relativistic plasma physics plays an essential role in a number of
  famous and longstanding astrophysical problems. Using the ultrafast
  code VPIC, we present one of the largest scale 3D particle-in-cell
  (PIC) simulations to date to examine relativistic magnetic reconnection
  in pair plasmas. These simulations are large enough to accommodate a
  sufficient number of kink modes. It is demonstrated that multiple,
  patchy reconnection sites form during the initial stage and then
  self-organize to form an elongated diffusion region with increased
  system size. The secondary kinking folds the current sheet in the
  orthogonal direction. The interaction between kink and tearing
  instabilities results in plasmoids, which affect the particle
  acceleration and reconnection rate. The reconnection rate remains fast
  and time varying. The relativistic effects increase the linear kink mode
  wavelengths and results in almost identical growth rates for initial
  linear kink and tearing modes. Relativistic drift kink instability,
  reconnection, folding of the diffusion region due to the secondary
  kink and plasmoids all contribute to the particle energization.

---------------------------------------------------------
Title: Long Term Evolution of Magnetized Bubbles in Galaxy Clusters
Authors: Liu, Wei; Li, Hui; Hsu, Scott; Li, Shengtai
2009APS..DPPXP8023L    Altcode:
  We have performed nonlinear ideal MHD simulations of the long term
  evolution of a magnetized low-density “bubble” plasma formed by
  a radio galaxy in a stratified cluster medium. It is found that
  about 3.5% of the initial magnetic energy remains in the bubble
  after 8 billion years, and the initial magnetic bubble expansion is
  adiabatic. The bubble can survive for at least 8 billion years due to
  the stabilizing effect of the bubble magnetic field on Rayleigh-Taylor
  and Kelvin-Holmholtz instabilities, possibly accounting for “ghost
  cavities” as observed in Perseus-A. A filament structure spanning
  about 500 kpc is formed along the path of bubble motion. The mean value
  of the magnetic field inside this structure is 0.88 micro Gauss at 8
  billion years. Finally, the initial bubble momentum and rotation have
  limited influence on the long term evolution of the bubble.

---------------------------------------------------------
Title: Ion temperature drop and quasi-electrostatic electric field
    at the current sheet boundary minutes prior to the local current
    disruption
Authors: Liang, Jun; Liu, W. W.; Donovan, E. F.
2009JGRA..11410215L    Altcode:
  From a survey of the cross-tail current disruption (CD) events in the
  near-Earth plasma sheet collected from the Time History of Events and
  Macroscale Interactions during Substorms (THEMIS) mission, we identify a
  highly repeatable class of event occurring at the current sheet boundary
  in a few minutes before the local CD onset. Salient features of this
  class of event include (1) a precipitous drop of the ion temperature,
  (2) concurrent growth of a neutral sheet-pointing electric field,
  and (3) ULF wave activations at Pi1/Pi2 bands. We interpret the
  ion temperature drop as a manifestation of the extremely thinning
  of the local current sheet prior to its disruption. This thinning
  process is inferred as nonadiabatic by nature. Particularly, when
  the current sheet thickness is down to ion kinetic scales, the ions
  are demagnetized, and a quasi-electrostatic neutral sheet-pointing
  electric field emerges owing to the charge separation. The ULF
  fluctuations of electric/magnetic field have a two-band structure. The
  lower-frequency band with a period of 50 to 80 s is interpreted as an
  Alfvenic mode coupled from other preonset wave modes excited at the
  equatorial plasma sheet such as the ballooning. The higher-frequency
  wave at 10- to 20-s periods is attributed to some instability mode,
  directly leading to the disruption of the thin current sheet (TCS). We
  suggest that an extremely thinned non-Harris TCS and the emergence of
  quasi-electrostatic field constitute the conducive conditions for a
  local CD to occur. A companion paper by Liu et al. (2009) covers some
  theoretical aspects of this study.

---------------------------------------------------------
Title: Ideal magnetohydrodynamic simulations of low beta compact
    toroid injection into a hot strongly magnetized plasma
Authors: Liu, Wei; Hsu, Scott C.; Li, Hui
2009NucFu..49i5008L    Altcode: 2009arXiv0902.2485L
  We present results from three-dimensional ideal magnetohydrodynamic
  simulations of low β compact toroid (CT) injection into a hot strongly
  magnetized plasma, with the aim of providing insight into CT fuelling of
  a tokamak with parameters relevant for the International Thermonuclear
  Experimental Reactor (ITER). A regime is identified in terms of CT
  injection speed and CT-to-background magnetic field ratio that appears
  promising for precise core fuelling. Shock-dominated regimes, which are
  probably unfavourable for tokamak fuelling, are also identified. The
  CT penetration depth is proportional to the CT injection speed and
  density. The entire CT evolution can be divided into three stages: (1)
  initial penetration, (2) compression in the direction of propagation
  and reconnection with the background magnetic field, and (3) coming to
  rest and spreading in the direction perpendicular to injection. Tilting
  of the CT is not observed due to the fast transit time of the CT across
  the background plasma.

---------------------------------------------------------
Title: Combined Modeling of Acceleration, Transport, and Hydrodynamic
    Response in Solar Flares. I. The Numerical Model
Authors: Liu, Wei; Petrosian, Vahé; Mariska, John T.
2009ApJ...702.1553L    Altcode: 2009arXiv0906.2449L
  Acceleration and transport of high-energy particles and fluid dynamics
  of atmospheric plasma are interrelated aspects of solar flares, but
  for convenience and simplicity they were artificially separated in the
  past. We present here self-consistently combined Fokker-Planck modeling
  of particles and hydrodynamic simulation of flare plasma. Energetic
  electrons are modeled with the Stanford unified code of acceleration,
  transport, and radiation, while plasma is modeled with the Naval
  Research Laboratory flux tube code. We calculated the collisional
  heating rate directly from the particle transport code, which is
  more accurate than those in previous studies based on approximate
  analytical solutions. We repeated the simulation of Mariska et
  al. with an injection of power law, downward-beamed electrons using
  the new heating rate. For this case, a ~10% difference was found from
  their old result. We also used a more realistic spectrum of injected
  electrons provided by the stochastic acceleration model, which has a
  smooth transition from a quasi-thermal background at low energies to a
  nonthermal tail at high energies. The inclusion of low-energy electrons
  results in relatively more heating in the corona (versus chromosphere)
  and thus a larger downward heat conduction flux. The interplay of
  electron heating, conduction, and radiative loss leads to stronger
  chromospheric evaporation than obtained in previous studies, which had a
  deficit in low-energy electrons due to an arbitrarily assumed low-energy
  cutoff. The energy and spatial distributions of energetic electrons
  and bremsstrahlung photons bear signatures of the changing density
  distribution caused by chromospheric evaporation. In particular, the
  density jump at the evaporation front gives rise to enhanced emission,
  which, in principle, can be imaged by X-ray telescopes. This model can
  be applied to investigate a variety of high-energy processes in solar,
  space, and astrophysical plasmas.

---------------------------------------------------------
Title: Copper speciation and partitioning between vapor and liquid
phases in sulphuric solution: An XAS study
Authors: Etschmann, B.; Liu, W.; Brugger, J.; Testemale, D.; Hazemann,
   J. L.; Müller, H.; Proux, O.
2009GeCAS..73R.341E    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Episodic X-Ray Emission Accompanying the Activation of an
Eruptive Prominence: Evidence of Episodic Magnetic Reconnection
Authors: Liu, Wei; Wang, Tong-Jiang; Dennis, Brian R.; Holman,
   Gordon D.
2009ApJ...698..632L    Altcode: 2009arXiv0902.1805L
  We present an X-ray imaging and spectroscopic study of a partially
  occulted (N16W93) C7.7 flare on 2003 April 24 observed by Reuven Ramaty
  High Energy Solar Spectroscopy Imager that accompanied a prominence
  eruption observed by Transition Region and Coronal Explorer. (1) The
  activation and rise of the prominence occurs during the preheating phase
  of the flare. The initial X-ray emission appears as a single coronal
  source at one leg of the prominence and it then splits into a double
  source. Such a source splitting happens three times, each coinciding
  with an increased X-ray flux and plasma temperature, suggestive of fast
  reconnection in a localized current sheet and an enhanced energy-release
  rate. In the late stage of this phase, the prominence displays a helical
  structure. These observations are consistent with the tether-cutting
  and/or kink-instability model for triggering solar eruptions. (2)
  The eruption of the prominence takes place during the flare impulsive
  phase. Since then, there appear signatures predicted by the classical
  model of two-ribbon flares occurring in a vertical current sheet
  trailing an eruption. These signatures include an extreme-ultraviolet
  (EUV) cusp and current-sheet-like feature (or ridge) above it. There is
  also X-ray emission along the EUV ridge both below and above the cusp,
  which in both regions appears closer to the cusp at higher energies
  in the thermal regime (lsim20 keV). This trend is reversed in the
  nonthermal regime. (3) Spectral analysis indicates thermal X-rays
  from all sources throughout the flare, while during the impulsive
  phase there is additional nonthermal emission which primarily comes
  from the coronal source below the cusp. This source also has a lower
  temperature (T = 20 ± 1 vs. 25 ± 1 MK), a higher emission measure (EM
  = (3.3 ± 0.4) vs. (1.2 ± 0.4) × 10<SUP>47</SUP> cm<SUP>-3</SUP>),
  and a harder nonthermal spectrum (electron power-law index δ = 5.4
  ± 0.4 vs. 8 ± 1) than the upper sources.

---------------------------------------------------------
Title: Monitoring Traveling Magnetospheric Waves In Optical Aurora
Authors: Uritsky, V.; Liang, J.; Donovan, E.; Spanswick, E.; Mende,
   S.; Liu, W.
2009AGUSMSM22A..01U    Altcode:
  The network of THEMIS all-sky imagers provides an unprecedented
  opportunity of studying time evolution of multiscale auroral
  disturbances associated with the magnetospheric substorm onset. In
  this talk, we report our recent results suggesting a possibility of
  direct optical monitoring of propagating low-frequency magnetotail
  disturbances associated with pre- and post-onset conditions. The results
  show a significant enhancement of spatial and temporal coherence of
  the growth phase aurora accompanied by increased ambipolar electric
  field fluctuations in the tail signaling a formation of a thin current
  sheet about ∼5 minutes prior to the main auroral breakup. During
  this time, growth phase arcs reveal various forms of azimuthal plasma
  motion including multiscale turbulence and westward propagating waves
  with traveling speeds of 2.0 -- 5.0 km/s. The post-breakup auroral
  dynamics exhibits wave-like forms which typically travel duskward at
  the velocity 8.0 -- 12.0 km/s, recurrence time 20 -- 30 s. These waves
  first appear within a local pre-midnight sector (∼1 hour MLT wide)
  shortly before to the global expansion onset, and they can be reliably
  detected during the first 10+ minutes following the breakup. The
  analysis of simultaneous in situ THEMIS measurements suggests that
  the observed pre-onset wave patterns can be an auroral footprint of
  flapping oscillations and/or other drift wave modes in the magnetotail
  which can arguably be related to the development of the initial plasma
  instability triggering the substorm onset.

---------------------------------------------------------
Title: Ideal Magnetohydrodynamic Simulations of Magnetic Bubble
    Expansion as a Model for Extragalactic Radio Lobes
Authors: Liu, Wei; Hsu, Scott; Li, Hui; Li, Shengtai; Lynn, Alan
2009APS..APR.K1013L    Altcode:
  Recent astronomical observations indicate that radio lobes are gigantic
  relaxed magnetized plasmas with kilo-to-megaparsec scale jets providing
  a source of magnetic energy from the galaxy to the lobes. Therefore
  we are conducting a laboratory plasma experiment, the Plasma Bubble
  Expansion Experiment (PBEX) in which a higher pressure magnetized plasma
  bubble (i.e., the lobe) is injected into a lower pressure background
  plasma (i.e., the intergalactic medium) to study key nonlinear plasma
  physics issues. Here we present detailed ideal magnetohydrodynamic
  (MHD) three-dimensional simulations of PBEX. First, the direction of
  bubble expansion depends on the ratio of the bubble toroidal to poloidal
  magnetic field, with a higher ratio leading to expansion predominantly
  in the direction of propagation and a lower ratio leading to expansion
  predominantly normal to the direction of propagation. Second, a
  leading MHD shock and a trailing slow-mode compressible MHD wave front
  are formed ahead of the bubble as it propagates into the background
  plasma. Third, the bubble expansion and propagation develop asymmetries
  about its propagation axis due to reconnection arising from numerical
  resistivity and to inhomogeneous angular momentum transport due to the
  background magnetic field. These results will help guide the initial
  experiments and diagnostic measurements on PBEX.

---------------------------------------------------------
Title: Elasticity of (Mg <SUB>0.87</SUB>Fe <SUB>0.13</SUB>)
    <SUB>2</SUB>SiO <SUB>4</SUB> wadsleyite to 12 GPa and 1073 K
Authors: Liu, Wei; Kung, Jennifer; Li, Baosheng; Nishiyama, Nori;
   Wang, Yanbin
2009PEPI..174...98L    Altcode:
  Elasticity of (Mg <SUB>0.87</SUB>Fe <SUB>0.13</SUB>) <SUB>2</SUB>SiO
  <SUB>4</SUB> wadsleyite has been measured at simultaneous high
  pressure and high temperature to 12 GPa and 1073 K using ultrasonic
  interferometry in conjunction with synchrotron X-radiation. The elastic
  moduli and their pressure and temperature derivatives are precisely
  determined using pressure-standard-free third-order and fourth-order
  finite strain equations. Combined with previous thermoelastic data
  on olivine, the density, velocity and acoustic impedance contrasts
  between α- and β-(Mg <SUB>0.9</SUB>Fe <SUB>0.1</SUB>) <SUB>2</SUB>SiO
  <SUB>4</SUB> at 410-km depth are calculated along a 1673 K adiabatic
  geotherm. Both the third- and fourth-order finite strain equation
  fitting results give estimation of ∼33-58% olivine content in the
  upper mantle to account for a seismic discontinuity of ∼5% velocity
  jumps, and 8.5% ( P wave) and 11.1% ( S wave) impedance jumps at 410
  km depth.

---------------------------------------------------------
Title: Helicity Transfer and Energy Release in the Bastille Day Flare
Authors: Hill, Nicholas; Kazachenko, M.; Liu, W.; Qiu, J.
2009SPD....40.2011H    Altcode:
  Spatial and temporal analysis of the 2000 Bastille Day event
  observed with SOHO and TRACE instrumentation is viewed in light of a
  three-dimensional topological reconnection model. The model measures
  the injection of helicity into the active region in a 36-hour build-up
  to the flare as well as the evolution of connected segmented areas of
  the active region to calculate flux available for the reconnection
  process. Utilizing the spatial evolution of the flare, the model
  predicts a reconnection flux of 9.45 x 10<SUP>21</SUP> Mx and a
  helicity transfer of -9.3 x 10<SUP>42</SUP> Mx<SUP>2</SUP> into a
  twisted flux rope subsequently ejected as a coronal mass ejection
  (CME). The results compare well with the flux swept out by the two
  flare ribbons (1.44 x 10<SUP>22</SUP> Mx) as viewed in TRACE 1600Å
  images and the helicity in magnetic cloud measurements (-15.0 x
  10<SUP>42</SUP> Mx<SUP>2</SUP>). Further analyses also reveal spatial
  and temporal correlation between reconnection rate and X-ray emissions,
  yielding evidence that reconnection governs energy release in flares. <P
  />This work was accomplished during the Solar REU program at Montana
  State University, which is in part supported by the National Science
  Foundation through contract ATM-0552958.

---------------------------------------------------------
Title: Unshearing Motions, Asymmetries, and Correlations of Conjugate
Hard X-ray Footpoints in the 2003 October 29 X10 Flare: an Imaging
    Spectroscopic Study
Authors: Liu, Wei; Petrosian, V.; Dennis, B. R.; Holman, G. D.
2009SPD....40.1916L    Altcode:
  We present a detailed imaging spectroscopic study of the conjugate hard
  X-ray (HXR) footpoints (FPs) observed with RHESSI in the 2003 October
  29 X10 flare. (1) The double FPs first move toward and then away from
  each other, mainly parallel and perpendicular to the magnetic neutral
  line, respectively. The transition of these two phases of FP unshearing
  motions coincides with the direction reversal of the motion of the
  loop-top (LT) source, and with the minima of the estimated loop length
  and LT height. (2) Asymmetries are observed between the FPs: on average,
  the eastern FP is 2.2 times brighter in HXR flux and 1.8 times weaker
  in magnetic field strength, and moves 2.8 times faster away from the
  neutral line than the western FP; the estimated coronal column density
  to the eastern FP from the LT source is 1.7 times smaller. The two FPs
  have marginally different spectral indexes. The eastern-to-western FP
  HXR flux ratio and magnetic field ratio are anti-correlated only before
  the second HXR peak's maximum. Neither magnetic mirroring nor column
  density alone can explain these observations when taken together,
  but their combination, along with other transport effects (e.g.,
  non-uniform target ionization, relativistic beaming, photospheric
  albedo, and return currents), might provide a full explanation. (3) The
  FPs show temporal correlations between the HXR flux, spectral index,
  and magnetic field strength. The HXR flux exponentially correlates
  with the magnetic field strength which also anti-correlates with
  the spectral index before the second HXR peak's maximum, suggesting
  that particle acceleration sensitively depends on the magnetic field
  strength and/or reconnection rate. (4) We have also developed novel
  techniques to remove particle contamination from HXR counts and to
  estimate effects of pulse pileup in imaging spectroscopy, which can
  be applied to other RHESSI flares in similar circumstances.

---------------------------------------------------------
Title: Long-Term Evolution of Magnetized Bubbles in Galaxy Clusters
Authors: Liu, Wei; Li, Hui; Li, Shengtai; Hsu, Scott
2009APS..APR.K1012L    Altcode:
  An unsolved problem in active galactic nuclei (AGN) feedback on
  clusters is how to account for the the morphology and stability of
  buoyant bubbles and their interactions with the ambient intracluster
  medium (ICM). Appreciable magnetic energy has been observed in both
  cluster and radio lobe plasmas. We have performed nonlinear ideal
  magnetohydrodynamic simulations of the long term evolution of a
  magnetized low-density “bubble” plasma formed by a radio galaxy
  in a stratified cluster medium. It is found that about 3.5% of the
  initial magnetic energy remains in the bubble after ∼8 x10^9 years,
  and the initial magnetic bubble expansion is adiabatic. The bubble
  can survive for at least 8x10^9 years due to the stabilizing effect
  of the bubble magnetic field on Rayleigh-Taylor and Kelvin-Holmholtz
  instabilities, possibly accounting for “ghost cavities" as observed
  in Perseus-A. A filament structure spanning about 500 kpc is formed
  along the path of bubble motion. The mean value of the magnetic field
  inside this structure is ∼0.88 μG at ∼8x10^9 years. Finally,
  the initial bubble momentum and rotation have limited influence on
  the long term evolution of the bubble.

---------------------------------------------------------
Title: Episodic X-ray Emission Accompanying the Activation of an
Eruptive Prominence: Evidence of Episodic Magnetic Reconnection
Authors: Liu, Wei; Wang, T.; Dennis, B. R.; Holman, G. D.
2009SPD....40.1911L    Altcode:
  We present an X-ray imaging and spectroscopic study of a partially
  occulted (N16W93) C7.7 flare on 2003 April 24 observed by RHESSI that
  accompanied a prominence eruption observed by TRACE. (1) The activation
  and rise of the prominence occurs during the preheating phase of
  the flare. The initial X-ray emission appears as a single coronal
  source at one leg of the prominence and it then splits into a double
  source. Such a source splitting happens three times, each coinciding
  with an increased X-ray flux and plasma temperature, suggestive
  of fast reconnection in a localized current sheet and an enhanced
  energy release rate. In the late stage of this phase, the prominence
  displays a helical structure. These observations are consistent with
  the tether-cutting and/or kink instability model for triggering solar
  eruptions. (2) The eruption of the prominence takes place during the
  flare impulsive phase. Since then, there appear signatures predicted by
  the classical CSHKP model of two-ribbon flares occurring in a vertical
  current sheet trailing an eruption. These signatures include an EUV
  cusp and current-sheet-like feature (or ridge) above it. There is also
  X-ray emission along the EUV ridge both below and above the cusp, which
  in both regions appears closer to the cusp at higher energies in the
  thermal regime (&lt;20 keV). This trend is reversed in the nonthermal
  regime (&gt;20 keV). (3) Spectral analysis indicates thermal X-rays
  from all sources throughout the flare, while during the impulsive phase
  there is additional nonthermal emission which primarily comes from the
  coronal source below the cusp. This source also has a lower temperature
  (T=20±1 vs. 25±1 MK), a higher emission measure (EM=[3.3±0.4]
  vs. [1.2±0.4] x10<SUP>47 </SUP>cm<SUP>-3</SUP>), and a much harder
  nonthermal spectrum (electron power-law index \delta=5.4±0.4 vs. 8±1)
  than the upper sources.

---------------------------------------------------------
Title: Coexistence of distinct power-law regimes in Self Organized
    Model for the Magnetosphere
Authors: Vallieres-Nollet, M.; Charbonneau, P.; Uritsky, V.; Liu, W.
2009AGUSMSM22A..06V    Altcode:
  It is now argued that the Central Pasma Sheet (CPS) may behave like a
  Self-Organized Critical (SOC) system, driven by the the solar wind. The
  power law distributions for the sizes, energy and durations of substorms
  that are reflected in observations can be reproduced using such SOC
  models. However, recent observations made with the POLAR-UVI instrument
  showed that there is in fact two distinct regimes in substorms energies
  : small and big events scales as different power laws, the smaller
  events having a steeper slope. We used a 2D-SOC model subject to a
  deterministic driving, with conservative redistributions laws. We where
  able, with a slow driving together with a small dissipation in energy
  redistribution, to reproduce the coexistence of these two scaling
  regimes. The computation of the waiting-times, under the imposition
  of a threshold, showed truncated exponentials distributions, which
  is consistent with observations. Finally, we computed statistics
  of substorms depending on their onset position, and found that the
  southward mapping events tends to exhibit the dual power-law scaling,
  while a single slope statistic was found for northward mapping
  substorms, which is again consistent with recent observations.

---------------------------------------------------------
Title: GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS: Reply to the
    “Comment on 'Ported from Self-Similar Analytic Solutions of
    Ginzburg-Landau Equation with Varying Coefficients'"
Authors: Feng, Jie; Xu, Wen-Cheng; Li, Shu-Xian; Liu, Wei-Ci; Liu,
   Song-Hao
2009ChPhL..26e9902F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Magnetic Bubble Expansion as an Experimental Model for
    Extra-Galactic Radio Lobes
Authors: Lynn, Alan; Zhang, Yue; Hsu, Scott; Li, Hui; Liu, Wei;
   Gilmore, Mark; Watts, Christopher
2009APS..APR.K1014L    Altcode:
  The Plasma Bubble Expansion Experiment (PBEX) has begun laboratory
  experiments and coordinated nonlinear MHD simulations to address
  outstanding nonlinear plasma physics issues related to how magnetic
  energy and helicity carried by extra-galactic jets interacts with the
  intergalactic medium to form radio lobe structures. Experiments are
  being conducted in the 4 meter long, 50 cm diameter HELCAT linear plasma
  device at UNM. A pulsed magnetized coaxial gun (∼10 kV, ∼100 kA,
  ∼2 mWb) forms and injects magnetized plasma bubbles perpendicularly
  into a lower pressure weakly magnetized background plasma formed by a
  helicon and/or hot cathode source in HELCAT. Experimental parameters
  can be adjusted so that important dimensionless parameters are relevant
  to the astrophysical context. Ideal MHD simulations show that an MHD
  shock develops ahead of the bubble as it propagates, and that the
  bubble develops asymmetries due to the background field [1]. First
  experimental data from plasma bubble injection into a background
  plasma, including magnetic probe measurements and high-speed camera
  imaging, will be presented. [1] W. Liu et al., Phys. Plasmas 15, 072905
  (2008). Supported by NSF-AST/DOE grant AST-0613577 and LANL LDRD.

---------------------------------------------------------
Title: Conjugate Hard X-Ray Footpoints in the 2003 October 29 X10
Flare: Unshearing Motions, Correlations, and Asymmetries
Authors: Liu, Wei; Petrosian, Vahé; Dennis, Brian R.; Holman,
   Gordon D.
2009ApJ...693..847L    Altcode: 2008arXiv0805.1055L
  We present a detailed imaging and spectroscopic study of the conjugate
  hard X-ray (HXR) footpoints (FPs) observed with the Ramaty High
  Energy Solar Spectroscopic Imager (RHESSI) in the 2003 October 29
  X10 flare. The double FPs first move toward and then away from each
  other, mainly parallel and perpendicular to the magnetic neutral line,
  respectively. The transition of these two phases of FP unshearing
  motions coincides with the direction reversal of the motion of the
  loop-top (LT) source, and with the minima of the estimated loop length
  and LT height. We find temporal correlations between the HXR flux,
  spectral index, and magnetic field strength of each FP. The HXR flux
  exponentially correlates with the magnetic field strength, which also
  anticorrelates with the spectral index before the second HXR peak's
  maximum, suggesting that particle acceleration sensitively depends
  on the magnetic field strength and/or reconnection rate. Asymmetries
  are observed between the FPs: on average, the eastern FP is 2.2
  times brighter in HXR flux and 1.8 times weaker in magnetic field
  strength, and moves 2.8 times faster away from the neutral line
  than the western FP; the estimated coronal column density to the
  eastern FP from the LT source is 1.7 times smaller. The two FPs have
  marginally different spectral indices. The eastern-to-western FP HXR
  flux ratio and magnetic field strength ratio are anticorrelated only
  before the second HXR peak's maximum. Neither magnetic mirroring nor
  column density alone can explain the totality of these observations,
  but their combination, together with other transport effects, might
  provide a full explanation. We have also developed novel techniques to
  remove particle contamination from HXR counts and to estimate effects
  of pulse pileup in imaging spectroscopy, which can be applied to other
  RHESSI flares in similar circumstances.

---------------------------------------------------------
Title: Calculation of astrophysical reaction rate of
    <SUP>82</SUP>Ge(n,γ)<SUP>83</SUP>Ge
Authors: Wang, Mian; Chen, Yong-Shou; Li, Zhi-Hong; Liu, Wei-Ping;
   Shu, Neng-Chuan
2009ChPhC..33...79W    Altcode:
  The neutron capture reaction on a neutron-rich near closed-shell nucleus
  <SUP>82</SUP>Ge may play an important role in the r-process following
  the fallout from nuclear statistical equilibrium in core-collapse
  supernovae. By carrying out a DWBA analysis for the experimental
  angular distribution of <SUP>82</SUP>Ge(d, p)<SUP>83</SUP>Ge reaction
  we obtain the single particle spectroscopic factors, S<SUB>2,5/2</SUB>
  and S<SUB>0,1/2</SUB> for the ground and first excited states
  of <SUP>83</SUP>Ge = <SUP>82</SUP>Geotimesn, respectively. And
  then these spectroscopic factors are used to calculate the direct
  capture cross sections for the <SUP>82</SUP>Ge(n, γ)<SUP>83</SUP>Ge
  reaction at energies of astrophysical interest. The optical potential
  for neutron scattering on unstable nucleus <SUP>82</SUP>Ge is not
  known experimentally. We employed a real folding potential which was
  calculated by using the proper <SUP>82</SUP>Ge density distribution
  and an effective nucleon-nucleon force DDM3Y. The neutron capture
  reactions on neutron-rich closed-shell nuclei are expected to be
  dominated by the direct capture to bound states. We will show that the
  direct capture rates on these nuclei are sensitive to the structure
  of the low-lying states.

---------------------------------------------------------
Title: Characterization of ULF pulsations by THEMIS
Authors: Sarris, T. E.; Liu, W.; Kabin, K.; Li, X.; Elkington, S. R.;
   Ergun, R.; Rankin, R.; Angelopoulos, V.; Bonnell, J.; Glassmeier,
   K. H.; Auster, U.
2009GeoRL..36.4104S    Altcode: 2009GeoRL..3604104S
  The THEMIS five-probe constellation was launched in 17 February 2007
  to study substorms; however its instrumentation and the alignment
  at distances &lt;1R<SUB>E</SUB> among some of the THEMIS probes,
  particularly in the first period of its mission, provides unique
  opportunities to study ULF pulsations in the magnetosphere. In the
  case study presented, electric and magnetic field fluctuations are
  identified as field line resonances and their modes of oscillation are
  discussed. Phase-difference calculations between probes allow estimates
  of the mode number of the fluctuations. These observations give an
  excellent source for the verification of model estimates of frequency
  and polarization of the various modes of field line resonances.

---------------------------------------------------------
Title: Observation and modeling of the injection observed by THEMIS
    and LANL satellites during the 23 March 2007 substorm event
Authors: Liu, W. L.; Li, X.; Sarris, T.; Cully, C.; Ergun, R.;
   Angelopoulos, V.; Larson, D.; Keiling, A.; Glassmeier, K. H.; Auster,
   H. U.
2009JGRA..114.0C18L    Altcode: 2009JGRA..11400C18L
  During the encounter of a substorm on 23 March 2007, the THEMIS
  constellation observed energetic particle injections and dipolarizations
  in the premidnight sector. Clear injection and dipolarization signatures
  were observed during the main intensification by three probes (A,
  B, and D) in the region around 11 R <SUB> E </SUB> and 2100 local
  time (LT). THEMIS C, which was leading in the constellation at 8.3
  R <SUB> E </SUB>, also observed a clear injection signature, but
  the dipolarization was not so clear. From the timing based on these
  observations, a fast westward expanding ion injection and dipolarization
  front was identified. In combination with the energetic particle
  observations from Los Alamos National Laboratory (LANL) geosynchronous
  satellites, the particle injection seemed to initiate between 2100 and
  0100 LT. This event provides an excellent opportunity to examine the
  dipolarization and particle injection processes beyond geosynchronous
  orbit and over a wide LT range. We model this injection event by means
  of test particle simulation, setting up an initial particle distribution
  and sending an earthward dipolarization-like pulse from the tail that
  also expands azimuthally, then recording the ions and electrons at the
  various satellite locations. Most features of the injected particles
  are reproduced by the test particle simulation. These include not only
  the earthward injections but also the fast westward expansion of the
  injection, as well as the timing of the injections as observed among
  different satellites that made the observations. On the basis of the
  observations and the simulation results, we suggest that this substorm
  injection was initiated around 2300 LT, farther down the tail, and
  propagated radially inward and expanded azimuthally.

---------------------------------------------------------
Title: Noise-sustained Convective Instability in a Magnetized
    Taylor-Couette Flow
Authors: Liu, Wei
2009ApJ...692..998L    Altcode: 2008arXiv0808.2513L
  The helical magnetorotational instability of the magnetized
  Taylor-Couette flow is studied numerically in a finite cylinder. A
  distant upstream insulating boundary is shown to stabilize the
  convective instability entirely while reducing the growth rate of
  the absolute instability. The reduction is less severe with greater
  height. After we model the boundary conditions properly, the wave
  patterns observed in the experiment turn out to be a noise-sustained
  convective instability. After the source of the noise resulting
  from unstable Ekman and Stewartson layers is switched off, a slowly
  decaying inertial oscillation is observed in the simulation. We reach
  the conclusion that the experiments completed to date have not yet
  reached the regime of absolute instability.

---------------------------------------------------------
Title: Warm ocean anomaly, air sea fluxes, and the rapid
    intensification of tropical cyclone Nargis (2008)
Authors: Lin, I. -I.; Chen, Chi-Hong; Pun, Iam-Fei; Liu, W. Timothy;
   Wu, Chun-Chieh
2009GeoRL..36.3817L    Altcode: 2009GeoRL..3603817L
  On 2 May 2008, category-4 tropical cyclone Nargis devastated Myanmar. It
  was observed that just prior to its landfall, Nargis rapidly intensified
  from a weak category-1 storm to an intense category-4 storm within only
  24 h. Using in situ ocean depth-temperature measurements and satellite
  altimetry, it is found that Nargis' rapid intensification took place
  on a pre-existing warm ocean anomaly in the Bay of Bengal. In the
  anomaly, the subsurface ocean is evidently warmer than climatology,
  as characterized by the depth of the 26°C isotherm of 73-101 m and
  the tropical cyclone heat potential of 77-105 kj cm<SUP>-2</SUP>. This
  pre-existing deep, warm subsurface layer leads to reduction in the
  cyclone-induced ocean cooling, as shown from the ocean mixed layer
  numerical experiments. As a result, there was a near 300% increase in
  the air-sea enthalpy flux to support Nargis' rapid intensification.

---------------------------------------------------------
Title: Energy Spectrum of the Electrons Accelerated by a Reconnection
Electric Field: Exponential or Power Law?
Authors: Liu, W. J.; Chen, P. F.; Ding, M. D.; Fang, C.
2009ApJ...690.1633L    Altcode: 2008arXiv0809.1212L
  The direct current (DC) electric field near the reconnection region
  has been proposed as an effective mechanism to accelerate protons and
  electrons in solar flares. A power-law energy spectrum was generally
  claimed in the simulations of electron acceleration by the reconnection
  electric field. However in most of the literature, the electric and
  magnetic fields were chosen independently. In this paper, we perform
  test-particle simulations of electron acceleration in a reconnecting
  magnetic field, where both the electric and magnetic fields are adopted
  from numerical simulations of the MHD equations. It is found that the
  accelerated electrons present a truncated power-law energy spectrum
  with an exponential tail at high energies, which is analogous to the
  case of diffusive shock acceleration. The influences of reconnection
  parameters on the spectral feature are also investigated, such as the
  longitudinal and transverse components of the magnetic field and the
  size of the current sheet. It is suggested that the DC electric field
  alone might not be able to reproduce the observed single or double
  power-law distributions.

---------------------------------------------------------
Title: Statefinder Diagnostic for Quintessence with or Without
    Thermal Interaction
Authors: Liu, Wei-Zhong; Liu, Dao-Jun
2009IJMPD..18...43L    Altcode: 2008arXiv0803.4039L
  The cosmological dynamics of a minimally coupled scalar field
  that couples to the background matter with thermal interactions is
  investigated using statefinder diagnostics. The time evolution of the
  statefinder pairs {r, s} and {r, q} are obtained under the circumstance
  that different values of model parameters are chosen. We show that the
  thermal coupling term does not affect the location of the late-time
  attractor, but exerts an influence on the evolution of the statefinder
  parameters. The most notable feature of the r-s plane for the thermal
  coupling model, which is distinguished from the other dark energy
  models, is that some part of the curve with thermal coupling can form
  a closed loop in the second quadrant (r &gt; 1, s &lt; 0).

---------------------------------------------------------
Title: Records from Lake Qinghai: Holocene climate history of
    Northeastern Tibetan Plateau linking to global change
Authors: An, Z.; Colman, S.; Zhou, W.; Brown, E.; Li, X.; Jull, T.;
   Wang, S.; Liu, W.; Sun, Y.; Lu, X.; Song, Y.; Chang, H.; Cai, Y.; Xu,
   H.; Wang, X.; Liu, X.; Wu, F.; Han, Y.; Cheng, P.; Ai, L.; Wang, Z.;
   Qiang, X.; Shen, J.; Zhu, Y.; Wu, Z.; Liu, X.
2008AGUFMPP24A..04A    Altcode:
  Lake Qinghai (99°36'-100°16'E, 36°32'-37°15'N ) of the north eastern
  margin of Tibet Plateau is the largest inland lake of China. It sits
  on the transitional zone of Asian monsoon- arid areas, receives
  influences of Asian monsoons and Westerlies, thus sensitive to
  global climate changes. Although previous studies had investigated
  Holocene climate change of Lake Qinghai area, it is rare to see
  precise Holocene climatic sequences of Lake Qinghai, nor in-depth
  discussions on controlling factors of Lake Qinghai climate changes. In
  Year 2005, with support from ICDP, Chinese Academy of Sciences (CAS),
  Chinese Ministry of Science and Technology (MOST) and National Science
  Foundation of China (NSFC), Drilling, Observation and Sampling of the
  Earths Continental Crust Corporation (DOSECC) and Institute of Earth
  Environment, Chinese Academy of Sciences (IEECAS) took a series of
  shallows cores from the southern basin of Lake Qinghai. West sub-basin
  sediments display Holocene lacustrine feature for the upper 5m, while
  the 5-18m are interbeded sediments of shallow lake, eolian-lacustrine
  and eolian loess. Chinese and US scientists with support from NSFC,
  MOST, CAS and NSF analysed 1F core from west sub-basin depocenter
  of the south basin with multiple physical, chemical, biological
  approaches. By comparing with modern process observation records, we
  obtained proxies that respectfully reflect precipitation, temperature
  and lake salinity changes, etc., reconstructed high resolution time
  sequences of magnetic susceptibility, colour scale, grain size, Corg,
  C/N, δ13Corg, carbonate, δ13C and δ18O of carbonate and ostracodes,
  elements, char-soot,Uk'37 and %C37:4 as well as pollen of the last
  13Ka. They indicate the climatic change history of Lake Qinghai since
  past 13Ka, and agreeable evidences are found from adjacent tree ring
  and stalagmite records. Comparison of Lake Qinghai Holocene climate
  change sequence with those from high altitude ice core, stalagmites
  and ocean records for East Asian monsoon and Indian monsoon show that,
  in accordance with Asian monsoon climate changes, at 11-5ka cal. 14C BP
  Lake Qinghai revealed the warm and humid Optimal climate, while since
  5ka cal.14C BP the Lake showed relatively cold and dry climate of New
  Glaciation, this orbital climate trend resembled northern hemisphere
  summer solar insolation changes. Lake Qinghai millennial-centennial
  climate events in Holocene are linked with Westerlies changes, and
  with East Asian summer monsoon front shift as well as winter monsoon,
  on centennial-decadal scale Lake Qinghai climate changes are controlled
  more by solar activities.

---------------------------------------------------------
Title: First Results from the THEMIS Mission
Authors: Angelopoulos, V.; Sibeck, D.; Carlson, C. W.; McFadden,
   J. P.; Larson, D.; Lin, R. P.; Bonnell, J. W.; Mozer, F. S.; Ergun,
   R.; Cully, C.; Glassmeier, K. H.; Auster, U.; Roux, A.; Le Contel,
   O.; Frey, S.; Phan, T.; Mende, S.; Frey, H.; Donovan, E.; Russell,
   C. T.; Strangeway, R.; Liu, J.; Mann, I.; Rae, J.; Raeder, J.; Li,
   X.; Liu, W.; Singer, H. J.; Sergeev, V. A.; Apatenkov, S.; Parks,
   G.; Fillingim, M.; Sigwarth, J.
2008SSRv..141..453A    Altcode: 2008SSRv..tmp...90A
  THEMIS was launched on February 17, 2007 to determine the trigger and
  large-scale evolution of substorms. During the first seven months of
  the mission the five satellites coasted near their injection orbit
  to avoid differential precession in anticipation of orbit placement,
  which started in September 2007 and led to a commencement of the
  baseline mission in December 2007. During the coast phase the probes
  were put into a string-of-pearls configuration at 100 s of km to 2
  R<SUB>E</SUB> along-track separations, which provided a unique view of
  the magnetosphere and enabled an unprecedented dataset in anticipation
  of the first tail season. In this paper we describe the first THEMIS
  substorm observations, captured during instrument commissioning on
  March 23, 2007. THEMIS measured the rapid expansion of the plasma sheet
  at a speed that is commensurate with the simultaneous expansion of the
  auroras on the ground. These are the first unequivocal observations of
  the rapid westward expansion process in space and on the ground. Aided
  by the remote sensing technique at energetic particle boundaries and
  combined with ancillary measurements and MHD simulations, they allow
  determination and mapping of space currents. These measurements show
  the power of the THEMIS instrumentation in the tail and the radiation
  belts. We also present THEMIS Flux Transfer Events (FTE) observations
  at the magnetopause, which demonstrate the importance of multi-point
  observations there and the quality of the THEMIS instrumentation in
  that region of space.

---------------------------------------------------------
Title: A Pleistocene Indian Monsoon record from Heqing Basin, SW China
Authors: Qiang, X.; An, Z.; Shen, J.; Jin, Z.; Sun, Y.; Tong, G.;
   Chang, H.; Liu, X.; Liu, W.; Wang, S.; Zhou, W.; Song, Y.; Xiao, X.;
   Xiao, H.
2008AGUFMPP24A..01Q    Altcode:
  Heqing Basin (100°06'-100°16'E, 26°28'-26°46'N) is situated in
  southeastern margin of Tibetan Plateau, a geological conjunction
  zone of three tectonic units separated by Jinshajiang, Honghe and
  Xiaojinhe-Lijiang fault belts. Modern climate in this region is mainly
  influenced by Indian monsoon circulation. In Year 2002, a 665.83 m
  long core was retrieved from the Heqing basin under the support of
  Chinese Environmental Scientific Drilling program, which permits a
  high-resolution reconstruction of the Indian monsoon evolution from
  a continental perspective. The core mainly consists of gray clay,
  silty clay and silt. Magnetostratographic result generated by both
  thermal and alternating-field demagnetization methods indicates that
  the bottom age of the Heqing core is about 2.78 Myr. Multiple proxies
  (magnetic susceptibility, grain size, CaCO3 content, loss of ignite,
  pollen concentrations, and major/trace elements) were generated
  to reconstruct regional climate change and its dynamical links to
  Indian summer monsoon and solar insolation forcing. The results
  suggest that during glacial periods, this region is characterized
  by reduced vegetation cover (e.g., low total pollen concentration)
  and enhanced physical weathering (e.g., high Rb/Sr ratio), whereas
  during interglacial times, vegetation cover was extensive and chemical
  weathering is relatively strong around Heqing basin. Good correlation
  between variations in proxy indicators from Heqing core and stacked
  Indian summer monsoon record from Arabian Sea (Clemens and Prell, 2003)
  indicates that over the last 0.35 Myr, Heqing basin is predominantly
  influenced by Indian summer monsoon. Unlike Indian monsoon records from
  the Arabian Sea and Indian Ocean which resolution is relatively low,
  our high-resolution proxy variations permit a robust understanding of
  the Indian summer monsoon variations over the last 2.6 Myr. Comparisons
  of monsoon proxies from land and ocean indicate that solar insolation
  is the dominant factor controlling the Indian summer monsoon variation,
  particularly low-latitude radiation difference between northern and
  southern Hemisphere. However, an evident 100-kyr cycle occurred around
  1.2 Myr and became remarkable after 0.5 Myr, implying that global ice
  volume might have a significant influence on the monsoon records in
  Heqing basin since at least mid- Pleistocene.

---------------------------------------------------------
Title: Statistical study on the characterization of ULF Pulsations
    in the Inner Magnetosphere by THEMIS
Authors: Liu, W.; Sarris, T.; Liu, X.; Elkington, S. R.; Ergun, R.;
   Kabin, K.; Rankin, R.; Angelopoulos, V.; Bonnell, J.; Glassmeier,
   K.; Auster, U.
2008AGUFMSM33A1753L    Altcode:
  ULF pulsations (2~25 mHz) have significant influence on the transport
  of energetic particles trapped in the outer radiation belt, which have
  drift frequencies comparable to this range. However recent studies
  indicate that not all classes of ULF waves are equally important
  for radiation belt electron acceleration. For example, simulations
  suggest that electrons could be adiabatically accelerated through a
  drift-resonance interaction with either azimuthal (toroidal) mode or
  radial (poloidal) mode ULF waves. THEMIS electric field observations
  provide a good opportunity to study and fully characterize the features
  of the ULF pulsations in the inner magnetosphere. The ULF polarization
  study by Sarris et al [2008] focuses on the observations made by one
  THEMIS probe during its out-bound pass on September 4th, 2007. Here
  we will present the statistical studies of the polarizations of ULF
  pulsations, based on the spin-fit electric and magnetic field data
  from July 2007 to June 2008, with full local time coverage. Through
  this global coverage, ULF polarizations are characterized at different
  regions, in terms of radial distance and local times. Preliminary
  analysis indicates that the polarizations of electric field pulsation
  are more radial in dawn/dusk sectors and more azimuthal in noon/midnight
  sectors.

---------------------------------------------------------
Title: Ion temperature drop and quasi-electrostatic electric field
    on edge of the current sheet minutes prior to the local current
    disruption
Authors: Liang, J.; Liu, W. W.; McFadden, J. P.
2008AGUFMSM43A1725L    Altcode:
  Cross-tail current disruption (CD) in the near-Earth plasma sheet has
  been well recognized as the key process at the substorm expansion
  phase onset. However, some outstanding questions such as: what
  is the principal local magnetospheric parameters that control the
  stableness/unstableness of a thin current sheet (TCS), what is the
  dominating plasma instability mode leading to the CD, remain to be
  answered. Recent theoretical studies indicated that the stableness of
  the TCS is particularly sensitive to the distribution of ion drift
  velocity across the thickness of the current sheet, and that the
  quasi-electrostatic electric field developed in an ion-kinetic-scale
  TCS may play a key role in driving the TCS to instability. This
  motivates an investigation of the variations of plasma parameters
  at the edge of the TCS during the final minutes prior to the local
  CD. On a statistical survey of the near-Earth CD events during substorm
  intervals collected form the first tail season of the THEMIS mission,
  we identify a consistent behavior of precipitous drops of the thermal
  ion temperature at the edge of the current sheet in a couple of minutes
  before the local CD. Such ion temperature drop is interpreted as
  associated with the extreme thinning of an embedded TCS structure that
  leads to its ultimate disruption. The observed ion cooling is always
  accompanied with significant electric and magnetic field perturbations
  containing both systematic shift and wave oscillations. In particular
  we also reveal the concurrent growth of a neutral sheet-pointing
  quasi-electrostatic electric field minutes prior to the local CD. We
  discuss and simulate the role of such quasi-electrostatic field in
  leading to the ion temperature drop and the subsequent CD process. The
  wave components of the observed electric/magnetic perturbations are
  interpreted as Alfvenic effects of the kinetic ballooning mode.

---------------------------------------------------------
Title: Electrostatic field prior to local current sheet disruption
Authors: Liu, W.; Liang, J.; Donovan, E.
2008AGUFMSM43A1726L    Altcode:
  We present observation of plasma waves in the current sheet across
  multiple THEMIS satellites in a substorm event on March 5, 2008. It is
  shown that the arrival of a kinetic ballooning perturbation interacts
  with the local current sheet to generate a quasi-electrostatic wave
  a few minutes before local onset, consistent with the prediction
  that the current sheet thins after the passage of a rarefaction
  wave. It is proposed that the presence of the quasi-electrostatic
  field may change the local stability condition and induce local current
  disruption. Preliminary theoretical calculation is given to substantiate
  this idea.

---------------------------------------------------------
Title: Characterization of ULF Pulsations by THEMIS
Authors: Sarris, T. E.; Liu, W.; Kabin, K.; Li, X.; Elkington, S.;
   Ergun, R.; Rankin, R.; Angelopoulos, V.; Bonnel, J.; Glassmeier, K.;
   Auster, U.
2008AGUFMSM33A1754S    Altcode:
  This paper reports the first use of THEMIS to determine the polarization
  properties of ULF waves in a non- dipolar magnetic topology: The
  instrumentation and the alignment at close distances (less than
  1 RE) among some of the THEMIS probes (particularly in the first
  period of its mission) provides unique opportunities to characterize
  ULF pulsations in the magnetosphere and enables us to validate and
  parameterize existing models. In the case study presented, electric and
  magnetic field fluctuations are identified as field line resonances
  and their modes of oscillation are compared to model estimates. Out
  of the various modes predicted by the model, the second fundamental
  mode, or toroidal mode, appears to have most similarities to the
  measured polarizations. Furthermore, phase-difference calculations
  using the probes' small separations allow estimates of mode number
  and propagation characteristics. It is shown that these observations
  give an excellent source for the verification of model estimates of
  frequency and polarization of the various modes of field line resonances
  in the magnetosphere.

---------------------------------------------------------
Title: Multiple intensifications inside the auroral bulge and their
    association with plasma sheet activities
Authors: Keiling, A.; Angelopoulos, V.; Larson, D.; McFadden, J.;
   Carlson, C.; Fillingim, M.; Parks, G.; Frey, S.; Glassmeier, K. -H.;
   Auster, H. U.; Magnes, W.; Liu, W.; Li, X.
2008JGRA..11312216K    Altcode:
  In this coordinated ground and space study, we report multiprobe
  measurements from Time History of Events and Macroscale Interactions
  during Substorms (THEMIS), LANL-97A, Polar, and ground observatories
  for a substorm that occurred on 23 March 2007. The THEMIS fleet and
  LANL-97A were located in the premidnight, near-Earth plasma sheet in
  the radial range from 6.6 to 13 R<SUB>E</SUB>, placing the spacecraft
  into different plasma environments which were subject to different
  activities. Simultaneous global Polar Ultraviolet Imager images of
  the aurora revealed a fine structure in the auroral bulge in the
  form of several time-delayed regions of brightening. We demonstrate a
  correspondence between this fine structure and the spatially separated
  plasma sheet activities (substorm injections with energies &gt;100
  keV) by showing that both executed periodic (100-150 s) one-to-one
  correlated modulations. Additionally, the different auroral brightening
  regions were modulated approximately out of phase to one another,
  as were the separated plasma sheet activities. The periodic plasma
  sheet and optical modulations were also one-to-one correlated with
  large-amplitude (δH ∼ 150 nT) ground Pi2 pulsations. In contrast
  to the most energetic ions (&gt;100 keV), the lower-energetic plasma
  sheet ions executed separate oscillations during the development of
  the substorm, including the preintensification phase, and showed the
  following properties. (1) The oscillation periods were different at
  different spacecraft locations and had a tendency to increase during
  the evolution of the substorm. During the preintensification phase,
  multiple (possibly harmonic) spectral components existed. (2) The
  oscillations were coupled to westward moving perturbations of an
  energized plasma boundary. The boundary perturbations were likely
  conjugate to azimuthally spaced auroral forms ("beads") observed by
  Polar-UVI during the preintensification phase and could play a role
  in the onset of the substorm intensification. (3) The oscillations
  of the lower-energetic ions were also one-to-one correlated with
  smaller-amplitude ground Pi2 pulsations (&lt;15 nT). In conclusion, the
  combination of these observations allowed us to construct a 3-D picture
  of low-frequency, near-Earth plasma sheet phenomena associated with a
  substorm and their connection to aurora and the ground. It appeared that
  not only one substorm current wedge, but additional current structures
  existed which started at different times, pulsated out of phase,
  and mapped from different active regions into the ionosphere. The
  active space regions appeared to be coupled and transferring energy
  from one region to the other while pulsating. We propose that the
  wave-like structures in the plasma sheet, observed before and during
  the substorm/intensification phase, and their demonstrated properties
  support a wave phenomenon (such as a ballooning-type mode) for the
  onset and development of the substorm/intensification, rather than
  directly driven periodic bursty bulk flow activations.

---------------------------------------------------------
Title: The magnetotail implications of optical observations of the
    brightening substorm aurora
Authors: Donovan, E.; Spanswick, E.; Moores, K.; Liu, W.; Liang, J.;
   Strangeway, R.; McFadden, J.; Carlson, C.
2008AGUFMSM23B1709D    Altcode:
  Ground-based optical and topside in situ observations have shown
  conclusively that many substorm auroral onsets occur immediately
  poleward of the proton aurora brightness peak. This has long been
  interpreted as placing a rather stringent constraint on the location
  of whatever magnetospheric process corresponds to the brightening
  auroral arc, namely that the relevant field lines thread the
  region of transition between dipole- and tail-like magnetic field
  topologies. However, this constraint, by itself, presents us with a
  number of critical questions. For example, we do not know how abrupt
  the transition between dipole- and tail-like topologies is, nor do we
  know the location of that transition in the magnetosphere on either an
  event by event or even a general basis. Not knowing the radial extent of
  the transition region limits our ability to explore the nature of the
  onset instability. Not knowing the actual location of the transition
  limits our ability to optimally utilize the ionospheric observations
  in conjunction with contemporaneous satellite observations. In this
  paper we take a step back from event studies and explore broader
  implications of the location of the onset arc relative to the peak
  in proton auroral brightness. More specifically, we use pitch-angle
  resolved FAST ESA ion observations from more than 20000 transits of
  the auroral zone to explore the latitudinal separation between the peak
  precipitating ion energy flux (which corresponds to the peak in proton
  auroral brightness) and the inner edge of the electron and ion plasma
  sheets. We use these results, in conjunction with magnetic mapping and
  published observations of the equatorial location of the inner edge of
  the ion and electron plasma sheets, to explore the range of locations
  in the magnetotail to which the onset arc is most likely to map, as
  well as how the relative distance between the transition region and
  the inner edge of the plasma sheet varies through the substorm cycle.

---------------------------------------------------------
Title: Global observations of injection region evolution during a
    reconnection initiated substorm
Authors: Spanswick, E.; Donovan, E.; Blake, J. B.; Cully, C.; Reeves,
   G.; Friedel, R.; Weatherwax, A.; Liu, W.
2008AGUFMSM43A1714S    Altcode:
  Recent studies have shown that dispersionless injections can be
  identified in riometer data [Spanswick et al., 2007]. This raises
  the possibility of using a network of riometers to identify the time
  when and location (at least as projected in the ionosphere) where
  an injection began, and of following its subsequent spatio- temporal
  evolution. In this paper, we present a detailed picture of the evolution
  of a large substorm injection. The event occurred on August 27, 2001,
  and has been discussed in numerous publications. The expansion phase
  in question followed several smaller activations that would reasonably
  be described as pseudobreakups. Baker et al. [2002] used Cluster in
  situ and IMAGE FUV observations to argue that near- Earth reconnection
  preceded the auroral onset. Blake et al. [2005] used Cluster, Polar, and
  Chandra data to investigate the large-scale expansion of the injection
  region, subject to the caveat that the injection was well underway when
  it expanded over the satellites. In this paper, we present riometer
  and in situ observations of an injection seen at more than 20 separate
  locations (including 6 satellites: Cluster, Polar, Chandra, and 3 LANL
  spacecraft). The injection is observed to be dispersionless at 12 of
  these locations (three of them are observations previously reported
  by Blake). We are able to identify the time and location at which
  the injection begins. Combining these observations with information
  from the GOES-8 geosynchronous satellite we argue that the injection
  initiated near-geosynchronous orbit and expanded poleward (tailward)
  and equatorward (earthward) from its beginning. Further, the injection
  began several minutes after the reconnection identified in the Cluster
  data, providing concrete evidence that near-Earth reconnection, in at
  least some events, has little if any ionospheric signature.

---------------------------------------------------------
Title: Long Term Evolution of Magnetized Bubbles in Galaxy Clusters
Authors: Liu, Wei; Li, Hui; Li, Shengtai; Hsu, Scott
2008APS..DPPUP6020L    Altcode:
  We have performed nonlinear ideal magnetohydrodynamic simulations of
  the long term evolution of a magnetized low-density “bubble" plasma
  formed by a radio galaxy in a stratified cluster medium. It is found
  that about 3.5% of the initial magnetic energy remains in the bubble
  after ∼8 x10^9 years, and the initial magnetic bubble expansion is
  adiabatic. The bubble can survive for at least 8 x10^9 years due to
  the stabilizing effect of the bubble magnetic field on Rayleigh-Taylor
  and Kelvin-Holmholtz instabilities, possibly accounting for “ghost
  cavities" as observed in Perseus-A@. A filament structure spanning
  about 500 kpc is formed along the path of bubble motion. The mean
  value of the magnetic field inside this structure is ∼0.57 μG at
  ∼8x10^9 years. Finally, the initial bubble momentum and rotation
  have limited influence on the long term evolution of the bubble.

---------------------------------------------------------
Title: Magnetic Bubble Expansion as an Experimental Model for
    Extra-Galactic Radio Lobes
Authors: Lynn, Alan G.; Zhang, Yue; Hsu, Scott; Li, Hui; Liu, Wei;
   Gilmore, Mark; Watts, Christopher
2008APS..DPPUP6046L    Altcode:
  The Plasma Bubble Expansion Experiment (PBEX) has begun laboratory
  experiments and coordinated nonlinear MHD simulations to address
  outstanding nonlinear plasma physics issues related to how magnetic
  energy and helicity carried by extra-galactic jets interacts with the
  intergalactic medium to form radio lobe structures. Experiments are
  being conducted in the 4 meter long, 50 cm diameter HELCAT linear plasma
  device at UNM. A pulsed magnetized coaxial gun (∼10 kV, ∼100 kA,
  ∼2 mWb) forms and injects magnetized plasma bubbles perpendicularly
  into a lower pressure weakly magnetized background plasma formed by a
  helicon and/or hot cathode source in HELCAT. Experimental parameters
  can be adjusted so that important dimensionless parameters are
  relevant to the astrophysical context. Ideal MHD simulations show
  that an MHD shock develops ahead of the bubble as it propagates,
  and that the bubble develops asymmetries due to the background field
  [1]. First experimental data, including magnetic probe measurements
  and high-speed camera imaging, will be presented. [1] W. Liu et al.,
  Phys. Plasmas 15, 072905 (2008).

---------------------------------------------------------
Title: Ideal MHD simulations of laboratory and astrophysical magnetic
    bubble expansion as a model for extragalactic radio lobes.
Authors: Liu, Wei; Hsu, Scott; Li, Hui; Li, Shengtai; Lynn, Alan
2008APS..DPPYP6053L    Altcode:
  Nonlinear ideal magnetohydrodynamic (MHD) simulations of the propagation
  and expansion of a magnetic “bubble” plasma into a lower density,
  weakly-magnetized background plasma are presented. These simulations
  mimic the geometry and parameters of the Plasma Bubble Expansion
  Experiment (PBEX), which is studying magnetic bubble expansion as a
  model for extra-galactic radio lobes. The simulations predict several
  key features of the bubble evolution. First, the direction of bubble
  expansion depends on the ratio of the bubble toroidal to poloidal
  magnetic field, with a higher ratio leading to expansion predominantly
  in the direction of propagation and a lower ratio leading to expansion
  predominantly normal to the direction of propagation. Second, an MHD
  shock and a trailing slow-mode compressible MHD wavefront are formed
  ahead of the bubble as it propagates into the background plasma. Third,
  the bubble expansion and propagation develop asymmetries about
  its propagation axis due to reconnection facilitated by numerical
  resistivity and to inhomogeneous angular momentum transport mainly
  due to the background magnetic field. These results will help guide
  the initial experiments and diagnostic measurements on PBEX.

---------------------------------------------------------
Title: Magnetic Fields and Turbulence in the Intra-cluster Medium
    of Galaxy Clusters
Authors: Li, Hui; Xu, Hao; Liu, Wei
2008APS..DPPUP6021L    Altcode:
  Recent observations have revealed that the intra-cluster medium (ICM) of
  galaxy clusters could be significantly magnetized. Observations further
  revealed that magnetic fields in the ICM have large amount of fluxes,
  yet appearing to have a power-law spectrum. It is often suggested that
  such magentic fields could be generated via a turbulent dynamo. Here,
  we study a different scenario where significant magnetic fields are
  produced by supermassive black holes (SMBHs) in the centers of massive
  galaxies, then these magnetic fields are transported to the wider
  ICM via jets/lobes during the lifetime of active galaxies (∼ 100
  Myr). Subsequent cluster mergers during the cluster evolution (up to
  10 Gyr) will stir, shear, and shock the ICM as well as the magnetic
  fields provided by SMBHs. We present numerical simulations of the
  evolution of clusters with magnetic fields using the newly developed
  cosmological MHD code with adaptive mesh refinement. The evolution
  of magnetic field energy and flux, along with the ICM dynamics,
  will be discussed in detail. By comparing our simulations with the
  observations, we will explore the implications for MHD turbulence and
  dynamo mechanisms in the ICM.

---------------------------------------------------------
Title: Overview of the Princeton MagnetoRotational Instability
    Experiment
Authors: Schartman, E.; Nornberg, M.; Roach, A.; Ji, H. T.; Coster,
   D.; Liu, W.; Goodman, J.; Burin, M. J.
2008APS..DPPUP6037S    Altcode:
  A turbulent viscosity is required to explain the
  observationally-inferred rates of angular momentum transport in
  accretion disks. Investigation of thin disks has focused on two
  sources of instability to drive the turbulence: the MagnetoRotational
  Instability (MRI) and Subcritical Hydrodynamic Instability (SHI). In
  MRI a weak ambient magnetic field causes the radially-decreasing angular
  velocity to become a source of free energy. In SHI, stable perturbations
  allow access to unstable modes. This experiment investigates both of
  these instabilities in a Couette-Taylor flow. Using water or liquid
  Gallium alloy we generate rotating shear flows with linear stability
  properties analagous to astrophysical disks. Differentially rotatable
  end-rings reduce boundary effects. We found no evidence of SHI, up
  to Reynolds number of order one million. During the MHD experiments a
  solenoidal magnetic field of up to 5 kG is applied. Radially-aligned
  induction coils detect magnetic perturbations generated by the liquid
  metal. Initial magnetized experiments focussed on magneto-Coriolis waves
  which at large magnetic Reynolds number are expected to transition into
  MRI modes. Results of the current search for the MRI will be presented.

---------------------------------------------------------
Title: Actuality and futurity of San Juan 7406 SLR Station
Authors: Liu, W.; Han, Y.; Actis, E.; Alonso, E.; Podesta, R.;
   Gonzalez, A. A.; Pacheco, A. M.; Zhao, L.; Liu, C.; Yin, Z.
2008lara.workE..96L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interaction between kinetic ballooning perturbation and thin
current sheet: Quasi-electrostatic field, local onset, and global
    characteristics
Authors: Liu, W. W.; Liang, J.; Donovan, E. F.
2008GeoRL..3520107L    Altcode:
  We present observation of plasma waves in the current sheet across
  multiple THEMIS satellites in a substorm event on March 5, 2008. It is
  shown that the arrival of a kinetic ballooning perturbation interacts
  with the local current sheet to generate a quasi-electrostatic wave
  a few minutes before local onset, consistent with the prediction that
  the current sheet thins after the passage of a rarefaction wave. The
  propagation speed of current disruption front is found to be ~100
  km/s, about a tenth of the fast mode speed. The observed pattern of
  interaction was constant across radial distances between 10 and 20
  R <SUB> E </SUB> in the event reported. It is further proposed that
  the presence of the quasi-electrostatic field may change the local
  stability condition and induce local current disruption.

---------------------------------------------------------
Title: Numerical Study of the Magnetorotational Instability in
    Princeton MRI Experiment
Authors: Liu, Wei
2008ApJ...684..515L    Altcode: 2008arXiv0804.0044L
  In preparation for an experimental study of magnetorotational
  instability (MRI) in liquid metal, we present nonideal axisymmetric
  magnetohydrodynamic simulations of the nonlinear evolution of MRI in the
  experimental geometry. The simulations adopt fully insulating boundary
  conditions. No-slip conditions are imposed at all boundaries. A clear
  linear phase is observed with reduced linear growth rate. MRI results in
  an inflowing "jet" near the midplane and enhances the angular momentum
  transport at saturation.

---------------------------------------------------------
Title: Long-Term Evolution of Magnetized Bubbles in Galaxy Clusters
Authors: Liu, Wei; Li, Hui; Li, Shengtai; Hsu, Scott C.
2008ApJ...684L..57L    Altcode: 2008arXiv0806.3717L
  We have performed nonlinear ideal magnetohydrodynamic simulations
  of the long-term evolution of a magnetized low-density "bubble"
  plasma formed by a radio galaxy in a stratified cluster medium. It
  is found that about 3.5% of the initial magnetic energy remains in
  the bubble after ~8 × 10<SUP>9</SUP> yr, and the initial magnetic
  bubble expansion is adiabatic. The bubble can survive for at least
  8 × 10<SUP>9</SUP> yr due to the stabilizing effect of the bubble
  magnetic field on Rayleigh-Taylor and Kelvin-Helmholtz instabilities,
  possibly accounting for "ghost cavities" as observed in Perseus A. A
  filament structure spanning about 500 kpc is formed along the path
  of bubble motion. The mean value of the magnetic field inside this
  structure is ~0.88 μG at ~8 × 10<SUP>9</SUP> yr. Finally, the initial
  bubble momentum and rotation have limited influence on the long-term
  evolution of the bubble.

---------------------------------------------------------
Title: Simultaneous THEMIS in situ and auroral observations of a
    small substorm
Authors: Donovan, E.; Liu, W.; Liang, J.; Spanswick, E.; Voronkov,
   I.; Connors, M.; Syrjäsuo, M.; Baker, G.; Jackel, B.; Trondsen, T.;
   Greffen, M.; Angelopoulos, V.; Russell, C. T.; Mende, S. B.; Frey,
   H. U.; Keiling, A.; Carlson, C. W.; McFadden, J. P.; Glassmeier,
   K. -H.; Auster, U.; Hayashi, K.; Sakaguchi, K.; Shiokawa, K.; Wild,
   J. A.; Rae, I. J.
2008GeoRL..3517S18D    Altcode:
  We present ground-based and in situ observations from March 13,
  2007. The THEMIS satellites were in the evening sector conjugate to
  THEMIS ground-based imagers. At ~0507 UT there was an optical onset on
  inner CPS field lines. This involved near-simultaneous brightening of 1
  MLT hour longitudinal segment of the onset arc. The part of the arc that
  brightened was that closest to the equatorward boundary of the diffuse
  (proton) aurora. Within one minute, a dipolarization front moved across
  four THEMIS satellites. Based on their locations, the order in which
  they detected the dipolarization front, and the auroral evolution, we
  assert that the expansion phase began earthward of the four satellites
  and evolved radially outwards. We conclude that this onset occurred
  in an azimuthally localized region of highly stretched field lines.

---------------------------------------------------------
Title: Wind power distribution over the ocean
Authors: Liu, W. Timothy; Tang, Wenqing; Xie, Xiaosu
2008GeoRL..3513808L    Altcode:
  Probability distribution and power density of wind speed over global
  oceans are computed from eight years of QuikSCAT measurements. They
  describe the variation and higher moments of wind speed that are
  critical in relating the non-linear effects of wind on electric
  power generation capability, shipping hazard, and air-sea exchanges
  in heat, water, and greenhouse gases. The power density distribution
  confirms our general knowledge of atmospheric circulation related to
  mid-latitude storm tracks, trade winds, and monsoons. It also reveals
  regions of high wind power associated with flow distortion by land,
  wind channeled by land topography, and buoyancy effect on turbulent
  stress driven by ocean fronts.

---------------------------------------------------------
Title: Ideal magnetohydrodynamic simulation of magnetic bubble
    expansion as a model for extragalactic radio lobes
Authors: Liu, Wei; Hsu, Scott C.; Li, Hui; Li, Shengtai; Lynn, Alan G.
2008PhPl...15g2905L    Altcode: 2008arXiv0804.3379L
  Nonlinear ideal magnetohydrodynamic (MHD) simulations of the propagation
  and expansion of a magnetic “bubble” plasma into a lower density,
  weakly magnetized background plasma, are presented. These simulations
  mimic the geometry and parameters of the Plasma Bubble Expansion
  Experiment (PBEX) [A. G. Lynn, Y. Zhang, S. C. Hsu, H. Li, W. Liu,
  M. Gilmore, and C. Watts, Bull. Am. Phys. Soc. 52, 53 (2007)], which
  is studying magnetic bubble expansion as a model for extragalactic
  radio lobes. The simulations predict several key features of the
  bubble evolution. First, the direction of bubble expansion depends
  on the ratio of the bubble toroidal to poloidal magnetic field, with
  a higher ratio leading to expansion predominantly in the direction
  of propagation and a lower ratio leading to expansion predominantly
  normal to the direction of propagation. Second, a MHD shock and a
  trailing slow-mode compressible MHD wavefront are formed ahead of the
  bubble as it propagates into the background plasma. Third, the bubble
  expansion and propagation develop asymmetries about its propagation
  axis due to reconnection facilitated by numerical resistivity and to
  inhomogeneous angular momentum transport mainly due to the background
  magnetic field. These results will help guide the initial experiments
  and diagnostic measurements on PBEX.

---------------------------------------------------------
Title: Solar Flares as Natural Particle Accelerators: A High-energy
    View from X-ray Observations and Theoretical Models
Authors: Liu, Wei
2008sfpa.book.....L    Altcode:
  Solar flares, which have significant space weather consequences,
  are natural particle accelerators and one of the most spectacular
  phenomena of solar activity. RHESSI is the most advanced solar X-ray
  and gamma-ray mission ever flown and has opened a new era in solar
  flare research following its launch in 2002. <P />This book offers a
  glimpse of this active research area from a high-energy perspective
  and contains a comprehensive guideline for RHESSI data analysis. Its
  main theme is the investigation of particle acceleration and transport
  in solar flares. The strength of this book lies in its well-balanced
  account of the latest X-ray observations and theoretical models. The
  observational focus is on the morphology and spectra of imaged X-ray
  sources produced by nonthermal electrons or hot plasma. The modeling
  takes the novel approach of combining the Fokker-Planck treatment of
  the accelerated particles with the hydrodynamic treatment of the heated
  atmosphere. Applications of this modeling technique reach beyond the
  Sun to other exotic environments in the universe, such as extrasolar
  planetary auroras, stellar flares, and flares on accretion disks around
  neutron stars and black holes.

---------------------------------------------------------
Title: Correlation of substorm injections, auroral modulations,
    and ground Pi2
Authors: Keiling, A.; Angelopoulos, V.; Larson, D.; Lin, R.; McFadden,
   J.; Carlson, C.; Bonnell, J. W.; Mozer, F. S.; Glassmeier, K. -H.;
   Auster, H. U.; Magnes, W.; Mende, S.; Frey, H.; Roux, A.; Le Contel,
   O.; Frey, S.; Phan, T.; Donovan, E.; Russell, C. T.; Mann, I.; Liu,
   W.; Li, X.; Fillingim, M.; Parks, G.; Shiokawa, K.; Raeder, J.
2008GeoRL..3517S22K    Altcode:
  In this case study we report a substorm, 23 March 2007, which exhibited
  oscillations with a period of ~135 s in three substorm phenomena all
  of which were one-to-one correlated. The in-situ observations are
  from one THEMIS spacecraft (8.3 R <SUB> E </SUB> geocentric distance)
  and the geosynchronous LANL-97A spacecraft. The focus here is on the
  intensification phase during which THEMIS was conjugate to the region
  of auroral brightening and its foot point was near the high-latitude
  ground station Kiana. The following results will be demonstrated: (1)
  THEMIS and LANL-97A (time-delayed) recorded periodic ion injections
  (&gt;100 keV). (2) Near-conjugate high-latitude ground magnetometer
  data show very large Pi2 (δH~150 nT) with a 6-s time delay compared
  to the THEMIS ion injections. (3) Low-latitude ground magnetometer
  data also show Pi2 with the same waveform as the high-latitude Pi2
  but with longer time delays (20-31 s). (4) Auroral luminosity was
  periodically modulated during the intensification phase. (5) All three
  signatures (ion injections, ground Pi2, optical modulation) had the same
  periodicity of ~135 s but with various time delays with respect to the
  THEMIS ion injections. These observations demonstrate that the three
  substorm phenomena had a common source which controlled the periodicity.

---------------------------------------------------------
Title: Intensification of preexisting auroral arc at substorm
expansion phase onset: Wave-like disruption during the first tens
    of seconds
Authors: Liang, Jun; Donovan, E. F.; Liu, W. W.; Jackel, B.; Syrjäsuo,
   M.; Mende, S. B.; Frey, H. U.; Angelopoulos, V.; Connors, M.
2008GeoRL..3517S19L    Altcode:
  With the deployment of the all-sky imager array of the THEMIS mission,
  we were able to construct a preliminary database of auroral substorm
  expansion phase onsets, from which we have established a number
  of common features characterizing the first tens of seconds of the
  substorm auroral intensification. We find that the intensification
  occurs within ~10 sec over an arc segment extending approximately 1 h
  MLT and featuring wave-like formations distributed in longitude. The
  longitudinal wave number ranges between 100 and 300 such that the
  wavelength is comparable to the ion gyroradius in the central plasma
  sheet. The scale the intensification is about 10-30 sec. This study
  casts important observational constraints on substorm onset theories.

---------------------------------------------------------
Title: Ideal Magnetohydrodynamical Simulations of Magnetic Bubble
    Expansion as a Model for Extragalactic Radio Lobes
Authors: Liu, Wei; Hsu, S.; Li, S.; Li, H.
2008AAS...212.0339L    Altcode: 2008BAAS...40..191L
  Recent observations indicate that radio lobes are gigantic "relaxed"
  magnetized plasmas with kilo-to-megaparsec scale jets providing a source
  of magnetic energy from the galaxy to the lobes. We therefore have
  proposed a laboratory plasma experiment, in which a higher pressure
  <P />magnetized plasma bubble (i.e., the lobe) is injected into a
  lower pressure background plasma (i.e., the intergalactic medium) to
  study key nonlinear plasma physics issues. Here we present detailed
  ideal magnetohydrodynamical (MHD) three-dimensional simulations of
  this experiment. <P />The properties of the evolution of the bubble
  is dependent on the value of α. Larger α results in a axially
  expanding bubble like a growing “mushroom" while smaller α produces
  something like a "crab", expanding horizontally. The expansion of the
  bubble generates one perpendicular shock and one reversal slow-mode
  compressible MHD wave front, where 3-D reconnection is happening. The
  structure of shock/wavefront is almost independent of the injection
  velocity if it is reasonably low. The initially uniformly rotating
  bubble quickly evolves into a quasi-force-free state and transits to
  two oppositely-rotating bubbles. The axial angular momentum has been
  transported from the side where the bubble field is along the background
  field to the side where the bubble field is opposite to the background
  field. The discovery of MHD shocks shows that our experimental
  facility provides a good opportunity to study the MHD shocks, which
  are hardly to be observed in a laboratory experiment. Comparison of
  models and measurements will be used to validate the theoretical tools,
  which we will apply to nonlinear relaxation of magnetized plasma in
  astrophysical systems.

---------------------------------------------------------
Title: Laboratory Study of Angular Momentum Transport in Sheared
    Rotating Flows
Authors: Ji, Hantao; Nornberg, M.; Schartman, E.; Goodman, J.; Liu,
   W.; Roach, A.
2008AAS...212.0344J    Altcode: 2008BAAS...40..192J
  Rapid angular momentum transport in accretion disks is a longstanding
  astrophysical puzzle. Transport by molecular viscosity is inadequate
  to explain observationally inferred accretion rates. Since Keplerian
  flows are linearly stable in hydrodynamics, there exist only two
  main viable mechanisms for the required turbulence: nonlinear
  hydrodynamic instability or linear magnetorotational instability
  (MRI). The latter is regarded as a dominant mechanism for rapid
  angular momentum transport in hot accretion disks ranging from quasars
  and X-ray binaries to cataclysmic variables. The former is proposed
  mainly for cooler protoplanetary disks, whose Reynolds numbers are
  typically large. Despite their popularity, however, there is limited
  experimental evidence for either mechanism. In this talk, I will
  describe a laboratory experiment at Princeton (http://mri.pppl.gov)
  in a short Taylor-Couette flow geometry intended to study these
  mechanisms. Based on the results from prototype experiments and
  simulations, the apparatus contains novel features for better controls
  of the boundary-driven secondary flows. The experiments in water have
  shown<SUP>1</SUP> that nonmagnetic quasi-Keplerian flows at Reynolds
  numbers as large as 2× 10<SUP>6</SUP> are essentially laminar, through
  means of direct measurements of Reynolds stress via a synchronized, dual
  Laser Doppler Velocimetry. Scaled to accretion disks, rates of angular
  momentum transport lie far below astrophysical requirements. By ruling
  out hydrodynamic turbulence, our results indirectly support MRI as the
  likely cause of turbulence even in cool disks. The experiments in liquid
  gallium eutectic alloy have recently begun, and initial results on MRI
  as well as other related phenomena including numerical predictions will
  be also discussed if available. <P />1. H. Ji, M. Burin, E. Schartman,
  &amp; J. Goodman, Nature 444, 343-346 (2006).

---------------------------------------------------------
Title: Magnetized Ekman layer and Stewartson layer in a magnetized
    Taylor-Couette flow
Authors: Liu, Wei
2008PhRvE..77e6314L    Altcode: 2007arXiv0712.2543L
  In this paper we present axisymmetric nonlinear simulations of
  magnetized Ekman and Stewartson layers in a magnetized Taylor-Couette
  flow with a centrifugally stable angular-momentum profile and with a
  magnetic Reynolds number below the threshold of magnetorotational
  instability. The magnetic field is found to inhibit the Ekman
  suction. The width of the Ekman layer is reduced with increased magnetic
  field normal to the end plate. A uniformly rotating region forms
  near the outer cylinder. A strong magnetic field leads to a steady
  Stewartson layer emanating from the junction between differentially
  rotating rings at the endcaps. The Stewartson layer becomes thinner
  with larger Reynolds number and penetrates deeper into the bulk flow
  with stronger magnetic field and larger Reynolds number. However, at
  Reynolds number larger than a critical value ∼600 , axisymmetric,
  and perhaps also nonaxisymmetric, instabilities occur and result in a
  less prominent Stewartson layer that extends less far from the boundary.

---------------------------------------------------------
Title: Ideal Magnetohydrodynamical Simulations of Magnetic Bubble
    Expansion as a model for extragalactic radio lobes
Authors: Liu, Wei; Hsu, Scott; Li, Hui; Li, Shengtai; Lynn, Allan
2008APS..APR.K1025L    Altcode:
  Recent astronomical observations indicate that radio lobes are gigantic
  relaxed magnetized plasmas with kilo-to-megaparsec scale jets providing
  a source of magnetic energy from the galaxy to the lobes. Therefore
  we are conducting a laboratory plasma experiment, the Plasma Bubble
  Expansion Experiment (PBEX) in which a higher pressure magnetized plasma
  bubble (i.e., the lobe) is injected into a lower pressure background
  plasma (i.e., the intergalactic medium) to study key nonlinear plasma
  physics issues. Here we present detailed ideal magnetohydrodynamic (MHD)
  three-dimensional simulations of PBEX. Given reasonably low injection
  speeds of the magnetic bubble, its expansion due to the Lorentz force
  leads to one perpendicular MHD shock and one compressible reversal
  MHD wavefront, where three-dimensional reconnection results due to
  numerical resistivity. With the expansion, some angular momentum is
  transported from the rotating magnetic bubble to the background plasma
  mainly due to advection. The discovery of MHD shocks in the simulations
  shows that PBEX provides a rare opportunity to study MHD shocks in
  a laboratory experiment. Comparison of models and measurements will
  be used to validate the theoretical tools, which we will apply to
  nonlinear relaxation of magnetized plasmas in astrophysical systems.

---------------------------------------------------------
Title: Experimental study of plasma bubble expansion as a model for
    extragalactic radio lobes
Authors: Hsu, Scott; Lynn, Alan G.; Zhang, Yue; Liu, Wei; Li, Hui;
   Watts, Christopher; Gilmore, Mark
2008APS..APR.K1024H    Altcode:
  Recent work in plasma astrophysics has suggested that magnetic
  energy features prominently in the large-scale evolution of active
  galaxies. The Plasma Bubble Expansion Experiment (PBEX) at UNM will
  conduct laboratory experiments to address outstanding nonlinear plasma
  physics issues related to how magnetic energy and helicity carried by
  extra-galactic jets interacts with the intergalactic medium to form
  extra-galactic radio lobe structures. A newly-built pulsed coaxial
  gun will form and inject magnetized plasma bubbles into a lower
  pressure weakly-magnetized background plasma formed by the helicon
  and/or hot cathode source in HELCAT, a 4 m long and 50 cm diameter
  linear plasma device. Plasma properties can be adjusted such that
  important dimensionless parameters are relevant to the astrophysical
  context. Ideal MHD simulations of the experiment have indicated the
  strong possibility of MHD shocks appearing. This poster will provide
  an overview of the physics goals, experimental design/status, and
  coordinated theory/modeling of PBEX.

---------------------------------------------------------
Title: Double Coronal Hard and Soft X-Ray Source Observed by RHESSI:
    Evidence for Magnetic Reconnection and Particle Acceleration in
    Solar Flares
Authors: Liu, Wei; Petrosian, Vahé; Dennis, Brian R.; Jiang, Yan Wei
2008ApJ...676..704L    Altcode: 2007arXiv0709.1963L
  We present data analysis and interpretation of an M1.4 class flare
  observed with the Reuven Ramaty High Energy Solar Spectroscopic Imager
  (RHESSI) on 2002 April 30. This event, with its footpoints occulted by
  the solar limb, exhibits a rarely observed, but theoretically expected,
  double-source structure in the corona. The two coronal sources,
  observed over the 6-30 keV range, appear at different altitudes and show
  energy-dependent structures with the higher energy emission being closer
  together. Spectral analysis implies that the emission at higher energies
  in the inner region between the two sources is mainly nonthermal,
  while the emission at lower energies in the outer region is primarily
  thermal. The two sources are both visible for about 12 minutes and have
  similar light curves and power-law spectra above about 20 keV. These
  observations suggest that the magnetic reconnection site lies between
  the two sources. Bidirectional outflows of the released energy in the
  form of turbulence and/or particles from the reconnection site could be
  the source of the observed radiation. The spatially resolved thermal
  emission below about 15 keV, on the other hand, indicates that the
  lower source has a larger emission measure but a lower temperature
  than the upper source. This is likely the result of the differences
  in the magnetic field and plasma density of the two sources.

---------------------------------------------------------
Title: Impact of the Three Gorges Dam water storage on the Yangtze
    River outflow into the East China Sea
Authors: Yan, Xiao-Hai; Jo, Young-Heon; Jiang, Lide; Wan, Zhenwen;
   Liu, W. Timothy; Li, Yan; Zhan, Jiemin; Du, Tao
2008GeoRL..35.5610Y    Altcode:
  The role of the Three Gorges Dam Water Storage (TGDWS) in changing
  salinity in the East China Sea (ECS) near the Yangtze River Estuary
  (YRE) was investigated using a multi-sensor remote sensing technique,
  namely the salt steric height anomaly, calculated from Sea Surface
  Height Anomaly (SSHA) and Sea Surface Temperature (SST) data. The
  patterns of the salt steric height anomaly near the YRE agreed
  well with the in situ Sea Surface Salinity (SSS) measurements. In
  order to examine the changes in stability in the mixed layer near
  the YRE due to TGDWS, the time series of the steric height anomaly
  ratio (R<SUB>s</SUB>') between heat and salt at three locations were
  estimated. The R<SUB>s</SUB>' was strongly associated with a coastal
  upwelling in the ECS, because the reduced freshwater outflow gives rise
  to changes of both mixed layer depth and surface current patterns off
  the YRE.

---------------------------------------------------------
Title: Auroral Processes and Atmospheric Response of Jupiters Around
Red Giants: a Combined Fokker-Planck and Hydrodynamic Approach
Authors: Liu, Wei; Airapetian, V.
2008AAS...21115901L    Altcode:
  A number of Jupiters have recently been detected around giant stars
  including one of the brightest stars in the sky and a well-studied
  K0 giant, β Gem. Giants stars have cool and massive winds that
  may affect the magnetospheres of Jupiters and cause a number of
  observational effects. We show that rescaling of intensities of auroral
  events observed on Jupiter and Saturn can provide an estimate for UV
  emission line intensities that can be observed by largest ground-based
  telescopes and/or space missions. In this study, we model the auroral
  processes and an evaporation scenario caused by injection of energetic
  electrons into the outer atmospheres of massive Jupiters located at
  1 AU from β Gem. We apply a state-of-the-art combined Fokker-Planck
  (Leach &amp; Petrosian 1981) and 1-D hydrodynamic (Mariska et al. 1989)
  code to study, for the first time, the transient effects of injection of
  energetic electrons with energies &gt; 10 keV heating the atmospheres
  due to Coulomb collisions. The energetic particles are produced
  as a result of the interaction between the magnetic fields of the
  stellar wind and the exoplanetary magnetosphere at the magnetopause
  or reconnection in the magnetotail. The combined Fokker-Plank and
  hydrodynamic code is capable of treating particle transport and the
  hydrodynamic atmospheric response in a self-consistent manner, and
  has been successfully used to study chromospheric evaporation during
  solar flares (Liu 2006). We discuss expected fluxes in UV continuum
  and emission lines and new observations that can be used to search
  for evaporating Jupiters around stars with high mass-loss rates.

---------------------------------------------------------
Title: Observation of isolated high-speed auroral streamers and their
    interpretation as optical signatures of Alfvén waves generated by
    bursty bulk flows
Authors: Liu, W. W.; Liang, J.; Donovan, E. F.; Trondsen, T.; Baker,
   G.; Sofko, G.; Jackel, B.; Wang, C. -P.; Mende, S.; Frey, H. U.;
   Angelopoulos, V.
2008GeoRL..35.4104L    Altcode:
  The THEMIS All-Sky Imager at Fort Smith, Canada observed a sudden
  appearance and subsequent evolution of auroral streamers on April 15,
  2006. The event took place in an oval that was optically dark, and
  evolved into a 20-minute period of intense equatorward streaming of
  red aurora. We characterize the incipient event as isolated streamers,
  a phenomenon previously linked with bursty bulk flows in the plasma
  sheet. Thanks to the high time and spatial resolution of THEMIS
  ASI, the observed streamer reveals some detailed features hitherto
  not reported. Aside from their exceptionally high speed and fine
  transient structures, the streamers are found to exhibit an unusual
  convergent motion (equatorward from high latitudes and poleward from
  low latitudes) to form a complete flow channel. Our analysis shows that
  this observation is best explained with a new theory on the origin of
  auroral streamers.

---------------------------------------------------------
Title: Testing the Neupert Effect With Combined Fokker-Planck and
    Hydrodynamic Simulations
Authors: Liu, Wei; Petrosian, Vahe; Holman, Gordon D.; Dennis, Brian
2008cosp...37.1804L    Altcode: 2008cosp.meet.1804L
  The Neupert effect in solar flares is an empirical temporal correlation
  between the microwave or hard X-ray (HXR) flux and the time derivative
  of the soft X-ray (SXR) flux. Such a correlation is expected from a
  simple energy argument and is considered as evidence of chromospheric
  evaporation. However, a quantitative statistical correlation and
  physical connection between these emissions have not been established,
  and in some flares the Neupert effect is not observed. In this study we
  apply a state-of-the-art combined Fokker-Planck (Petrosian et al. 2001)
  and hydrodynamic (Mariska et al. 1989) code to model the atmospheric
  response to collisional heating by accelerated electrons. This code
  treats acceleration and transport of particles and hydrodynamics of
  plasma in a self-consistent manner (Liu 2006). It also evaluates various
  energy contents and thermal SXR and nonthermal HXR bremsstrahlung
  emissions. We confirm the existence of a temporal and statistical
  correlation between the SXR derivative and the HXR flux. In addition,
  we find a statistically more significant and physically more natural
  correlation between the SXR derivative and the thermal energy variation
  rate. The simulation results will be presented and implications for
  the energy release and particle acceleration processes in solar flares
  will be discussed.

---------------------------------------------------------
Title: Measurements of stellar and explosive nuclear astrophysics
    reactions
Authors: Liu, W. P.; Li, Z. H.; Bai, X. X.; Wang, Y. B.; Lian, G.; Guo,
   B.; Su, J.; Zeng, S.; Wang, B. P.; Li, Z. H.; Bai, X. X.; Wang, Y. B.;
   Lian, G.; Guo, B.; Su, J.; Zeng, S.; Wang, B. X.; Yan, S. Q.; Li, Y. J.
2008nuco.confE..11L    Altcode: 2008PoS....53E..11L
  No abstract at ADS

---------------------------------------------------------
Title: Statefinder diagnostic for cosmology with the abnormally
    weighting energy hypothesis
Authors: Liu, Dao-Jun; Liu, Wei-Zhong
2008PhRvD..77b7301L    Altcode: 2007arXiv0711.4854L
  In this paper, we apply the statefinder diagnostic to the cosmology
  with the abnormally weighting energy hypothesis (AWE cosmology),
  in which dark energy in the observational (ordinary matter) frame
  results from the violation of the weak equivalence principle by
  pressureless matter. It is found that there exist closed loops in
  the statefinder plane, which is an interesting characteristic of the
  evolution trajectories of statefinder parameters and can be used to
  distinguish AWE cosmology from other cosmological models.

---------------------------------------------------------
Title: Determination of the substorm initiation region from a major
    conjunction interval of THEMIS satellites
Authors: Lui, A. T. Y.; Angelopoulos, V.; Le Contel, O.; Frey, H.;
   Donovan, E.; Sibeck, D. G.; Liu, W.; Auster, H. U.; Larson, D.; Li,
   X.; Nosé, M.; Fillingim, M. O.
2008JGRA..113.0C04L    Altcode:
  We investigate in detail the time history of substorm disturbances
  in the magnetotail observed during a major tail conjunction of Time
  History of Events and Macroscale Interactions during Substorms (THEMIS)
  satellites on 29 January 2008, 0700-0900 UT. During this interval,
  all THEMIS satellites were closely aligned along the tail axis near
  midnight and were bracketed in local time by GOES 11 and 12. The radial
  distance covered ranges from the geosynchronous altitude to ∼30
  R<SUB>E</SUB> in the tail. This interval consists of three activations
  detected by the THEMIS satellites with good ground all-sky-camera
  observations of auroral activity. The first activation is a small
  substorm with spatially limited disturbance in the tail. The onset
  arc was equatorward of an undisturbed arc. The second activation is
  a moderate size substorm with the onset arc also being equatorward of
  an undisturbed arc. The third activation is an intensification of the
  substorm with its onset indicated by the second activation. The active
  auroral arc for this intensification was near the poleward boundary
  of the auroral oval. Analysis of these observations indicates that the
  first activation is a small substorm initiated in the near-Earth plasma
  sheet and does not involve magnetic reconnection of open magnetic field
  lines. Magnetic reconnection on closed field lines can be ruled out
  for this substorm because it cannot generate the observed high-speed
  plasma flow. The second and third activations are part of a moderate
  size substorm initiated also in the near-Earth plasma sheet, with
  a subsequent substorm intensification involving activity initiated
  tailward of ∼30 R<SUB>E</SUB>. Overall, the time history of substorm
  activity for these two substorms is consistent with the near-Earth
  initiation model.

---------------------------------------------------------
Title: Azimuthal evolution of the aurora in tens of seconds around
    the expansive phase onset
Authors: Liang, J.; Donovan, E.; Liu, W.; Jackel, B.; Spanswick, E.;
   Syrjaesuo, M.; Partamies, N.; Voronkov, I.; Connors, M.; Mende, S.;
   Angelopoulos, V.; Frey, H.; Ge, Y.; Russell, C.; Rae, J.; Mann, I.
2007AGUFMSM21B..03L    Altcode:
  Using data from the implementation phase (2004-2007) of the THEMIS
  All-Sky Imager (ASI) array, we carry out a study of the temporal
  evolution and fine structure of the substorm onset arc in the tens
  of seconds around expansive phase (EP) onset. The continent-wide
  array provides an unprecedented combination of mesoscale imaging
  with relatively high time resolution (3 second cadence), subject to
  the limitations imposed by viewing conditions. We have identified
  eight events in which we have excellent viewing of the onset
  aurora. Our results show the following salient features: 1. The
  initial brightening occurs along an azimuthally extended region of
  the arc. This brightening typically spans ~1 hour of MLT. In cases
  that the camera provides ideal coverage of the arc, the length of
  the brightening does not noticeably change during the first tens of
  seconds of EP. 2. Periodic structures along the arc emerge from ~10 s
  before the EP onset, and significantly brightens within ~10 s after the
  onset, constituting the most unambiguous and prominent feature from the
  optical auroral aspects of the substorm EP onset. Those periodic "wave"
  structure, on its initial formation and brightening, are usually well
  aligned (&lt;15 deg) with the L-shell. The wavelength is about 40-130
  km. These structures either remain stationary or propagate east or west
  during the initial brightening. 3. About 20-30 s after the onset, the
  brightening arc is no longer aligned with the L-shell. Titled structure,
  typically appears as a "bifurcation" of the initial onset arc, starts to
  develop and leads the poleward progression of the substorm auroras. We
  interpret these results as follows. First, the auroral breakup is on
  field lines connected to a region in the CPS that is unstable over an
  extended azimuthal range, but in a limited radial range (the latter
  a conclusion based on contemporaneous riometer observations). Second,
  the instability grows very rapidly across this initially unstable region
  but the region itself does not grow in size for tens of seconds after
  the initial onset. Third, the alignment between the onset-associated
  periodic structures and the magnetic L-shell gives strongly hints
  that they are controlled by near-Earth magnetotail dynamics. If that
  is true, then waves associated with the breakup in the CPS appear to
  have no preferred propagation direction. We finish by discussing the
  implications of these results for substorm onset mechanism theories.

---------------------------------------------------------
Title: Investigation of space and ground low-frequency particle and
    field oscillations during the 23 March 2007 substorm
Authors: Keiling, A.; Angelopoulos, V.; Larson, D.; McFadden, J.;
   Carlson, C.; Bonnell, J. W.; Mozer, F.; Glassmeier, K.; Auster, U.;
   Roux, A.; Le Contel, O.; Mende, S.; Frey, H.; Donovan, E.; Mann, I.;
   Shiokawa, K.; Yumoto, K.; Liu, W.; Li, X.; Parks, G.; Fillingim, M.;
   Lui, A.
2007AGUFMSM22A..03K    Altcode:
  We will report in-situ THEMIS and ground observations and analyses
  of various quantities at and after the onset of the 23 March 2007
  substorm. The spacecraft were located in the Southern Hemisphere
  magnetotail between 8 and 12 RE (radial distance) while their local time
  meridians approximately mapped onto the 210MM magnetometer network. The
  following key results will be presented: (1) Alfven waves (circularly
  polarized) coincided with substorm-related energetic ion injections. (2)
  Strong ion outflow occurred on the same field lines as those carrying
  the Alfven waves and the ion injections. (3) Simultaneously, ground
  magnetometer recorded very large, long-period Pi2 (~135 sec) covering
  low- to high latitudes. (4) Periodic (~135 sec) energetic ion fluxes at
  THEMIS were temporally one-to-one correlated with the ground Pi2, both
  of which showing similar characteristics. Results of all five THEMIS
  spacecraft, THEMIS ground stations, and the 210MM ground stations will
  be included.

---------------------------------------------------------
Title: THEMIS overview, first results and near future
Authors: Angelopoulos, V.; Sibeck, D.; McFadden, J. P.; Carlson, C. W.;
   Larson, D.; Bonnell, J. W.; Mozer, F. S.; Phan, K. H.; Glassmeier,
   K. H.; Auster, U.; Roux, A.; Le Contel, O.; Parks, G.; Fillingim, M.;
   Sigwarth, J.; Mende, S.; Frey, H.; Donovan, E. T.; Russell, C. T.;
   Strangeway, R.; Mann, I.; Rae, J.; Raeder, J.; Ergun, R. E.; Li, X.;
   Liu, W.; Singer, H. J.
2007AGUFMSM13D..01A    Altcode:
  Since its launch, on February 17 2007, the five-satellite (or -probe)
  THEMIS mission has been operating nominally in a 14.6Re apogee
  (low-perigee), near-equatorial orbit. Most instruments have been on
  since March 15. Electric field (EFI) instruments on three probes were
  turned on and operating nominally since mid-June. EFI instruments on
  the other two probes will be deployed in early winter. THEMIS nominal
  science operations commenced on July 1. In its early orbits through
  the dusk magnetotail, the THEMIS probes captured several substorms
  and a small storm at roughly radial alignments along the 20-23MLT
  meridian. The THEMIS first-light (a single orbit in nominal science
  mode during early operations) on March-23, was nature's welcome:
  Two substorm sequences were captured in fast survey mode: particle
  injections and dipolarization signatures were seen propagating from
  one probe to another. An Earthward flow pulse ahead of a predominantly
  duskward flow accompanied a strong field-aligned current pair signature
  at the THEMIS altitude. POLAR VIS,UVI imaged the global evolution of
  the aurora. The THEMIS GBO array captured the salient features of the
  largest intensification of the first substorm, concurrent with the
  most intense particle injection on THEMIS probes. FAST, whose orbit
  passed through the vicinity of the THEMIS footprints 3 min after the
  major intensification, made detailed observations of the field aligned
  currents, arc and outflowing ions. In July and August, the THEMIS probes
  repeatedly encountered the magnetopause and bow shock, observing FTEs,
  LLBL and boundary layers with the three inner, deployed-EFI-bearing
  probes (C,D,E) at 100-500km separations, and the two outer probes
  (B, A) at 5,000-10,000 km separations. Dissecting FTEs, providing
  evidence for simultaneous reconnection at both cusps for northward IMF
  orientation, and directly relating magnetopause and boundary layer
  motion to corresponding ULF waves in the magnetosphere, are some of
  the exciting findings from this dayside interlude. In September 2007
  the probes commenced the series maneuvers that will place them into
  their final orbits with approximately 30Re, 20Re, 12Re (2) and 10Re
  apogees and orbital periods of 4, 2, and 1 days. In these orbits,
  they will be aligned along the Sun-Earth line in Earth's magnetotail
  in January - March 2008. Results obtained demonstrate the high data
  quality and the potential for scientific discovery, particularly when
  combined with existing ancillary data or campaigns.

---------------------------------------------------------
Title: Magnetic Reconnection Site Suggested by a Double Coronal
    X-ray Source Observed by RHESSI
Authors: Liu, W.; Petrosian, V.; Dennis, B. R.; Jiang, Y.
2007AGUFMSH44A1732L    Altcode:
  In the classical reconnection model, magnetic field annihilation in a
  current sheet generates turbulence and outflows of high speed plasmas
  in opposite directions. The turbulence accelerates particles and heats
  the background plasma. Observational signatures, such as radio emission
  and hard and soft X-rays produced by these high-energy particles and
  hot plasmas, are thus expected to show the two oppositely directed
  outflows. However, such observations have rarely been reported in
  the past. In this talk, we present data analysis and interpretation
  of an M1.4-class flare observed with the Reuven Ramaty High Energy
  Solar Spectroscopic Imager (RHESSI) on April 30, 2002. This event,
  with its footpoints occulted by the solar limb, exhibits such a rarely
  observed double-source morphology in the corona over the 6--30~keV
  range. The two coronal sources, appearing at different altitudes, show
  energy-dependent structures with the higher-energy emission being closer
  together. Spectral analysis implies that the emission at higher energies
  in the inner region between the two sources is mainly nonthermal,
  while the emission at lower energies in the outer region is primarily
  thermal. The two sources are both visible for about 12 minutes and
  have similar light curves and power-law spectra (assumed nonthermal)
  above about 20~keV. These observations suggest that the magnetic
  reconnection site lies between the two sources. Bi-directional outflows
  of the released energy in the form of turbulence and/or particle beams
  away from the reconnection site can be the source of the observed
  radiation. The spatially resolved thermal emission below about 15~keV,
  on the other hand, indicates that the lower coronal source has a larger
  emission measure but a lower temperature than the upper source. This
  is likely the result of the different magnetic topologies of the two
  sources. Implications of these results for particle acceleration and
  plasma heating in theoretical flare models will be discussed.

---------------------------------------------------------
Title: Observation and modeling of the injection observed by THEMIS
    and LANL satellites during March 23rd, 2007 substorm event
Authors: Liu, W.; Li, X.; Sarris, T.; Cully, C.; Ergun, R.;
   Angelopoulos, V.; Larson, D.; Keiling, A.; Glassmeier, K.; Auster, U.
2007AGUFMSM23A1179L    Altcode:
  During the first encounter of a substorm on March 23rd, 2007, THEMIS
  constellation observed energetic particle injections and dipolarizations
  in the pre-midnight sector during the onset. Clear injection and
  dipolarization signatures were observed by three probes (A, B and D)
  in the region around 11 Re and 21:00 local time. THEMIS C, which was
  leading in the constellation at 8.3 Re, also observed a good injection
  signature, but the dipolarization is not so clear. From the timing
  based on these observations, a westward expanding ion injection and
  dipolarization front is identified. In combination with the energetic
  particle observations from LANL geosynchronous satellites, the particle
  injection seemed to initiate between LANL-97A (21 LT) and 1989-046 (1
  LT). Ion injection can only be observed west of the center, whereas
  electron injections can only be seen east of the center. This event
  provides us an excellent opportunity to examine the dipolarization and
  particle injection processes beyond geosynchronous orbit. We model this
  injection event by sending an earthward dipolarization-like pulse at 23
  local time and record the injected ions and electrons associated this
  pulse at the various satellite locations. Most of the basic features
  of the injected particles during the main injection are reproduced
  and the timing among satellites is consistent with observations. It
  is suggested from the model that the center of this substorm injection
  was initiated around 23 local time and located beyond 19 Re.

---------------------------------------------------------
Title: Multiscale magnetospheric physics from a simple model of
    self-organized dynamics
Authors: Liu, W.; Charbonneau, P.
2007AGUFMSM54A..05L    Altcode:
  Distributions of geomagnetic indices and aurora have been used to show
  the nonlinear characteristics of magnetospheric dynamics. However,
  the physics underlying these distributions is often not clear. Self
  organization of micro-scale perturbations has been suggested as a
  possibility whereby robust power-law distributions of magnetospheric
  dynamics indices can be produced. Earlier we proposed that some aspects
  of observed substorm distributions can be explained qualitatively by
  a model featuring interactive discrete flux tubes which are used to
  simulate the central plasma sheet dynamics driven by a constant energy
  input. A one- dimensional simulation of the model yielded scale-free
  distributions of auroral activity and quasiperiodic injection. This
  result raised the question what dynamical category the substorm belongs
  to, scale-free or with definite scales. In this talk, we present the
  latest two-dimensional simulation and auroral observational results,
  in an attempt to elucidate the dynamical nature of the substorm.

---------------------------------------------------------
Title: Comparison of Auroral and Inner CPS in situ Measurements
    During an Expansive Phase Onset
Authors: Donovan, E.; Spanswick, E.; Jackel, B.; Trondsen, T.;
   Syrjaesuo, M.; Liang, J.; Liu, W.; Connors, M.; Voronkov, I.; Wild,
   J.; Daum, P.; Mende, S.; Frey, H.; Angelopoulos, V.; Russell, C.;
   McFadden, J.; Glassmeier, K.; Auster, U.; Singer, H.; Sakaguchi, K.;
   Shiokawa, K.; Rostoker, G.; Rae, J.; Mann, I.; Dunlop, M.; Reme, H.;
   Fazakerly, A.
2007AGUFMSM14A..03D    Altcode:
  On March 13, 2007, there was a sequence of auroral and contemporaneous
  magnetotail activity that occurred during a period when the THEMIS
  constellation was in the evening sector inner CPS. The satellites were
  magnetically conjugate to the auroral zone in western Canada. The
  viewing conditions over numerous All-Sky Imagers (ASIs) in Canada
  were excellent. Although the THEMIS satellites were still in
  commissioning phase, the fluxgate magnetometers (FGM) were operating
  on all five satellites during this event, as was the electrostatic
  analyzer instrument on THEMIS A. As well, three GOES satellites were
  collecting geosynchronous magnetic field data over Canada throughout
  the event. Preliminary analysis shows the following. There was an
  onset at roughly 0508 UT either at or earthward of the position of
  THEMIS D (just beyond geosynchronous distance), and then propagated
  outwards over THEMIS B, A, and E in turn. This appears as an outwardly
  propagating decrease in cross-tail current as inferred from FGM;
  however, the current sheet in the vicinity of THEMIS E was increasing
  in strength and/or thinning while the onset was already in progress
  closer to the Earth. ASI, meridian scanning photometer, and riometer
  data show that the onset occurs in the same meridian as the THEMIS
  spacecraft, and allow us to identify the ionospheric signatures
  of the dispersionless injection and the earthward edge of the ion
  plasma sheet. Our conclusions based on this preliminary study are as
  follows: 1) the 0508 UT onset occurred near geosynchronous orbit and
  was not preceded by a fast earthward flow; 2) growth phase continued
  further from the Earth on probes to the East of the onset meridian;
  3) the optical onset, dispersionless injection (from riometers), and
  local decrease in cross tail current all happened at the same time; 4)
  inter-comparison of ground- based and in situ observations highlight
  the importance of the coordinated use of ground and satellite data
  for overcoming azimuthal and radial magnetic projection uncertainties.

---------------------------------------------------------
Title: An XAS study of the structure and thermodynamics of Cu(I)
    chloride complexes in brines up to high temperature (400 °C, 600 bar)
Authors: Brugger, J.; Etschmann, B.; Liu, W.; Testemale, D.; Hazemann,
   J. L.; Emerich, H.; van Beek, W.; Proux, O.
2007GeCoA..71.4920B    Altcode:
  The transport and deposition of copper in saline hydrothermal
  fluids are controlled by the stability of copper(I) complexes with
  ligands such as chloride. Despite their role in the formation of
  most hydrothermal copper deposits, the nature and stability of Cu(I)
  chloride complexes in highly saline brines remains controversial. We
  present new X-ray absorption data ( P = 600 bar, T = 25-400 °C,
  salinity up to 17.2 m Cl), which indicate that the linear CuClx1-x ( x
  = 1, 2) complexes are stable up to supercritical conditions. Distorted
  trigonal planar CuCl32- complexes predominate at room temperature and
  at high salinity (&gt;3 m LiCl): subtle changes in the XANES spectrum
  with increasing salinity may reflect geometric distortions of this
  CuCl32- complex. Similar changes were observed in UV-Vis data [Liu,
  W., Brugger, J., McPhail, D.C., Spiccia, L., 2002. A spectrophotometric
  study of aqueous copper(I) chloride complexes in LiCl solutions between
  100 °C and 250 °C. Geochim. Cosmochim. Acta66, 3615-3633], and were
  erroneously interpreted as a new species, CuCl42-. Our XAS data and
  ab-initio XANES calculations show that this tetrahedral species is
  not present to any significant degree in our solutions. The stability
  of the CuCl32- complexe decreases with increasing temperature; under
  supercritical conditions and in brines under magmatic-hydrothermal
  conditions (e.g., 15.58 m Cl, 400 °C, 600 bar), only the linear Cu(I)
  chloride complexes were observed. This result and the instability of the
  CuCl42- complex are also consistent with the recent ab-initio molecular
  dynamic calculations of Sherman [Sherman D. M.(2007) Complexation
  of Cu <SUP>+</SUP> in hydrothermal NaCl brines: ab-initio molecular
  dynamics and energetics. Geochim. Cosmochim. Acta71, 714-722]. This
  study illustrates the power of the quantitative nature of XANES and
  EXAFS measurements for deciphering the speciation of weak transition
  metal complexes up to magmatic-hydrothermal conditions. The systematic
  XANES data are used to retrieve the formation constant for CuCl32- at
  150 °C, which is in good agreement with the reinterpretation of the
  UV-Vis data of Liu et al. (Liu et al., 2002). At high temperatures
  (≫400 °C), the solubility of chalcopyrite in equilibrium with
  hematite-magnetite-pyrite and K-feldspar-muscovite-quartz calculated
  with the new properties is lower than that calculated using the previous
  model, and the calculated solubilities are at the lower end of the range
  of values measured in brine inclusions from porphyry copper systems.

---------------------------------------------------------
Title: On the equatorward motion and fading of proton aurora during
    substorm growth phase
Authors: Liu, W. W.; Donovan, E. F.; Liang, Jun; Voronkov, Igor;
   Spanswick, Emma; Jayachandran, P. T.; Jackel, Brian; Meurant, Mathieu
2007JGRA..11210217L    Altcode:
  Using 50 high-quality events from the Canadian Auroral Network for
  the OPEN Program Unified Study (CANOPUS) Gillam Meridian Scanning
  Photometer over 10 a (1989-1998), we show that proton aurora in the
  substorm growth phase exhibits a systematic tendency to fade. The
  average pattern of fading consists of a period of relatively stable
  proton aurora brightness and then a period of 15-20 min before onset
  during which the brightness decreases by an average of 15%. We interpret
  the observed proton aurora brightness variation in terms of the magnetic
  field stretching in the near-Earth magnetosphere; in particular, the
  fading is interpreted as a result of the central plasma sheet magnetic
  field lines having stretched to such a degree that the loss cone closing
  effect dominates precipitation due to nonadiabatic proton motions.

---------------------------------------------------------
Title: A MHD mechanism for the generation of the meridional current
    system during substorm expansion phase
Authors: Liang, Jun; Liu, W. W.
2007JGRA..112.9208L    Altcode: 2007JGRA..11209208L
  In this study we propose a MHD mechanism for the generation of the
  meridional current system (MCS) during the substorm expansion phase
  (EP). The upward field-aligned current (FAC) intensifies as the
  dawn-dusk plasma pressure gradient enhances in the Harang region during
  the substorm EP. As a consequence of this intensification, the plasma
  convection pattern changes, with eastward flow accelerations observed
  in both the ionosphere and midmagnetotail during early substorm EP. The
  increasing eastward flow is associated with an inertial current in
  the midtail whose divergence give rise to a downward FAC poleward of
  the upward FAC region, constituting a MCS configuration. Theoretical
  calculations based upon the mechanism shows consistency with many
  observed features of the MCS. We further discuss how the present work
  relates to the large-scale FAC system and the interactions among its
  various components, with a particular emphasis on the MCS contribution
  to the overall substorm current closure.

---------------------------------------------------------
Title: Azimuthal structures of substorm electron injection and their
    signatures in riometer observations
Authors: Liang, Jun; Liu, W. W.; Spanswick, E.; Donovan, E. F.
2007JGRA..112.9209L    Altcode: 2007JGRA..11209209L
  We propose a theoretical model to investigate the effects of the
  curvature/gradient (c/g) drift and the finite azimuthal extent of the
  dipolarization region on the electron injection process associated
  with the substorm dipolarization. We study the azimuthal structure
  of high-energy (&gt;30 keV) electron precipitation flux and compare
  the result with riometer observations. We are able to reproduce
  three basic archetypes of riometer responses to substorms, namely,
  the spike, dispersionless injection, and dispersed injection events
  catalogued in previous observations. The electron injection near
  the duskward edge of the dipolarization region is most subject to
  azimuthal c/g drift loss, appearing in riometer observations as the
  “spike” feature. The “dispersionless injection” response is
  seen inside the dipolarization region but some distance away from
  its western border: or, alternatively, when the substorm has a rapid
  westward expansion, so that the gain and loss of electrons from the
  duskside and dawnside of a dipolarizing flux tube roughly balance. The
  “dispersed injection” feature is seen east of the dipolarization
  region. Our theory successfully explains the statistical differences
  in terms of magnetic local time location and peak intensity between
  spikes and injection events. Through the substorm event on 23 May 1998
  we demonstrate that our theoretical predictions of riometer responses
  are very consistent with the observations. We highlight the potential
  of riometers in resolving the azimuthal extent and evolution of the
  dipolarization region, which provides a new ground-based technique of
  remote sensing the substorm process.

---------------------------------------------------------
Title: Axisymmetric numerical and analytical studies of the
    magnetorotational instability in a magnetized Taylor-Couette flow
Authors: Liu, Wei
2007PhDT........19L    Altcode:
  The magnetorotational instability (MRI) is probably the main cause
  of turbulence and accretion in sufficiently ionized astrophysical
  disks. However, despite much theoretical and computational work,
  the nonlinear saturation of MRI is imperfectly understood. In Chap. 2
  and Chap. 3 of this thesis we present non-ideal magnetohydrodynamic
  simulations of the Princeton MRI experiment. In vertically infinite or
  periodic cylinders, MRI saturates in a resistive current-sheet with a
  significant reduction of the mean shear, and with poloidal circulation
  scaling as the square root of resistivity. Angular momentum transport
  scales as the reciprocal square root of viscosity but only weakly
  depends on resistivity. For finite cylinders with insulating end caps,
  a method for implementing the fully insulating boundary condition is
  introduced. MRI grows with a clear linear phase from small amplitudes
  at rates in good agreement with linear analysis. In the final state
  one inflowing "jet" opposite to the usual Ekman "jet" is found near
  the inner cylinder. The MRI enhances the angular momentum transport
  at saturation. Under proper conditions, our experimental facility
  is a good platform to show that MRI could be suppressed by a strong
  magnetic field. <P />Recently, Hollerbach and Rüdiger have reported
  that MRI modes may grow at much reduced magnetic Reynolds number (
  Re m ) and Lundquist number S in the presence of a helical background
  field, a current-free combination of axial and toroidal field. We
  have investigated these helical MRI modes in Chap. 4 and Chap. 5. In
  vertically infinite or periodic cylinders, resistive HMRI is a weakly
  destabilized hydrodynamic inertial oscillation propagating axially
  along the background Poynting flux. Growth rates are small, however,
  and require large axial currents. Furthermore, finite cylinders
  with insulating endcaps were shown to reduce the growth rate and to
  stabilize highly resistive, inviscid flows entirely, and the new mode
  is stable in Keplerian flow profiles regardless of end conditions. We
  also numerically investigate a traveling wave pattern observed in
  experimental magnetized Taylor-Couette flow at low magnetic Reynolds
  number. By accurately modeling viscous and magnetic boundaries in all
  directions, we reproduce the experimentally measured wave patterns
  and their amplitudes. Contrary to previous claims, the waves are
  shown to be transiently amplified disturbances launched by viscous
  boundary layers rather than globally unstable magnetorotational
  modes. <P />The experiment is complicated by the extremely large
  Reynolds number and by Ekman circulation and Stewartson layers,
  even though the experimental apparatus has been designed to minimize
  the circulation ( e.g. by the use of independently controlled split
  endcaps). Understanding the role of the boundary layers is critical to
  this research. In Chap. 6 the magnetic field is found to inhibit the
  Ekman suction. While we quantitatively confirmed the conclusions of
  Gilman et al , the finite differential rotation cannot be neglected
  and modifies the linear Ekman layer. The width of the Ekman layer
  is reduced with increased magnetic field normal to the end plate. A
  uniformly-rotating region forms near the outer cylinder. The Stewartson
  layer penetrates deeper into the fluid with larger Reynolds number and
  stronger magnetic field. Furthermore a strong magnetic field leads to
  a steady Stewartson layer, at least in axisymmetric configuration.

---------------------------------------------------------
Title: Traveling waves in a magnetized Taylor-Couette flow
Authors: Liu, Wei; Goodman, Jeremy; Ji, Hantao
2007PhRvE..76a6310L    Altcode: 2007astro.ph..3525L
  We investigate numerically a traveling wave pattern observed in
  experimental magnetized Taylor-Couette flow at low magnetic Reynolds
  number. By accurately modeling viscous and magnetic boundaries in all
  directions, we reproduce the experimentally measured wave patterns
  and their amplitudes. Contrary to previous claims, the waves are shown
  to be transiently amplified disturbances launched by viscous boundary
  layers, rather than globally unstable magnetorotational modes.

---------------------------------------------------------
Title: Polar cap potential saturation: An energy conservation
    perspective
Authors: Liu, W. William
2007JGRA..112.7210L    Altcode: 2007JGRA..11207210L
  In the long run, energy entering the magnetosphere from the solar
  wind must be balanced by energy dissipation in or escape from the
  system. It then follows that the Joule heating rate in the ionosphere
  statistically should be bounded from the upside by the solar wind
  energy input function (e.g., the Perrault-Akasofu parameter). We
  show that this energy constraint, coupled with some observationally
  motivated assumptions about the behavior of the auroral oval under
  escalating solar wind conditions, leads to the prediction of polar
  cap potential saturation.

---------------------------------------------------------
Title: In search of the near-Earth neutral line: How much a role
    can ground-based observations play?
Authors: Liu, W.; Liang, J.; Voronkov, I.; Spanswick, E.; Jackel,
   B.; Jayachandran, P.
2007AGUSMSM22A..03L    Altcode:
  The launch of THEMIS has raised the expectation that new progress
  will be made on the assessment and evaluation of competing substorm
  models. While the THEMIS spacecraft will offer much improved capability
  to delimit and localize substorm triggers, they will measure primarily
  "perpendicular" signatures of a near-Earth neutral line (e.g.,
  BBFs). For "parallel" signatures of NENL, ground-based observations
  should prove more advantageous. However, there has been relatively
  little attention to what effects can be uniquely attributed to a
  would-be NENL, as a given auroral signature can receive more than one
  theoretical explanations. There is therefore a need to systematize
  and quantify our approach to the use of ground-based observations to
  detect, constrain, and characterize NENL. In this talk, we will review
  the ground-based observations that will be made in conjunction with
  THEMIS during its tail operation, identify some candidate signatures
  that might be related to the NENL, and outline steps to evolve this
  line of research through focused theory and modeling efforts.

---------------------------------------------------------
Title: Characteristics of Solar Flare Hard X-ray Emissions:
    Observations and Models
Authors: Liu, Wei
2007AAS...210.6801L    Altcode: 2007BAAS...39..175L
  The main theme of this dissertation is the investigation of the
  physics of acceleration and transport of particles in solar flares
  and their radiative signatures. <P />The observational studies, using
  hard X-rays (HXRs) observed by RHESSI, concentrate on four flares,
  which support the classical magnetic reconnection model of flares in
  various ways. In the 11/03/2003 X3.9 flare, there is an upward motion
  of the loop-top source, accompanied by a systematic increase in the
  separation of the foot-point sources at a comparable speed. This is
  consistent with the reconnection model with an inverted-Y geometry. The
  04/30/2002 M1.3 event exhibits rarely observed two coronal sources,
  with very similar spectra and their higher-energy emission being
  close together. This suggests that reconnection occurs between the two
  sources. In the 10/29/2003 X10 flare, the logarithmic total HXR flux
  of the two foot-points correlates with their mean magnetic field. The
  foot-points show asymmetric HXR fluxes, qualitatively consistent
  with the magnetic mirroring effect. The 11/13/2003 M1.7 flare reveals
  evidence of chromospheric evaporation directly imaged by RHESSI for the
  first time. The emission centroids move toward the loop-top, indicating
  a density increase in the loop. <P />The theoretical modeling of this
  work combines the Stanford stochastic acceleration model with the NRL
  hydrodynamic model to study the interplay of the particle acceleration,
  transport, and radiation effects and the atmospheric response to the
  energy deposition by electrons. I find that low-energy electrons in
  the quasi-thermal portion of the spectrum affects the hydrodynamics
  by producing more heating in the corona than the previous models
  that used a power-law spectrum with a low-energy cutoff. The Neupert
  effect is found to be present and effects of suppression of thermal
  conduction are tested in the presence of hydrodynamic flows. <P />I
  gratefully thank my adviser, Prof. Vahe' Petrosian, my collaborators,
  and funding support from NSF and NASA.

---------------------------------------------------------
Title: Remote-sensing magnetospheric dynamics with riometers:
    Observation and theory
Authors: Liu, W. W.; Liang, J.; Spanswick, E.; Donovan, E. F.
2007JGRA..112.5214L    Altcode: 2007JGRA..11205214L
  The importance of monitoring particle injection into the inner
  magnetosphere from the plasma sheet is exceeded perhaps only by its
  difficulty. The recent progress in using ground-based riometer data
  [e.g., Spanswick et al., 2007] to detect by proxy particle injection
  has raised much hope that this important aspect of substorms can be
  more consistently monitored. In this paper we develop a theoretical
  model for explaining the observed dispersionless injection events
  reported by Spanswick et al. The substorm event on 3 October 1998 is
  analyzed to give the empirical context for riometer responses during a
  typical substorm. Our simulation shows that riometer electrons produce
  a clean and strong signal that can be uniquely and easily related to
  magnetic field dipolarization that normally gives rise to injection.

---------------------------------------------------------
Title: Global auroral imaging in the ILWS era
Authors: Donovan, E.; Trondsen, T.; Spann, J.; Liu, W.; Spanswick, E.;
   Lester, M.; Tu, C. -Y.; Ridley, A.; Henderson, M.; Immel, T.; Mende,
   S.; Bonnell, J.; Syrjäsuo, M.; Sofko, G.; Cogger, L.; Murphree, J.;
   Jayachandran, P. T.; Pulkkinen, T.; Rankin, R.; Sigwarth, J.
2007AdSpR..40..409D    Altcode:
  The overarching objective of the ILWS Geospace program is to facilitate
  system level science. This demands synoptic observations such as global
  auroral imaging. At present, there is no funded mission during ILWS
  that incorporates a global auroral imager. The imaging community
  needs to move now to address this important gap. While doing so,
  it is interesting to take stock of global auroral observations that
  have not been achieved, or that have been achieved only to a limited
  extent. These include simultaneous imaging across all relevant
  scales, spectral resolution of sufficient quality to allow for
  global maps of characteristic energy and energy flux of precipitating
  electrons, continuous global auroral imaging for time periods spanning
  long-duration geomagnetic events, systematic interhemispheric conjugate
  observations, auroral observations magnetically conjugate to in situ
  measurements, and automatic classification of auroral images. These
  observations can be achieved within the next decade. If they are,
  then they will facilitate exciting new science.

---------------------------------------------------------
Title: Evolution of electron energy spectrum during solar flares
Authors: Liu, W. J.; Chen, P. F.; Fang, C.; Ding, M. D.
2007AdSpR..39.1394L    Altcode:
  Particle acceleration by direct current electric field in the current
  sheet has been extensively studied, in which an electric and a magnetic
  field are generally prescribed, and a power law distribution of the
  electron energy is obtained. Based on MHD numerical simulations of
  flares, this paper aims at investigating the time evolution of the
  electron energy spectrum during solar flares. It turns out that the
  model reproduces the soft-hard-hard spectral feature which was observed
  in some flares.

---------------------------------------------------------
Title: Determination of astrophysical <SUP>11</SUP>C(p,
    γ)<SUP>12</SUP>N reaction rate from the asymptotic normalization
    coefficients of <SUP>12</SUP>B →<SUP>11</SUP>B + n
Authors: Guo, B.; Li, Z. H.; Liu, W. P.; Bai, X. X.
2007JPhG...34..103G    Altcode:
  The squares of the neutron asymptotic normalization coefficient (ANC)
  for the virtual decay <SUP>12</SUP>B →<SUP>11</SUP>B + n are extracted
  to be 1.20 ± 0.26, 0.354 ± 0.107 and 1.98 ± 0.35 fm<SUP>-1</SUP> from
  the angular distributions of the <SUP>11</SUP>B(d, p)<SUP>12</SUP>B
  reaction leading to the ground, first and second excited states of
  <SUP>12</SUP>B respectively, using the Johnson Soper approach. According
  to charge symmetry of strong interaction, the square of proton ANC
  of virtual decay <SUP>12</SUP>N →<SUP>11</SUP>C + p is determined
  to be 1.63 ± 0.35 fm<SUP>-1</SUP> and then utilized to calculate the
  astrophysical S-factor and the rate of the direct capture contribution
  in the <SUP>11</SUP>C(p, γ)<SUP>12</SUP>N reaction. The astrophysical
  S-factor at zero energy for the direct capture, S(0), is derived to be
  0.088 ± 0.019 keV b. An evaluated S(0) of 0.092 ± 0.009 keV b is then
  given by using the present and pre-existing experimental results. In
  addition, the proton widths of the first and second excited states of
  <SUP>12</SUP>N are derived to be 0.91 ± 0.29 and 99 ± 20 keV from
  the neutron ANCs of <SUP>12</SUP>B and used to compute the contribution
  from the first two resonances of <SUP>12</SUP>N, respectively. We have
  also calculated the contribution from the interference effect between
  the direct capture and the second resonance.

---------------------------------------------------------
Title: Magnetic reconnection configurations and particle acceleration
    in solar flares
Authors: Chen, P. F.; Liu, W. J.; Fang, C.
2007AdSpR..39.1421C    Altcode:
  Numerical simulations of two types of flares indicate that magnetic
  reconnection can provide environments favorable for various particle
  acceleration mechanisms to work. This paper reviews recent test particle
  simulations of DC electric field mechanism, and discusses how the flare
  particles can escape into the interplanetary space under different
  magnetic configurations.

---------------------------------------------------------
Title: Laboratory Spectroscopy of Planetary Molecules
Authors: Brown, L.; Drouin, B.; Miller, C.; Pearson, J.; Orton,
   G.; Toth, R.; Benner, C.; Devi, M.; Blake, T.; Masiello, T.; Sams,
   R.; Butler, R.; Champion, J.; Chelin, P.; Dehayem, A.; Kleiner, I.;
   Orphal, J.; Sagui, L.; Gamache, R.; Humphrey, C.; Liu, W.; Predoi
2007plat.work...19B    Altcode:
  An international team of laboratory spectroscopists are working
  in concert to support remote sensing of planetary atmospheres and
  Titan. An overview of high resolution laboratory investigations will
  be presented for spectral bands from the rotational wavelengths into
  the near infrared. The studies include measurements and theoretical
  analyses of the line positions, intensities and/or broadening
  coefficients needed to improve the spectroscopic databases required
  for planetary applications. The molecular studies include water (H2O)
  broadened by carbon dioxide in the far- and mid-infrared; positions,
  intensities, broadening and line mixing of carbon dioxide (CO2) in the
  near-IR; broadening and line mixing of methane in the mid- and near-IR;
  frequencies of methyl cyanide (CH3CN) in the rotational region and line
  positions, intensities and nitrogen broadening of methyl cyanide in
  the low fundamental bands; global theoretical modeling of the phosphine
  (PH3) parameters; and frequencies of acetaldehyde (CH3CHO), methylamine
  (CH3NH2) and deuterated acetylene (HCCD, DCCD) in the rotational region.

---------------------------------------------------------
Title: Characteristics of Solar Flare Hard X-ray Emissions:
    Observations and Models
Authors: Liu, Wei
2006PhDT........35L    Altcode:
  The main theme of this thesis is the investigation of the physics of
  acceleration and transport of particles in solar flares, and their
  thermal and nonthermal radiative signatures. <P />The observational
  studies, using hard X-rays (HXRs) observed by the RHESSI mission,
  concentrate on four flares, which support the classical magnetic
  reconnection model of solar flares in various ways. In the X3.9 flare
  occurring on 11/03/2003, there is a monotonic upward motion of the loop
  top (LT) source accompanied by a systematic increase in the separation
  of the footpoint (FP) sources at a comparable speed. This is consistent
  with the reconnection model with an inverted-Y geometry. The 04/30/2002
  event exhibits rarely observed two coronal sources. The two sources
  (with almost identical spectra) show energy-dependent structures,
  with higher-energy emission being close together. This suggests that
  reconnection takes place within the region between the sources. In
  the 10/29/2003 X10 flare, the logarithmic total HXR flux of the FPs
  correlates with the mean magnetic field. The two FPs show asymmetric HXR
  fluxes, which is qualitatively consistent with the magnetic mirroring
  effect. The M1.7 flare on 11/13/2003 reveals evidence of evaporation
  directly imaged by RHESSI for the first time, in which emission from the
  legs of the loop appears at intermediate energies. The emission centroid
  moves toward the LT as time proceeds, indicating an increase of density
  in the loop. <P />The theoretical modeling of this work combines the
  stochastic acceleration model with the NRL hydrodynamic model to study
  the interplay of the particle acceleration, transport, and radiation
  effects and the atmospheric response to the energy deposition by
  nonthermal electrons. <P />We find that low-energy electrons in the
  quasi-thermal portion of the spectrum affects the hydrodynamics by
  producing more heating in the corona than the previous models that
  used a power-law spectrum with a low-energy cutoff. <P />The Neupert
  effect is found to be present and effects of suppression of conduction
  are tested in the presence of hydrodynamic flows.

---------------------------------------------------------
Title: Magnetorotational instability and angular momentum transport
    in magnetized Taylor- Couette flows
Authors: Liu, W.; Goodman, J.; Ji, H.
2006AGUFMGP43A1029L    Altcode:
  The magnetorotational instability (MRI) is probably the main cause
  of turbulence and accretion in sufficiently ionized astrophysical
  disks. Despite much theoretical and computational work, however,
  nonlinear MRI is imperfectly understood. We present non-ideal
  magnetohydrodynamic simulations of MRI in the geometry of the Princeton
  MRI experiment. MRI saturates in a resistive current-sheet with
  significant reduction of the mean shear, and with poloidal circulation
  scaling as the square root of resistivity. Angular momentum transport
  scales as the reciprocal square root of viscosity but hardly depends on
  resistivity [1]. Separately, we have studied MRI in the presence of a a
  current-free combination of toroidal and axial magnetic field. The new
  mode (HMRI) persists to smaller magnetic Reynolds number and Lundquist
  number than standard MRI, which relies on axial field alone. This
  would seem to make HMRI attractive for experiments and perhaps for
  application to resistive astrophysical disks. In vertically infinite or
  periodic cylinders, resistive HMRI is a weakly destabilized hydrodynamic
  inertial oscillation propagating axially along the background Poynting
  flux [2]. Growth rates are small, however, and require large axial
  currents. Furthermore, highly resistive HMRI is stabilized in finite
  cylinders with insulating endcaps, and also in keplerian flow profiles
  regardless of end conditions. In both of these studies, comparison of
  models and measurements is used to validate our theoretical tools,
  which we will apply to nonlinear saturation of resistive MRI in
  astrophysical systems. Theoretical modeling has already played a major
  role in the design of the MRI experiment, and the physics of these
  modes may be of interest for fluid dynamics and geophysics as well
  as astrophysics. {[1]} Wei Liu, Jeremy Goodman and Hantao Ji, ApJ,
  643, 306. {[2]} Wei Liu, Jeremy Goodman, Hantao Ji and Isom Herron,
  submitted to PRE. Supported by DoE, NASA and NSF.

---------------------------------------------------------
Title: High-energy electron injection associated with substorm
dipolarization: Models and comparison with riometer observations
Authors: Liang, J.; Liu, W.; Donovan, E. F.; Spanswick, E.
2006AGUFMSM51B1404L    Altcode:
  Energetic particle injection has long been recognized as a common
  signature of magnetospheric substorms. In this study the injection
  process is modeled via the Fokker-Planck equation wherein the convective
  transport terms are associated with adiabatic changes imposed on the
  distribution of high-energy electrons by a rapid- varying magnetic
  fields simulating the substorm dipolarization. The model results are
  compared with the riometer observations of ionospheric absorption of
  cosmic radio noises, which is known to respond to the precipitation
  of magnetospheric electrons with energy &gt;30 keV. In particular, our
  model is capable of reproducing the riometer dispersionless injection
  event defined by Spanswick [2006]. The interrelationship between the
  riometer injections and observations from other instruments prescribed
  by our theoretic framework is discussed. We suggest the possibility
  that the riometer data become one of the most accurate methods to
  pinpoint and quantify the magnetospheric dynamics underlying a substorm.

---------------------------------------------------------
Title: Helical magnetorotational instability in magnetized
    Taylor-Couette flow
Authors: Liu, Wei; Goodman, Jeremy; Herron, Isom; Ji, Hantao
2006PhRvE..74e6302L    Altcode: 2006astro.ph..6125L
  Hollerbach and Rüdiger have reported a new type of magnetorotational
  instability (MRI) in magnetized Taylor-Couette flow in the presence of
  combined axial and azimuthal magnetic fields. The salient advantage of
  this “helical” MRI (HMRI) is that marginal instability occurs at
  arbitrarily low magnetic Reynolds and Lundquist numbers, suggesting
  that HMRI might be easier to realize than standard MRI (axial field
  only), and that it might be relevant to cooler astrophysical disks,
  especially those around protostars, which may be quite resistive. We
  confirm previous results for marginal stability and calculate HMRI
  growth rates. We show that in the resistive limit, HMRI is a weakly
  destabilized inertial oscillation propagating in a unique direction
  along the axis. But we report other features of HMRI that make it less
  attractive for experiments and for resistive astrophysical disks. Large
  axial currents are required. More fundamentally, instability of highly
  resistive flow is peculiar to infinitely long or periodic cylinders:
  finite cylinders with insulating endcaps are shown to be stable
  in this limit, at least if viscosity is neglected. Also, Keplerian
  rotation profiles are stable in the resistive limit regardless of
  axial boundary conditions. Nevertheless, the addition of a toroidal
  field lowers thresholds for instability even in finite cylinders.

---------------------------------------------------------
Title: Indirect measurements of nuclear astrophysics reactions at CIAE
Authors: Liu, Wei-Ping; Li, Zhi-Hong; Bai, Xi-Xiang; Wang, You-Bao;
   Lian, Gang; Guo, Bing; Zeng, Sheng; Yan, Sheng-Quan; Wang, Bao-Xiang;
   Su, Jun; Shu, Neng-Chuan; Chen, Yong-Shou
2006AIPC..865..358L    Altcode:
  This paper described the nuclear astrophysical studies using the
  unstable ion beam facility GIRAFFE, by indirect measurements. We
  measured the angular distributions for some single proton or
  neutron transfer reactions, such as <SUP>7</SUP>Be(d,n)<SUP>8</SUP>B,
  <SUP>11</SUP>C(d,n)<SUP>12</SUP>N, <SUP>8</SUP>Li(d,n)<SUP>9</SUP>Be,
  <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li and <SUP>13</SUP>N(d,n)<SUP>14</SUP>O
  in inverse kinematics, and derived the astrophysical S-factors
  or reaction rates of <SUP>7</SUP>Be(p,γ)<SUP>8</SUP>B,
  <SUP>11</SUP>C(p,γ)<SUP>12</SUP>N, <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li,
  <SUP>13</SUP>N(p,γ)<SUP>14</SUP>O by asymptotic normalization
  coefficient, spectroscopic factor, and R-matrix approach at
  astrophysically relevant energies.

---------------------------------------------------------
Title: RHESSI Observation of Chromospheric Evaporation
Authors: Liu, Wei; Liu, Siming; Jiang, Yan Wei; Petrosian, Vahé
2006ApJ...649.1124L    Altcode: 2006astro.ph..3510L
  We present analyses of the spatial and spectral evolution of hard
  X-ray emission observed by RHESSI during the impulsive phase of an
  M1.7 flare on 2003 November 13. In general, as expected, the loop top
  (LT) source dominates at low energies, while the footpoint (FP) sources
  dominate the high-energy emission. At intermediate energies, both the
  LT and FPs may be seen, but during certain intervals emission from the
  legs of the loop dominates, in contrast to the commonly observed LT
  and FP emission. The hard X-ray emission tends to rise above the FPs
  and eventually merge into a single LT source. This evolution starts
  at low energies and proceeds to higher energies. The spectrum of
  the resultant LT source becomes more and more dominated by a thermal
  component with an increasing emission measure as the flare proceeds. The
  soft and hard X-rays show a Neupert-type behavior. With a nonthermal
  bremsstrahlung model, the brightness profile along the loop is used to
  determine the density profile and its evolution, which reveals a gradual
  increase of the gas density in the loop. These results are evidence
  for chromospheric evaporation and are consistent with the qualitative
  features of hydrodynamic simulations of this phenomenon. However, some
  observed source morphologies and their evolution cannot be accounted
  for by previous simulations. Therefore, simulations with more realistic
  physical conditions are required to explain the results and the particle
  acceleration and plasma heating processes.

---------------------------------------------------------
Title: Heat flux in magnetospheric convection: A calculation based
    on adiabatic drift theory
Authors: Liu, W. William
2006GeoRL..3319104L    Altcode:
  Empiric evidence and theoretical argument indicate that magnetospheric
  convection is globally sub-adiabatic. Reconciliation of the
  sub-adiabaticity with the underlying adiabatic particle drifts is a
  problem that has not been conclusively demonstrated. In this paper,
  through an ensemble average, we show that the Rice Convection Model
  contains a heat flux due to thermal inequilibrium between two adjacent
  flux tubes of equal volume. The averaged theory is based on field
  variables obeying a set of partial differential equations (Eulerian
  formulation), instead of conservative variables advecting with fluid
  elements (Langrangian formulation). We apply the theory to investigate
  a one-dimensional case of subadiabatic variation of thermodynamic
  properties in the plasma sheet.

---------------------------------------------------------
Title: Energy avalanches in the central plasma sheet
Authors: Liu, W. W.; Charbonneau, P.; Thibault, K.; Morales, L.
2006GeoRL..3319106L    Altcode:
  The central plasma sheet (CPS) is simulated as a 1D cellular
  automaton. The system is driven deterministically and globally by
  a spatially non-uniform energy loading (convection). Each node (a
  flux tube) evolves until one of two local instability criteria is
  exceeded. The unstable node releases a small amount of energy to the
  ionosphere and another small amount is distributed to its neighboring
  nodes. The partition between the two modes of energy distribution
  is the only random factor in the model. The energy redistribution
  relaxes the node deterministically to a stable state. The simulation
  suggests that a central plasma sheet driven in the above manner is
  in a self-organized critical state, with energy avalanches obeying
  a scale-free distribution. The avalanches, however, co-exist with
  quasi-periodic intermittencies manifested in ring-current injection,
  which is correlated with strong CPS avalanches, and tailward energy
  ejection, which shows no apparent correlation in this aspect.

---------------------------------------------------------
Title: Magnetorotational instability in magnetized Taylor-Couette
    flows
Authors: Liu, Wei; Goodman, Jeremy; Ji, Hantao
2006APS..DPPBP1100L    Altcode:
  We present non-ideal magnetohydrodynamic simulations of MRI in the
  geometry of the Princeton MRI experiment. MRI saturates in a resistive
  current-sheet with significant reduction of the mean shear, and with
  poloidal circulation scaling as the square root of resistivity. Angular
  momentum transport scales as the reciprocal square root of viscosity but
  hardly depends on resistivity. Separately, we have studied MRI in the
  presence of a current-free combination of toroidal and axial magnetic
  field. The new mode (HMRI) persists to smaller magnetic Reynolds number
  and Lundquist number than standard MRI, which relies on axial field
  alone. In vertically infinite or periodic cylinders, resistive HMRI is
  a weakly destabilized hydrodynamic inertial oscillation propagating
  axially along the background Poynting flux. Growth rates are small,
  however, and require large axial currents. Furthermore, highly resistive
  HMRI is stabilized in finite cylinders with insulating endcaps, and also
  in keplerian flow profiles regardless of end conditions. Comparison of
  models and measurements is used to validate our theoretical tools, which
  we will apply to nonlinear saturation of resistive MRI in astrophysical
  systems. Theoretical modeling has already played a major role in the
  design of the MRI experiment, and the physics of these modes may be
  of interest for fluid dynamics and geophysics as well as astrophysics

---------------------------------------------------------
Title: An efficient control of ultrashort laser filament location
    in air for the purpose of remote sensing
Authors: Liu, W.; Théberge, F.; Daigle, J. -F.; Simard, P. T.;
   Sarifi, S. M.; Kamali, Y.; Xu, H. L.; Chin, S. L.
2006ApPhB..85...55L    Altcode:
  The unavoidable hot spots in a practical terawatt level laser pulse
  will self-focus in air at a short distance. The short distance
  cannot be changed significantly by only controlling the chirp
  or divergence. We overcome such early self-focusing by using a
  telescope, which enlarges the diameter of the beam, thus that of the
  hot spots. The telescope’s effective focal length is much shorter
  than the self-focusing distance of both the enlarged beam and the hot
  spots. Then, the resulting filaments merge into the geometrical focus
  whose position is controllable by the telescope. This technique also
  minimizes the generation of white light.

---------------------------------------------------------
Title: N13(d,n)O14 reaction and the astrophysical N13(p,γ)O14
    reaction rate
Authors: Li, Z. H.; Guo, B.; Yan, S. Q.; Lian, G.; Bai, X. X.; Wang,
   Y. B.; Zeng, S.; Su, J.; Wang, B. X.; Liu, W. P.; Shu, N. C.; Chen,
   Y. S.; Chang, H. W.; Jiang, L. Y.
2006PhRvC..74c5801L    Altcode: 2009arXiv0903.3094L
  N13(p,γ)O14 is one of the key reactions in the hot CNO cycle which
  occurs at stellar temperatures around T<SUB>9</SUB>⩾0.1. Up to now,
  some uncertainties still exist for the direct capture component in
  this reaction, thus an independent measurement is of importance. In
  present work, the angular distribution of the N13(d,n)O14 reaction at
  E<SUB>c.m.</SUB>=8.9 MeV has been measured in inverse kinematics, for
  the first time. Based on the distorted-wave Born approximation (DWBA)
  analysis, the nuclear asymptotic normalization coefficient (ANC),
  C<SUB>1,1/2</SUB><SUP><SUP>14</SUP>O</SUP>, for the ground state of
  O14 →N13 + p is derived to be 5.42±0.48 fm<SUP>-1/2</SUP>. The
  N13(p,γ)O14 reaction is analyzed with the R-matrix approach, its
  astrophysical S factors and reaction rates at energies of astrophysical
  relevance are then determined with the ANC. The implications of the
  present reaction rates on the evolution of novae are then discussed
  with the reaction network calculations.

---------------------------------------------------------
Title: Thermal equation of state of (Mg <SUB>0.9</SUB>Fe
    <SUB>0.1</SUB>) <SUB>2</SUB>SiO <SUB>4</SUB> olivine
Authors: Liu, Wei; Li, Baosheng
2006PEPI..157..188L    Altcode:
  In situ synchrotron X-ray diffraction measurements have been carried
  out on San Carlos olivine (Mg <SUB>0.9</SUB>Fe <SUB>0.1</SUB>)
  <SUB>2</SUB>SiO <SUB>4</SUB> up to 8 GPa and 1073 K. Data analysis
  using the high-temperature Birch-Murnaghan (HTBM) equation of
  state (EoS) yields the temperature derivative of the bulk modulus
  (∂ K<SUB>T</SUB>/∂ T) <SUB>P</SUB> = -0.019 ± 0.002 GPa K
  <SUP>-1</SUP>. The thermal pressure (TH) approach gives αK<SUB>T</SUB>
  = 4.08 ± 0.10 × 10 <SUP>-3</SUP> GPa K <SUP>-1</SUP>, from which (∂
  K<SUB>T</SUB>/∂ T) <SUB>P</SUB> = -0.019 ± 0.001 GPa K <SUP>-1</SUP>
  is derived. Fitting the present data to the Mie-Grüneisen-Debye (MGD)
  formalism, the Grüneisen parameter at ambient conditions γ<SUB>0</SUB>
  is constrained to be 1.14 ± 0.02 with fixed volume dependence q =
  1. Combining the present data with previous results on iron-bearing
  olivine and fitting to MGD EoS, we obtain γ<SUB>0</SUB> = 1.11 ±
  0.01 and q = 0.54 ± 0.36. In this study the thermoelastic parameters
  obtained from various approaches are in good agreement with one another
  and previous results.

---------------------------------------------------------
Title: SHRIMP zircon geochronological constraints on a Pan-African
    orogeny in the Yadong Area, Southern Tibet
Authors: Liu, W. C.; Zhou, Z. G.; Zhang, X. X.; Zhao, X. G.
2006GeCAS..70Q.365L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Copper(I) in brines up to supercritical conditions
Authors: Brugger, J.; Liu, W.; Hazemann, J. -L.; Etschmann, B.;
   Testemale, D.
2006GeCAS..70R..70B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Speciation of Fe<SUP>II</SUP> in hydrothermal saline brines
    by X-ray absorption techniques
Authors: Testemale, D.; Brugger, J.; Liu, W.; Etschmann, B.; Hazemann,
   J. -L.
2006GeCAS..70R.646T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A XANES study of Zn and Fe(II) chloride complexes in
    hypersaline brines
Authors: Liu, W.; Etschmann, B.; Foran, G.; Shelley, M.; Brugger, J.
2006GeCAS..70R.364L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Rossby Wave and Eddies in the North Pacific Subtropical
    Countercurrent
Authors: Liu, Q.; Li, L.; Liu, W.
2006ESASP.614E..28L    Altcode:
  In the North Pacific, Subtropical Countercurrent (STCC) has two
  branches: one located in the Northwestern Pacific and the other is to
  the west of Hawaii Islands. In both STCC regions, the SSHA exhibits
  remarkable oscillations with period of 80-210 days, corresponding to
  westward propagation of free Rossby waves. The larger amplitude of
  those Rossby waves in the west end of the Northwest STCC seemingly
  due to stronger baroclinic instability. In addition, there is also a
  vortex pair with the orbital period of 10-11days and the radius of
  58-68km to the west of Hawaii Islands. The average T/P SSHA shows
  general distribution of the vortices in a region broader than that
  covered by the trajectories. The T/P SSHA clearly demonstrates two
  symmetrical arrays of cyclonic and anticyclonic vortices that are
  similar to the pattern of the vortex Street.

---------------------------------------------------------
Title: X-ray Emission from Flaring Loops: Comparison Between RHESSI
    Observations and Hydrodynamic Simulations
Authors: Liu, Wei; Jiang, Y. W.; Petrosian, V.; Liu, S.; Mariska, J. T.
2006SPD....37.2705L    Altcode: 2006BAAS...38..254L
  RHESSI with its high temporal, spatial, and spectral resolution
  has revealed many interesting results on the X-ray emission from
  solar flares, some of which can shed light on the processes of
  energy release, particle acceleration, heating, and evaporation of
  chromospheric plasmas. During the impulsive phase of a limb flare,
  Liu et al. (2006) reported hard X-ray (HXR) emission dominated by the
  legs of the loop, as opposed to the commonly observed loop top (LT)
  and footpoint (FP) emissions. The HXR emission tends to rise above
  the FPs and eventually merge into a single LT source, suggestive of a
  gradual density increase in the loop possibly caused by chromospheric
  evaporation. During the decay phase of six limb flares, Jiang et
  al. (2006) found that the thermal LT source is confined in a small
  region near the top of the loop rather than spreading throughout the
  whole loop. The total energy of the source decays much slower than
  expected from the classical Spitzer conductive cooling alone. A
  quasi-steady loop model that includes significant suppression of
  thermal conductivity and/or continuous heating of the LT plasma,
  presumably by plasma wave turbulence, was proposed to account for
  this observation. A more thorough understanding of these phenomena
  requires a solution of the time-dependent hydrodynamics of the flaring
  plasma. We have embarked on combining our particle acceleration and
  transport code with a one-dimensional hydrodynamics code (Mariska et
  al. 1989) to simulate the response of the atmosphere to the energy
  input during the impulsive and decay phases, and investigate the
  effects of such response on the energy transport, X-ray radiation,
  and even particle acceleration and plasma heating processes. Current
  results from this work in progress will be presented. We will also
  compare the results with RHESSI observations and thus put important
  constraints on theoretical models.

---------------------------------------------------------
Title: Princeton MagnetoRotational Instability (MRI) Experiment:
    Overview and Recent Progress in the Search for the MRI
Authors: Schartman, E.; Ji, H.; Burin, M. J.; Cutler, R.;
   Heitzenroeder, P.; Liu, W.; Raftopoulos, S.; Waksman, J.; Goodman,
   J.; Stone, J.; Kageyama, A.
2006AAS...20721107S    Altcode:
  The MagnetoRotational Instability (MRI) is likely to be the dominant
  mechanism for angular momentum transport in electrically conducting
  accretion disks, such as those found in Quasars, X-ray binaries,
  cataclysmic variables and possibly protoplanetary disks. To date,
  the MRI has not been convincingly demonstrated in the laboratory. The
  Princeton MagnetoRotational Instability Experiment investigates the
  MRI in a magnetized liquid Gallium flow between concentric spinning
  cylinders. The low aspect ratio of our apparatus is vulnerable to
  large boundary effects, which are mitigated by splitting the ends
  of the chamber into pairs of differentially rotating rings. Initial
  experiments in water demonstrate reduction of the boundary effects
  and a scaling of the velocity profile with Reynolds Number. Also
  investigated are non-linear hydrodynamic effects which have also been
  proposed to drive angular momentum transport in accretion disks. The
  role of purely hydrodynamic processes is uncertain, with experiments
  and simulations giving apparently different results. The apparatus
  will next be filled with Gallium to search for signatures of the MRI:
  namely, an amplification of the non-axial components of the magnetic
  field, and an enhanced effective viscosity coupling the inner and
  outer cylinders. Initial diagnostics measure torque and external
  radial magnetic fields. In the near future internal magnetic field
  and flow diagnostics will be implemented. Our main objectives are
  (1) to clearly demonstrate MRI; (2) to study its nonlinear behavior
  and angular momentum transport; (3) to compare with state-of-the-art
  simulations similar to those used for astrophysical disks. This work
  is supported by the US DOE, NSF, and NASA.

---------------------------------------------------------
Title: Simulations of Magnetorotational Instability in a Magnetized
    Couette Flow
Authors: Liu, Wei; Goodman, Jeremy; Ji, Hantao
2006ApJ...643..306L    Altcode: 2005astro.ph..8665L
  In preparation for an experimental study of magnetorotational
  instability (MRI) in liquid metal, we present nonideal two-dimensional
  magnetohydrodynamic simulations of the nonlinear evolution of MRI in
  the experimental geometry. The simulations adopt initially uniform
  vertical magnetic fields, conducting radial boundaries, and periodic
  vertical boundary conditions. No-slip conditions are imposed at
  the cylinders. Our linear growth rates compare well with existing
  local and global linear analyses. The MRI saturates nonlinearly
  with horizontal magnetic fields comparable to the initial axial
  field. The rate of angular momentum transport increases modestly but
  significantly over the initial state. For modest fluid and magnetic
  Reynolds numbers Re,Re<SUB>m</SUB>~10<SUP>2</SUP>-10<SUP>3</SUP>,
  the final state is laminar reduced mean shear except near the radial
  boundaries, and with poloidal circulation scaling as the square root
  of resistivity, in partial agreement with the analysis of Knobloch
  and Julien. A sequence of simulations at Re<SUB>m</SUB>=20 and
  10<SUP>2</SUP>&lt;~Re&lt;~10<SUP>4.4</SUP> enables extrapolation
  to the experimental regime (Re<SUB>m</SUB>~20, Re~10<SUP>7</SUP>),
  albeit with unrealistic boundary conditions. MRI should increase the
  experimentally measured torque substantially over its initial purely
  hydrodynamic value.

---------------------------------------------------------
Title: A New Color-Magnitude Diagram for Palomar 11
Authors: Lewis, Matthew S.; Liu, W. M.; Paust, N. E. Q.; Chaboyer,
   Brian
2006AJ....131.2538L    Altcode: 2006astro.ph..1294L
  We present new photometry for the Galactic thick-disk globular cluster
  Palomar 11 extending well past the main-sequence turnoff in the V
  and I bands. This photometry shows noticeable, but depleted, red
  giant and subgiant branches. The difference in magnitude between the
  red horizontal branch (red clump) and the subgiant branch is used to
  determine that Palomar 11 has an age of 10.4+/-0.5 Gyr. The red clump
  is used to derive a distance d<SUB>solar</SUB>=14.3+/-0.4 kpc and a mean
  cluster reddening of E(V-I)=0.40+/-0.03. There is differential reddening
  across the cluster, of order δE(V-I)~0.07. The color-magnitude diagram
  of Palomar 11 is virtually identical to that of the thick-disk globular
  cluster NGC 5927, implying that these two clusters have a similar age
  and metallicity. Palomar 11 has a slightly redder red giant branch
  than 47 Tuc, implying that Palomar 11 is 0.15 dex more metal-rich, or
  1 Gyr older, than 47 Tuc. Ca II triplet observations, such as those
  of Rutledge and coworkers, favor the hypothesis that Palomar 11 is
  the same age as 47 Tuc, but slightly more metal-rich.

---------------------------------------------------------
Title: Spacebased observations of oceanic influence on the annual
    variation of South American water balance
Authors: Liu, W. Timothy; Xie, Xiaosu; Tang, Wenqing; Zlotnicki, Victor
2006GeoRL..33.8710L    Altcode:
  The mass change of South America (SA) continent measured by the
  Gravity Recovery and Climate Experiment (GRACE) imposes a constraint
  on the uncertainties in estimating the annual variation of rainfall
  measured by Tropical Rain Measuring Mission (TRMM) and ocean moisture
  influx derived from QuikSCAT data. The approximate balance of the
  mass change rate with the moisture influx less climatological river
  discharge, in agreement with the conservation principle, bolsters
  not only the credibility of the spacebased measurements, but supports
  the characterization of ocean's influence on the annual variation of
  continental water balance. The annual variation of rainfall is found to
  be in phase with the mass change rate in the Amazon and the La Plata
  basins, and the moisture advection across relevant segments of the
  Pacific and Atlantic coasts agrees with the annual cycle of rainfall
  in the two basins and the Andes mountains.

---------------------------------------------------------
Title: Determination of the astrophysical Si26(p,γ)P27 reaction rate
    from the asymptotic normalization coefficients of Mg27 → Mg26 + n
Authors: Guo, B.; Li, Z. H.; Bai, X. X.; Liu, W. P.; Shu, N. C.;
   Chen, Y. S.
2006PhRvC..73d8801G    Altcode:
  The squares of neutron asymptotic normalization coefficient (ANC)
  for Mg27 → Mg26 + n are extracted to be 44.0 ± 5.3, 3.40 ± 0.32
  and 0.90 ± 0.08 fm<SUP>-1</SUP> from the angular distributions of
  the Mg26(d,p)Mg27 reaction leading to the ground, first, and second
  excited states of Mg27, respectively, based on distorted wave Born
  approximation (DWBA) analysis. According to charge symmetry of mirror
  nuclei, the square of proton ANC for P27 → Si26 + p is determined
  to be 1840 ± 240 fm<SUP>-1</SUP> and then utilized to calculate the
  astrophysical S-factor and rate for the direct capture into the P27
  ground state. In addition, the proton widths for the first and second
  excited states in P27 are derived to be 1.30 ± 0.12 × 10<SUP>-8</SUP>
  and 1.79 ± 0.15 × 10<SUP>-5</SUP> MeV from the neutron ANCs and used
  to compute the contribution of the resonant captures. Furthermore, we
  have also presented the total astrophysical Si26(p,γ)P27 reaction rate.

---------------------------------------------------------
Title: Study of Magnetorotational Instability and Hydrodynamic
    Stability at Large Reynolds Numbers in a Short Couette Flow
Authors: Ji, Hantao; Burin, Michael; Schartman, Ethan; Goodman,
   Jeremy; Liu, Wei
2006APS..APR.D1042J    Altcode:
  Rapid angular momentum transport in accretion disks has been a
  longstanding astrophysical puzzle. Molecular viscosity is inadequate
  to explain observationally inferred accretion rates. Since Keplerian
  flow profiles are linearly stable in hydrodynamics, there exist
  only two viable mechanisms for the required turbulence: nonlinear
  hydrodynamic instability or magnetorotational instability (MRI). The
  latter is regarded as a dominant mechanism for rapid angular momentum
  transport in hot accretion disks ranging from quasars and X-ray
  binaries to cataclysmic variables. The former has been proposed mainly
  for colder protoplanetary disks, whose Reynolds numbers are typically
  large. Despite their popularity, however, both candidate mechanisms have
  been rarely demonstrated and studied in the laboratory. In this paper,
  I will describe a laboratory experiment in a short Taylor-Couette flow
  geometry intended for such purposes. Based on the results from prototype
  experiments and simulations, the apparatus containing novel features
  for better controls of the boundary-driven secondary flows has been
  constructed. Initial results on hydrodynamic stability have shown,
  somewhat surprisingly, robust quiescence of the Keplerian-like flows
  with million Reynolds numbers, casting questions on viability of the
  nonlinear hydrodynamic instability.

---------------------------------------------------------
Title: Impact of atmospheric submonthly oscillations on sea surface
    temperature of the tropical Indian Ocean
Authors: Han, Weiqing; Liu, W. Timothy; Lin, Jialin
2006GeoRL..33.3609H    Altcode: 2006GeoRL..3303609H
  Impacts of atmospheric intraseasonal oscillations (ISOs) at submonthly
  periods (10-30 days) on Indian Ocean sea surface temperature (SST)
  are studied using satellite observed outgoing long wave radiation,
  QuikSCAT winds, SST and an ocean general circulation model for the
  period of 1999-2004. The results suggest that submonthly ISOs can cause
  significant 10-30 day SST changes throughout the equatorial basin and
  northern Bay of Bengal, with an amplitude of as large as 0.5°C and
  standard deviation of exceeding 0.2°C for a 4-year record. Impact
  of the submonthly ISO associated with the Indian summer monsoon is
  separately examined. It is associated with basin-scale SST evolution
  with distinct spatial structures. The SST variation results mainly from
  submonthly wind forcing, which causes changes in oceanic processes and
  surface turbulent heat fluxes. Radiative fluxes can also have large
  influences in some regions for some ISO events.

---------------------------------------------------------
Title: Evolution of the Loop-Top Source of Solar Flares: Heating
    and Cooling Processes
Authors: Jiang, Yan Wei; Liu, Siming; Liu, Wei; Petrosian, Vahé
2006ApJ...638.1140J    Altcode: 2005astro.ph..8532J
  We present a study of the spatial and spectral evolution of the loop-top
  (LT) sources in a sample of six flares near the solar limb observed by
  RHESSI. A distinct coronal source, which we identify as the LT source,
  was seen in each of these flares from the early “preheating” phase
  through the late decay phase. Spectral analyses reveal an evident
  steep power-law component in the preheating and impulsive phases,
  suggesting that the particle acceleration starts upon the onset of the
  flares. In the late decay phase the LT source has a thermal spectrum
  and appears to be confined within a small region near the top of the
  flare loop and does not spread throughout the loop, as is observed
  at lower energies. The total energy of this source decreases usually
  faster than expected from the radiative cooling but much slower than
  that due to the classical Spitzer conductive cooling along the flare
  loop. These results indicate the presence of a distinct LT region,
  where the thermal conductivity is suppressed significantly and/or there
  is a continuous energy input. We suggest that plasma wave turbulence
  could play important roles in both heating the plasma and suppressing
  the conduction during the decay phase of solar flares. With a simple
  quasi-steady loop model we show that the energy input in the gradual
  phase can be comparable to that in the impulsive phase and demonstrate
  how the observed cooling and confinement of the LT source can be used
  to constrain the wave-particle interaction.

---------------------------------------------------------
Title: Methane-rich fluid inclusions from ophiolitic dunite and
post-collisional mafic ultramafic intrusion: The mantle dynamics
    underneath the Palaeo-Asian Ocean through to the post-collisional
    period
Authors: Liu, Wei; Fei, Pan Xiao
2006E&PSL.242..286L    Altcode:
  The protracted development history of the Palaeo-Asian Ocean starting
  from ∼1000 Ma to ∼320 Ma, and continuation of mantle-derived
  magmatism right through the post-collisional period as manifested by the
  widespread mafic-ultramafic intrusion and alkaline-peralkaline granite
  suggest a vigorous, long-running mantle dynamo. Using the micro-laser
  Raman spectrometer, we analyzed olivine- and plagioclase-hosted fluid
  inclusions from ophiolitic dunite, Kudi of the western Kunlun Range,
  and post-collisional mafic-ultramafic intrusions of the Xiangshan and
  the Huangshandong, eastern Chinese Tienshan Mountains. Our results
  show that fluids brought from the mantle by these rocks are rich
  in H <SUB>2</SUB>O and CH <SUB>4</SUB> with variable amounts of N
  <SUB>2</SUB>. Estimation of the redox state, pressure and depth of
  formation for the melt-CH <SUB>4</SUB>-H <SUB>2</SUB>O + N <SUB>2</SUB>
  fluid systems from the 3 rock suites of the Xinjiang, and comparison
  of these parameters with those of the peridotite-fluid parageneses for
  the sub-cratonic upper mantle give meaningful results. These fluids
  were formed in the asthenosphere, were originally CH <SUB>4</SUB>-N
  <SUB>2</SUB>-rich, primordial mantle fluid, but have been progressively
  diluted with H <SUB>2</SUB>O and become oxidized by repeated
  subduction of oceanic slab. We propose that repeated redox melting
  in the mantle due to dilution of CH <SUB>4</SUB> with H <SUB>2</SUB>O
  and oxidation caused formation of the long-lived Palaeo-Asian Ocean,
  brought about extensive intrusion of mafic-ultramafic complexes and
  alkaline-peralkaline granites right through the post-collisional period,
  and, consequently, resulted in significant Phanerozoic continental
  growth in the Central Asian Orogenic Belt. Rise of atmospheric O
  <SUB>2</SUB> and the Earth's major oxidation occurred at about 2.4 to
  2.2 Ga. Oxidation of the Earth's mantle promoted the mantle melting
  and magma input to the crust, resulting in major continental growth
  after 2.5 Ga. However, much-postponed oxidation of the primordial
  mantle underneath the Central Asian Orogenic Belt led to significant
  continental growth in the Phanerozoic times.

---------------------------------------------------------
Title: Indirect Measurements of Nuclear Astrophysics Reactions Using
    Unstable Nuclear Beams
Authors: Liu, Wei-Ping; Li, Zhi-Hong; Bai, Xi-Xiang; Wang, You-Bao;
   Lian, Gang; Guo, Bing; Zeng, Sheng; Yan, Sheng-Quan; Wang, Bao-Xiang;
   Su, Jun; Shu, Neng-Chuan; Chen, Yong-Shou
2006IJMPE..15.1899L    Altcode:
  This paper described the nuclear astrophysical studies using the
  unstable ion beam facility GIRAFFE, by indirect measurements. We
  measured the angular distributions for some single proton or
  neutron transfer reactions, such as <SUP>7</SUP>Be(d,n)<SUP>8</SUP>B,
  <SUP>11</SUP>C(d,n)<SUP>12</SUP>N, <SUP>8</SUP>Li(d,n)<SUP>9</SUP>Be,
  <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li and <SUP>13</SUP>N(d,n)<SUP>14</SUP>O
  in inverse kinematics, and derived the astrophysical S-factors
  or reaction rates of <SUP>7</SUP>Be(p,γ)<SUP>8</SUP>B,
  <SUP>11</SUP>C(p,γ)<SUP>12</SUP>N, <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li,
  <SUP>13</SUP>N(p,γ)<SUP>14</SUP>O by asymptotic normalization
  coefficient, spectroscopic factor, and R-matrix approach at
  astrophysically relevant energies.

---------------------------------------------------------
Title: Laboratory Study of Magnetorotational Instability and
    Hydrodynamic Stability at Large Reynolds Numbers
Authors: Ji, H.; Burin, M.; Schartman, E.; Goodman, J.; Liu, W.
2006nla..conf..106J    Altcode:
  Two plausible mechanisms have been proposed to explain rapid angular
  momentum transport during accretion processes in astrophysical disks:
  nonlinear hydrodynamic instabilities and magnetorotational instability
  (MRI). A laboratory experiment in a short Taylor-Couette flow geometry
  has been constructed in Princeton to study both mechanisms, with novel
  features for better controls of the boundary-driven secondary flows
  (Ekman circulation). Initial results on hydrodynamic stability have
  shown negligible angular momentum transport in Keplerian-like flows
  with Reynolds numbers approaching one million, casting strong doubt
  on the viability of nonlinear hydrodynamic instability as a source
  for accretion disk turbulence.

---------------------------------------------------------
Title: A machine learning based approach to remote sensing image
    classification
Authors: Zhang, J.; Liu, W.; Gruenwald, L.
2006cosp...36..235Z    Altcode: 2006cosp.meet..235Z
  Decision Tree DT has been widely used for training and classification
  of remotely sensed image data due to its capability to generate human
  interpretable decision rules and its relatively fast speed in training
  and classification This paper proposes a Successive Decision Tree SDT
  approach where the samples in the ill-classified branches of a previous
  resulting decision tree are used to construct a successive decision tree
  The decision trees are chained together through pointers and used for
  classification The proposed approach is applied to two real remotely
  sensed image data sets for evaluations in terms of classification
  accuracy and interpretability of the resulting decision rules

---------------------------------------------------------
Title: Deramp Range Migration Processing for Satellite-borne Spotlight
    Synthetic Aperture Radar
Authors: Ding, Z.; Zeng, T.; Long, T.; Liu, W.
2006cosp...36.3786D    Altcode: 2006cosp.meet.3786D
  Based on the two-step algorithm and range migration algorithm the deramp
  range migration algorithm for the high-resolution satellite-borne
  spotlight synthetic aperture radar SAR is presented The algorithm
  combines the advantages of SPECAN algorithm and range migration
  algorithm The first step of the proposed algorithm implements a
  linear and space-invariant azimuth filtering that is carried out via
  a deramp-based technique representing a simplified version of SPECAN
  approach This operation allows us to perform a bulk azimuth raw data
  compression and to achieve a pixel spacing no larger than the expected
  azimuth resolution of the fully focused image Thus the azimuth spectral
  folding phenomenon which is typical for satellite-borne spotlight SAR
  is overcome And the space-variant characteristics of the strip-map
  system transfer function are preserved Secondly the residual and
  precise focusing of the SAR data is achieved by applying the range
  migration algorithm The range migration algorithm can be applied to
  carry out by simply accounting for a new system transfer function and
  by considering the new azimuth sampling frequency In this algorithm
  the squinted equivalent range model that is fitter for satellite-borne
  SAR is introduced The equivalent velocity and equivalent squint angle
  are two important parameters in the algorithm and should accurately
  be acquired When the equivalent velocity and equivalent squint angle
  acquired form the spacecraft ancillary data are imprecise the estimation
  of the two parameters is circumvent through estimating the Doppler

---------------------------------------------------------
Title: Time-frequency Analysis for Acoustic Emission Signals of
    Hypervelocity Impact
Authors: Liu, W. G.; Pang, B. J.; Zhang, W.; Sun, F.; Guan, G. S.
2006cosp...36.2724L    Altcode: 2006cosp.meet.2724L
  The risk of collision of man-made orbital debris with spacecraft in
  near Earth orbits continues to increase A major of the space debris
  between 1mm and 10mm can t be well tracked in Earth orbits Damage from
  these un-tracked debris impacts is a serious hazard to aircraft and
  spacecraft These on-orbit collisions occur at velocities exceeding
  10km s and at these velocities even very small particles can create
  significant damage The development of in-situ impact detecting system is
  indispensable for protecting the spacecraft from tragedy malfunction
  by the debris Acoustic Emission AE detecting technique has been
  recognized as an important technology for non-destructive detecting
  due to the AE signals offering a potentially useful additional means
  of non-invasively gathering concerning the state of spacecrafts Also
  Acoustic emission health monitoring is able to detect locate and assess
  impact damage when the spacecrafts is impacted by hypervelocity space
  debris and micrometeoroids This information can help operators and
  designers at the ground station take effective measures to maintain
  the function of spacecraft In this article Acoustic emission AE is
  used for characterization and location for hypervelocity Impacts Two
  different Acoustic Emission AE sensors were used to detect the arrival
  time and signals of the hits Hypervelocity Impacts were generated with
  a two-stage light-gas gun firing small Aluminum ball projectiles 4mm
  6 4mm In the impact studies the signals were recorded with Disp AEwin
  PAC instruments by the conventional crossing

---------------------------------------------------------
Title: System-level science in the ILWS era
Authors: Liu, W.
2006cosp...36..988L    Altcode: 2006cosp.meet..988L
  Solar system plasma physics is moving steadily toward the era of true
  system-level science While multiscale computational modeling has seen
  rapid progress over the past decade our experimental methodology has
  also moved toward the orientation of observing the multiscale coupling
  in solar system plasmas A more comprehensive and at the same time less
  ambiguous observational description of the system is fundamental to
  further understanding and is a goal that the International Living With
  a Star promotes Some noteworthy trends in our science are broader
  international participation greater awareness of mission synergy
  carefully coordinated satellite constellations and last but not least
  a much closer integration of ground-based observations as part of the
  frontline scientific programs A much improved observational description
  will provide more sharply defined constraints to which computational
  models must meet not only in principle but also in detail While the
  task is obviously daunting I will give a synthesis of where we are
  in multiscale system-level science with an emphasis on mission and
  experimental elements associated with the ILWS program

---------------------------------------------------------
Title: Astrophysical Reaction Rates of the
    <SUP>8</SUP>Li(p,γ)<SUP>9</SUP>Be<SUB>g.s.</SUB> Direct Capture
    Reaction
Authors: Su, Jun; Li, Zhi-Hong; Guo, Bing; Liu, Wei-Ping; Bai,
   Xi-Xiang; Zeng, Sheng; Lian, Gang; Yan, Sheng-Quan; Wang, Bao-Xiang;
   Wang, You-Bao
2006ChPhL..23...55S    Altcode:
  Based on the angular distribution of the
  <SUP>8</SUP>Li(d,n)<SUP>9</SUP>Be<SUB>g.s.</SUB> reaction at
  E<SUB>c.m.</SUB> = 8.0 MeV and distorted wave Born approximation
  analysis, the single particle spectroscopic factor S<SUB>1,3/2</SUB> for
  the ground state of <SUP>9</SUP>Be = <SUP>8</SUP>Liotimesp is derived
  to be 0.64 ± 0.21. In addition, we deduce the astrophysical S-factors
  and rates of the <SUP>8</SUP>Li(p,γ)<SUP>9</SUP>Be<SUB>g.s.</SUB>
  direct capture reaction at energies of astrophysical interests.

---------------------------------------------------------
Title: Magnetic reconnection configurations and particle accelerations
    on the Sun
Authors: Chen, P. F.; Liu, W. J.; Fang, C.
2006cosp...36.3345C    Altcode: 2006cosp.meet.3345C
  The electric field near the small-scale reconnection site has been
  suggested to be a plausible mechanism for the nonthermal particles
  that produce type III radio bursts and hard X-ray emissions in the
  corona and chromosphere It has been demonstrated that the magnetic
  configuration near the reconnection site plays an important role in
  determining the final energy spectrum of the particles In this paper we
  first review different reconnection configurations in the Sun which are
  associated with various eruptive phenomena such as two-ribbon flares
  emerging flux coronal loop-loop interactions and so on We then perform
  test particle simulations with these magnetic configurations in order
  to investigate their effect on the energy spectrum of the accelerated
  particles Their application to observations is discussed

---------------------------------------------------------
Title: Investigation of Electron Energy Spectrum During Solar Flares
Authors: Liu, W. J.; Chen, P. F.; Fang, C.; Ding, M. D.
2006cosp...36.2650L    Altcode: 2006cosp.meet.2650L
  Observations indicated that the energy spectrum of non-thermal
  particles during the evolution of solar flares changes rapidly with
  the power index alternating from soft to hard and soft again Based on
  MHD numerical simulation of a flare with the typical prephase impulsive
  and decay phases we perform the test-particle simulations in order to
  investigate the time evolution of the electron spectrum The results
  are compared with observations in detail

---------------------------------------------------------
Title: The <SUP>21</SUP>Na(p, γ) <SUP>22</SUP>Mg Reaction from
    E<SUB>cm</SUB> = 200 to 850 KeV in Explosive Stellar Events
Authors: Bishop, S.; D'Auria, J. M.; Chen, A.; Hunter, D.; Lamey, M.;
   Liu, W.; Wrede, C.; Azuma, R. E.; King, J. D.; Buchmann, L.; Hutcheon,
   D.; Laird, A. M.; Olin, A.; Ottewell, D.; Rogers, J.; Chatterjee,
   M. L.; Engel, S.; Gigliotti, D.; Hussein, A.; Greife, U.; Jewett,
   C. C.; José, J.; Kubono, S.; Michimasa, S.; Lewis, R.; Parker, P.
2005omeg.conf..375B    Altcode:
  The long-lived radioactive nuclide <SUP>22</SUP>Na (t<SUB>1/2</SUB> =
  2.6 y) is, in principle, an astronomical observable for understanding
  the physics processes of oxygen-neon novae. Production and abundance
  yields of <SUP>22</SUP>Na in these events are dependent to the hitherto
  unknown rate of the <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg reaction. Using
  a high intensity radioactive <SUP>21</SUP>Na beam at the TRIUMF-ISAC
  facility, direct measurements of the strengths of six potentially
  astrophysically important resonances have been made at center of
  mass energies in the range: E<SUB>cm</SUB> = 200 to 850 keV. Reported
  herein are preliminary results obtained for these strengths and their
  respective contributions to the <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg
  stellar reaction rate.

---------------------------------------------------------
Title: A New Color-Magnitude Diagram for Palomar 11
Authors: Chaboyer, B.; Lewis, M. S.; Liu, W. M.; Paust, N. E. Q.
2005AAS...20712805C    Altcode: 2005BAAS...37R1372C
  We present new photometry for the Galactic thick disk globular cluster
  Palomar 11 extending well past the main sequence turn-off in the
  V and I bands. This photometry shows noticeable, but depleted red
  giant and subgiant branches. The difference in magnitude between the
  red horizontal branch (red clump) and the subgiant branch is used to
  determine that Palomar 11 has an age of 10.4± 0.5 Gyr. The red clump
  is used to derive a distance d<SUB>⊙</SUB>=14.3± 0.4 kpc, and a
  cluster reddening of E(V-I)=0.40± 0.03. The colour magnitude diagram
  of Palomar 11 is virtually identically to the thick disk globular
  cluster NGC 5927, implying that these two clusters have a similar age
  and metallicity. Palomar 11 has a slightly bluer red giant branch than
  47 Tuc, implying that Palomar 11 is 0.15 dex more metal-rich, or 1 Gyr
  older than 47 Tuc. Ca II triplet observations (Rutledge et al. 1997,
  PASP, 109, 907) favour the hypothesis that Palomar 11 is the same age
  as 47 Tuc, but slightly more metal-rich. <P />Research supported in
  part by a NSF CAREER grant 0094231 to BC. BC is a Cottrell Scholar of
  the Research Corporation.

---------------------------------------------------------
Title: Hard X-ray Emissions From The Legs of Flaring Loops
Authors: Liu, W.; Liu, S.; Jiang, Y.; Petrosian, V.
2005AGUFMSH13A0287L    Altcode:
  or the first time in the RHESSI era, Liu et al. (2005) reported hard
  X-ray emissions coming from the legs of a flaring loop at intermediate
  energies, as opposed to the commonly observed looptop (LT) and footpoint
  (FP) emissions. In an M-1.7 flare observed by RHESSI on November 13,
  2003, we found that the FPs in the 9-20 keV energy range rose up to
  the legs and eventually merged at the LT, suggestive of a gradual
  density enhancement in the loop possibly caused by chromospheric
  evaporation. We identified several flares with similar behavior and
  analyzed their images, spectra, and imaging spectroscopy, in an effort
  to better understand the nature of the leg emissions. We will present
  the results of our data analysis of all such flares and discuss their
  implications for the particle acceleration and other theoretical aspects
  of flares such as chromospheric evaporation. The work is supported
  by NASA grants NAG5-12111, NAG5 11918-1, and NSF grant ATM-0312344 at
  Stanford University.

---------------------------------------------------------
Title: Magnetic topologies and two-class coronal mass ejections:
    a numerical magnetohydrodynamic study
Authors: Liu, W.; Zhao, X. P.; Wu, S. T.; Scherrer, P. H.
2005astro.ph.11023L    Altcode:
  White-light observations of the solar corona show that there are two
  characteristic types of Coronal Mass Ejections (CMEs) in terms of
  speed-height profiles: so-called fast CMEs that attain high speeds
  low in the corona and slow CMEs that gradually accelerate from low
  initial speeds. Low and Zhang (2002) have recently proposed that fast
  and slow CMEs result from initial states with magnetic configurations
  characterized by normal prominences (NPs) and inverse prominences (IPs),
  respectively. To test their theory, we employed a two-dimensional,
  time-dependent, resistive magnetohydrodynamic code to simulate the
  expulsion of CMEs in these two different prominence environments. Our
  numerical simulations demonstrate that (i) a CME-like expulsion is more
  readily produced in an NP than in an IP environment, and, (ii) a CME
  originating from an NP environment tends to have a higher speed early
  in the event than one originating from an IP environment. Magnetic
  reconnection plays distinct roles in the two different field
  topologies of these two environments to produce their characteristic
  CME speed-height profiles. Our numerical simulations support the
  proposal of Low and Zhang (2002) although the reconnection development
  for the NP associated CME is different from the one sketched in their
  theory. Observational implications of our simulations are discussed.

---------------------------------------------------------
Title: The <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li reaction and
    astrophysical <SUP>8</SUP>B(p,γ)<SUP>9</SUP>C reaction rate
Authors: Guo, B.; Li, Z. H.; Liu, W. P.; Bai, X. X.; Lian, G.; Yan,
   S. Q.; Wang, B. X.; Zeng, S.; Su, J.; Lu, Y.
2005NuPhA.761..162G    Altcode:
  Angular distribution of the Li8(d,p)Lig.s.9 reaction at
  E<SUB></SUB>=7.8MeV was measured in inverse kinematics. The square of
  asymptotic normalization coefficient (ANC) for the virtual decay
  Li9→Li8+n was derived to be 1.33±0.33fm<SUP></SUP> through
  distorted wave Born approximation (DWBA) analysis, for the first
  time. According to charge symmetry, (ANC)<SUP>2</SUP> for C9→B8+p
  was then extracted to be 1.14±0.29fm<SUP></SUP>. We have deduced
  the astrophysical S-factors and reaction rates for direct capture in
  B8(p,γ)C9 at energies of astrophysical relevance using the ANC for
  C9→B8+p extracted from the mirror system.

---------------------------------------------------------
Title: Exact soliton solutions and nonlinear modulation instability
    in spinor Bose-Einstein condensates
Authors: Li, Lu; Li, Zaidong; Malomed, Boris A.; Mihalache, Dumitru;
   Liu, W. M.
2005PhRvA..72c3611L    Altcode:
  We find one-, two-, and three-component solitons of the polar and
  ferromagnetic (FM) types in the general (nonintegrable) model of a
  spinor (three-component) model of the Bose-Einstein condensate, based on
  a system of three nonlinearly coupled Gross-Pitaevskii equations. The
  stability of the solitons is studied by means of direct simulations
  and, in a part, analytically, using linearized equations for small
  perturbations. Global stability of the solitons is considered by means
  of an energy comparison. As a result, ground-state and metastable
  soliton states of the FM and polar types are identified. For the
  special integrable version of the model, we develop the Darboux
  transformation (DT). As an application of the DT, analytical solutions
  are obtained that display full nonlinear evolution of the modulational
  instability of a continuous-wave state seeded by a small spatially
  periodic perturbation. Additionally, by dint of direct simulations,
  we demonstrate that solitons of both the polar and FM types, found in
  the integrable system, are structurally stable; i.e., they are robust
  under random changes of the relevant nonlinear coefficient in time.

---------------------------------------------------------
Title: Acoustic Emission Detection and Location for Hypervelocity
    Impacts
Authors: Liu, W. G.; Sun, F.; Pang, B. J.; Zhang, W.
2005ESASP.587..661L    Altcode: 2005spde.conf..661L
  No abstract at ADS

---------------------------------------------------------
Title: Variations of N<SUP>+</SUP>/O<SUP>+</SUP> in the ring current
    during magnetic storms
Authors: Liu, W. L.; Fu, S. Y.; Zong, Q. -G.; Pu, Z. Y.; Yang, J.;
   Ruan, P.
2005GeoRL..3215102L    Altcode:
  Based on the energetic particle measurements obtained by CRRES/MICS,
  variations of the third most important ion species, N<SUP>+</SUP>,
  in the ring current region have been investigated in detail. The
  ratio of N<SUP>+</SUP>/O<SUP>+</SUP> during geomagnetic quiet times
  is found to be about 0.314 +/- 0.043 and decreases with enhanced
  solar radiation, as indicated by the F10.7 index. Through a statistic
  study, the ratio of N<SUP>+</SUP>/O<SUP>+</SUP> has been demonstrated
  to decrease with enhanced geomagnetic activity for strong storms,
  whereas for small storms, there is no obvious correlation found for
  this ratio. It is worthy to note that not all the values during active
  times are higher than those at quiet times. The quite different ratios
  of N<SUP>+</SUP>/O<SUP>+</SUP> (up to 50%) in the ring current region
  found between quiet and storm times in this paper, together with the
  different combination rates of atomic oxygen and nitrogen, suggest
  that the ionospheric nitrogen ions may play a crucial role during
  some magnetic storms and should have a strong impact on the magnetic
  storm simulation works on the build-up and/or decay processes of the
  ring current.

---------------------------------------------------------
Title: Elasticity of San Carlos olivine to 8 GPa and 1073 K
Authors: Liu, Wei; Kung, Jennifer; Li, Baosheng
2005GeoRL..3216301L    Altcode:
  Elasticity of San Carlos olivine, (Mg<SUB>0.9</SUB>,
  Fe<SUB>0.1</SUB>)<SUB>2</SUB>SiO<SUB>4</SUB>, has been measured at
  simultaneous high pressure and high temperature to 8.2 GPa and 1073
  K using ultrasonic interferometry in conjunction with synchrotron
  X-radiation. The elastic moduli and their pressure and temperature
  derivatives are precisely determined using a pressure standard
  free fit using third-order finite strain equations to the velocity
  and unit cell volume data in the entire pressure and temperature
  range, yielding K<SUB>S0</SUB> = 130.3(4) GPa, G<SUB>0</SUB>
  = 77.4(2) GPa, K'<SUB>S0</SUB> = 4.61(11), G'<SUB>0</SUB> =
  1.61(4), ∂K<SUB>S</SUB>/∂T = -0.0164(5) GPa/K, and ∂G/∂T
  = -0.0130(3) GPa/K. Combined with previous thermoelastic data
  on wadsleyite, the velocity contrasts between α- and β-(Mg,
  Fe)<SUB>2</SUB>SiO<SUB>4</SUB> at 410-km depth are calculated along a
  1673 K adiabatic geotherm with plausible iron partition between the
  two phases. The fraction of olivine consistent with a ~5% seismic
  discontinuity in an anhydrous mantle is constrained to be less than
  ~50% with the possibility that a hydrous or a cooler mantle increases
  the olivine content towards pyrolitic composition.

---------------------------------------------------------
Title: The <SUP>11</SUP>C(p,γ)<SUP>12</SUP>N reaction rate and the
    conversion of <SUP>3</SUP>He into CNO
Authors: Shu, N. -C.; Chen, Y. -S.; Wu, K. -S.; Bai, X. -X.; Li,
   Z. -H.; Liu, W. -P.
2005NuPhA.758..419S    Altcode:
  The reaction sequence of
  <SUP>3</SUP>He(α,γ)<SUP>7</SUP>Be(α,γ)<SUP>11</SUP>C(p,γ)<SUP>12</SUP>N
  to CNO could be an alterative way of 3α →<SUP>12</SUP>C to
  convert <SUP>3</SUP>He into CNO. It may become important in some
  specific environments, such as in a very massive star with low
  metallicity. Whether it is significant depends on the reactions
  involved, one of the important reactions is the <SUP>11</SUP>C
  p-capture competing with its β<SUP>+</SUP> decay. The S factor for
  the <SUP>11</SUP>C(p,γ)<SUP>12</SUP>N direct capture was obtained in
  our previous work. This work is to update the reaction rate by adding
  uncertainty and fitting with the Thielemann format. With the new rate,
  nucleosynthesis simulations are performed to study the bridge of the
  p-p chains to CNO through the above sequence.

---------------------------------------------------------
Title: Impulsive Phase Hard X-Ray Source Motions Observed by RHESSI
Authors: Liu, W.; Liu, S.; Jiang, Y.; Petrosian, V.
2005AGUSMSP41C..06L    Altcode:
  High temporal, spatial, and spectral resolution observations by RHESSI
  have provided some interesting and surprising results. In this paper
  we present results of our analyses of the spatial evolution during
  the impulsive phase, in particular the motions of the looptop (LT)
  and footpoint (FP) sources of flares with a simple loop structure. For
  the first time, on November 13, 2003 RHESSI observed HXR emissions
  from the legs of a flaring loop, in contrast to the commonly observed
  LT and FP emissions. In the 9-30 keV energy range, emissions from
  the FPs initially appear to extend toward the legs, then rise up,
  and eventually merge at the LT. This motion happens first at lower
  energies and proceeds to higher energies, indicating a gradual density
  increase in the flaring loop, induced possibly by chromospheric
  evaporation. Spectral analyses are carried out to determine the nature
  of these sources. We discuss the implications of these results on the
  particle acceleration, plasma heating, and chromospheric evaporation
  processes. The work is supported by NASA grants NAG5-12111, NAG5
  11918-1, and NSF grant ATM-0312344 at Stanford University.

---------------------------------------------------------
Title: The <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li reaction and the
    astrophysical <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li reaction rate
Authors: Li, Z. H.; Liu, W. P.; Bai, X. X.; Guo, B.; Lian, G.; Yan,
   S. Q.; Wang, B. X.; Zeng, S.; Lu, Y.; Su, J.; Chen, Y. S.; Wu, K. S.;
   Shu, N. C.; Kajino, T.
2005PhRvC..71e2801L    Altcode: 2009arXiv0903.3092L
  The <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li reaction plays an
  important role in both the r-process nucleosynthesis and the
  inhomogeneous big bang models. Its direct capture rates can be
  extracted from the <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li reaction,
  indirectly. We have measured the angular distribution of the
  <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li<SUB>g.s.</SUB> reaction at
  E<SUB>c.m.</SUB> = 7.8 in inverse kinematics using coincidence
  detection of <SUP>9</SUP>Li and the recoil proton, for the first
  time. Based on distorted wave Born approximation (DWBA) analysis,
  the <SUP>8</SUP>Li(d,p)<SUP>9</SUP>Li<SUB>g.s.</SUB> cross
  section was determined to be 7.9 ± 2.0 mb. The single particle
  spectroscopic factor S<SUB>1,3/2</SUB> for the ground state of
  <SUP>9</SUP>Li=<SUP>8</SUP>Li⊗n was derived to be 0.68±0.14,
  and then used to calculate the direct capture cross sections for
  the <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li<SUB>g.s.</SUB> reaction
  at energies of astrophysical interest. The astrophysical
  <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li<SUB>g.s.</SUB>
  reaction rate for the direct capture was found to be
  3970±950cm<SUP>3</SUP>mole<SUP>-1</SUP>s<SUP>-1</SUP> at
  T<SUB>9</SUB>=1. This presents the first experimental constraint for
  the <SUP>8</SUP>Li(n,γ)<SUP>9</SUP>Li reaction rates of astrophysical
  relevance.

---------------------------------------------------------
Title: On the cooling processes of solar flare loops in the gradual
    decaying phase---Suppression of conduction and heating by plasma
    wave turbulence
Authors: Jiang, Y.; Liu, S.; Liu, W.; Petrosian, V.
2005AGUSMSP23B..05J    Altcode:
  High spectral and spatial resolution observations of RHESSI show
  that emission in the gradual phase of many solar flares is dominated
  by a thermal looptop source, which cools down faster than expected
  from the radiative cooling but much slower than that due to the
  cooling by classical Spitzer conductivity. This could be due to a
  continuous energy input at a rate equal to the conduction rate. One
  would then expect a nearly isothermal loop with an almost uniform
  emission along the loop and significant energy injections at the foot
  points. However, the looptop image is resolved along the loop and
  appears to be confined to the top portion of the loop. This requires a
  suppression of conduction within the source region. Combining imaging
  spectroscopic observations of RHESSI with the GOES light curves,
  we model the evolution of the loops in the gradual phase of several
  flares. We find that the suppression of conduction alone can not
  account for the RHESSI observations in a quasi-steady equilibrium
  loop model. A sustained (although declining) energy input is also
  needed. Thermal damping of turbulence produced continuously (albeit
  at a declining rate) during the decay phase can be responsible for
  the heating process. Presence of turbulence could also suppress the
  conduction rate. This work is supported by NASA grants NAG5-12111,
  NAG5 11918-1, and NSF grant ATM-0312344.

---------------------------------------------------------
Title: The <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg reaction in novae
    and x-ray bursts
Authors: Chen, A. A.; Azuma, R. E.; Bishop, S.; Buchmann, L.;
   Chatterjee, M. L.; D'Auria, J. M.; Engel, S.; Gigliotti, D.; Greife,
   U.; Hunter, D.; Hussein, A.; Hutcheon, D.; Jewett, C. C.; José, J.;
   King, J. D.; Laird, A. M.; Lamey, M.; Lewis, R.; Liu, W.; Olin, A.;
   Ottewell, D.; Parker, P.; Rogers, J.; Ruiz, C.; Trinczek, M.; Wrede, C.
2005NuPhA.752..510C    Altcode:
  The <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg reaction is an important link
  in the synthesis of <SUP>22</SUP>Na in oxygenneon novae, and serves
  as one of the first steps of the rp-process in x-ray bursts. This
  reaction has recently been studied at the TRIUMF-ISAC radioactive beam
  facility with the new DRAGON recoil separator. Resonant contributions
  have been measured for seven <SUP>22</SUP>Mg states, from near the
  proton threshold to about 6 MeV in excitation energy. We report the
  results and their impact on the <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg
  reaction rate in novae and x-ray bursts.

---------------------------------------------------------
Title: Substorm Associated Spikes in High Energy Particle
    Precipitation
Authors: Spanswick, E.; Donovan, E.; Liu, W.; Wallis, D.; Aasnes,
   A.; Hiebert, T.; Jackel, B.; Henderson, M.; Frey, H.
2005GMS...155..227S    Altcode:
  Using data from the 13 instrument CANOPUS riometer array in
  north-central Canada, we have examined a large number of substorm
  events. Here, we focus on a substorm associated transient "spike"
  of significant absorption. We present a statistical analysis
  of temporal structure, propagation characteristics, and relative
  occurrence of absorption spikes seen with the CANOPUS array. We also
  present examples of both isolated transient spike events and a single
  propagating event. Seen from any one station, the spike lasts several
  minutes. More globally, it typically takes tens of minutes to propagate
  across the CANOPUS array. The propagation is in general a combination
  of azimuthal (ie., East or West) and poleward motion. Spikes are
  associated with the vast majority of substorms and at least some
  pseudobreakups. Simultaneous X-ray images confirm that the spike is
  a spatially localized region of high-energy precipitation and not,
  for example, a boundary. We discuss possible magnetospheric sources
  of this precipitation.

---------------------------------------------------------
Title: Ion composition variations in the plasma sheet observed
    by Cluster/RAPID
Authors: Ruan, P.; Fu, S. Y.; Zong, Q. -G.; Pu, Z. Y.; Cao, X.; Liu,
   W. L.; Zhou, X. Z.; Daly, P. W.
2005GeoRL..32.1105R    Altcode: 2005GeoRL..3201105R
  Based on the energetic particle measurements obtained by Cluster/RAPID
  (Research with Adaptive Particle Imaging Detectors), ion composition
  variations in the plasma sheet have been investigated. By comparing
  observations during quiet and storm intervals, it is found that,
  in addition to the enhanced energy density for all ion species, the
  ratio of energetic O<SUP>+</SUP> ions to protons shows an increase
  during geomagnetic active periods in the near-Earth plasma sheet
  (-15 R<SUB>E</SUB> &lt; X &lt; -12 R<SUB>E</SUB>). However, the ratio
  shows a decrease in the middle plasma sheet (-19 R<SUB>E</SUB> &lt;
  X &lt; -15 R<SUB>E</SUB>). These observation results have been further
  confirmed by a statistical study of all the plasma sheet crossing
  events from 2001 to 2003. Observations also show that energetic
  particles embedded in the earthward high-speed streams observed in
  the plasma sheet have an obvious low abundance of heavy ions compared
  with surrounding plasmas. It is implied that energetic O<SUP>+</SUP>
  ions could be distributed in a limited region in the plasma sheet and
  much less ionosphere origin particles could reach the region beyond
  X = -15 R<SUB>E</SUB>. Bursty Bulk Flows (BBFs) could not supply more
  energetic O<SUP>+</SUP> ions to the near-Earth plasma sheet, whereas
  the ionospheric supplement, together with local acceleration processes,
  leads to an enhanced oxygen abundance during active times.

---------------------------------------------------------
Title: Canadian space environment program and international living
    with a star
Authors: Liu, W. William
2005AdSpR..35...51L    Altcode:
  Canada has a vibrant and balanced research program in the space
  environment discipline. Two major thrusts are manifested in the
  current program direction, the integration of ground instruments for
  the remote-sensing of the magnetosphere-ionosphere system (geospace
  monitoring), and the development and flight of a small satellite for
  the study of particle acceleration and radio tomography in the auroral
  ionosphere (enhanced polar outflow probe). A general description of
  the mission science objectives is given. These and other potential
  Canadian contributions are discussed in the context of international
  living with a star.

---------------------------------------------------------
Title: A study of the freshwater discharge from the Amazon River
    into the tropical Atlantic using multi-sensor data
Authors: Jo, Young-Heon; Yan, Xiao-Hai; Dzwonkowski, Brian; Liu,
   W. Timothy
2005GeoRL..32.2605J    Altcode: 2005GeoRL..3202605J
  We study freshwater discharge from the Amazon River into the tropical
  Atlantic using monthly mean multi-sensor data from September 1997
  to July 2003. In order to demonstrate freshwater discharge, we used
  chlorophyll concentration (Chl_a) and diffuse attenuation coefficient
  (DAC) measured by the Sea-viewing Wide Field-of-view Sensor (SeaWiFS),
  and salt steric height anomaly (Δη'<SUB>S</SUB>) derived from
  Integrated Multi-Sensor Data Analysis (IMSDA). IMSDA was obtained from
  estimating the long term-time series of Δη'<SUB>S</SUB> by removing
  the thermal steric height anomaly (η'<SUB>T</SUB>) from altimetry
  data. Comparisons of long-term time series of Δη'<SUB>S</SUB>, Chl_a,
  and DAC were made with mooring data at 8°N, 38°W, which were highly
  correlated. There are three- to five-month lags between the Amazon
  River discharge and 4°N latitude estimated from latitude-time diagram
  derived from SeaWiFS measurements.

---------------------------------------------------------
Title: Energization of the Inner Magnetosphere by Solar Wind
    Pressure Pulses
Authors: Liu, W. William
2005GMS...155..113L    Altcode:
  Geomagnetic storms involve the entry of a prodigious amount of energy
  into the inner magnetosphere. Despite decades of research, there remain
  serious, if often overlooked, gaps in our understanding of how energy
  transport is effected in the storm process. A minimal theory of storm
  energization must explain the following observations: 1) The timescale
  of energization is shorter than that of radial diffusion and perhaps
  also convection; 2) the energization favors the ring current region
  (L≤5) and 3) the transferred energy is of a significant magnitude, on
  the order of 10<SUP>15</SUP> J or more. Resonant magnetospheric coupling
  with solar wind pressure pulses has been considered in the past as a
  candidate mechanism for the energy transfer; however, this view has not
  been elaborated quantitatively to show that the mechanism is powerful
  enough to meet the energy requirement of a storm. In this paper, we
  construct a theoretical model to show that pressure pulse coupling can
  attain the requisite magnitude to provide for storm-time energization.

---------------------------------------------------------
Title: Multiscale Geospace Physics in Canada
Authors: Liu, W.; Burchill, J.; Cogger, L.; Donovan, E.; James, G.;
   Kendall, D.; Knudsen, D.; Lu, J.; Mann, I.; Michaud, R.; Murphree, S.;
   Rankin, R.; Samson, J.; Spanswick, E.; Sofko, G.; Trondsen, T.; Yau, A.
2005mcsp.conf..487L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Four Years of Nulling Interferometry: A Summary of Results
    Since PPIV
Authors: Liu, W. M.; Hinz, P. M.; Hoffmann, W. F.; Meyer, M. R.;
   Mamajek, E. E.; Mmt Adaptive Optics Group
2005prpl.conf.8564L    Altcode: 2005LPICo1286.8564L
  No abstract at ADS

---------------------------------------------------------
Title: Spatial distribution of energetic ion compositions in the
    plasma sheet observed by Cluster/RAPID
Authors: Yang, J.; Fu, S.; Liu, W.; Ruan, P.; Pu, Z.; Daly, P.;
   Wang, Y.
2005ChJGC..48.1226Y    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Near-Infrared Synchrotron Spectral Index of Cassiopeia A
Authors: Eriksen, K. A.; McCarthy, D. W.; Liu, W. M.
2004AAS...205.7001E    Altcode: 2004BAAS...36.1462E
  We report on our observations of diffuse near-infrared emission in the
  young supernova remnant Cassiopeia A with the PISCES infrared camera on
  the University of Arizona Bok 2.3 meter telescope. While previous K-band
  imaging (Gerardy and Fesen 2001) and polarimetry (Jones et al. 2003)
  confirms its synchrotron origin, our J and H detections allow us to
  measure the first near-infrared spectral index for this emission. We
  compare our results with radio, microwave, and X-ray observations,
  and discuss the implications for models of diffusive shock acceleration
  of cosmic rays.

---------------------------------------------------------
Title: The Princeton Magnetorotational Instability Experiment:
    Overview and Initial Results
Authors: Burin, M. J.; Goodman, J.; Ji, H.; Schartman, E.; Liu, W.
2004AAS...205.0702B    Altcode: 2004AAS...205..702B; 2004BAAS...36.1346B
  Accretion disk turbulence is thought to be governed by the
  magnetorotational instability (MRI). To date however there has been no
  clear experimental demonstration of this instability, though it appears
  plausible to do so via a suitably designed laboratory apparatus. To
  this end a modified Taylor-Couette apparatus, to be filled with a liquid
  gallium alloy and placed within a magnetic field, has been designed and
  built. Here we discuss various engineering challenges of the design,
  and detail the controls, diagnostics, and data acquisition methods
  of the experiment. We also review some supportive numerical modeling
  work. In preparation for MRI studies with gallium we have tested
  the device with water. The data resulting from these initial studies
  bears upon recent work involving nonlinear hydrodynamic instabilities,
  which may be a competing mechanism in cool accretion disks. This work
  is supported by DoE, NSF, and NASA.

---------------------------------------------------------
Title: Adaptive Optics Nulling Interferometric Observations of AB
Aur and V892 Tau: Resolved Disks in the Mid-IR
Authors: Liu, W. M.; Hinz, P. M.; Hoffmann, W. F.; Brusa, G.; Miller,
   D.; Kenworthy, M. A.
2004AAS...205.1716L    Altcode: 2004BAAS...36.1367L
  We present the results of adaptive optics nulling interferometric
  observations of two Herbig Ae stars, AB Aur and V892 Tau, at 10.3
  microns. Our observations show resolved circumstellar emission from both
  sources. The emission from AB Aur suggests that there is an inclined
  disk surrounding the star. The diameter of the disk is derived to
  be 24 to 30 AU with an inclination of 45 to 65 degrees from face-on,
  and a major-axis PA of 30 +/- 15 degrees (E of N). Differences in the
  physical characteristics between the mid-IR emission and emission at
  other wavelengths found in previous studies suggest a complex structure
  for AB Aur's circumstellar environment, which may not be explained by
  a disk alone. The similarity in the observed size of AB Aur's resolved
  emission and that of another Herbig Ae star, HD 100546, is likely
  coincidental, as their respective evolutionary states and spectral
  energy distributions suggest significantly different circumstellar
  environments. <P />The PI was supported under a Michelson Graduate
  Fellowship

---------------------------------------------------------
Title: Geomagnetic Activity Dependence of the Ratio N+/O+ in the
    Ring Current
Authors: Fu, S.; Liu, W.; Zong, Q.; Pu, Z.; Ruan, P.
2004AGUFMSM13A1182F    Altcode:
  Based on the energetic particle measurement obtained by
  CRRES/MICS, ion composition variations in the ring current have been
  investigated. Observation shows that in addition to O+ and H+, N+ ions
  are also an important composition in the ring current region. The ratio
  of N+/O+ during geomagnetic quiet times is about 0.26, while a smaller
  valued could be found for strong active times. The variation of the
  ratio follows the same trace as the Dst index. Through a statistic
  study, it is demonstrated that the ratio of N+/O+ decreases with an
  enhanced geomagnetic activity for strong storms, whereas for small
  storms, there is no obvious correlations of the ratio to the activity
  level. Based on the IRI model, we show that different ion species reach
  their peak values at different altitude. The maximum of oxygen ions
  sit in a lower altitude than that of nitrogen ions. It is thus implied
  that the altitude of the ion up-flowing in the ionosphere is closely
  related to the geomagnetic activity. The stronger storms, the lower
  ionosphere could be involved in the magnetosphere-ionosphere coupling.

---------------------------------------------------------
Title: Magnetorotational Instability in a Short Couette Flow of
    Liquid Gallium
Authors: Ji, Hantao; Goodman, Jeremy; Kageyama, Akira; Burin, Michael;
   Schartman, Ethan; Liu, Wei
2004AIPC..733...21J    Altcode:
  A concise review is given of an experimental project to study
  magnetorotational instability (MRI) in a short Couette geometry
  using liquid gallium. Motivated by the astrophysical importance and
  lack of direct observation of MRI in nature and in the laboratory, a
  theoretical stability analysis was performed to predict the required
  experimental parameters. Despite the long-wavelength nature of MRI,
  local analysis agrees excellently with global eigenmode calculations
  when periodic boundary conditions are used in the axial direction. To
  explore the effects of rigidly rotating vertical boundaries (endcaps),
  a prototype water experiment was conducted using dimensions and
  rotation rates favored by the above analysis. Significant deviations
  from the expected Couette flow profiles were found. The cause of the
  discrepancy was investigated by nonlinear hydrodynamic simulations using
  realistic boundary conditions. It was found that Ekman circulation
  driven by the endcaps transports angular momentum and qualitatively
  modifies the azimuthal flow. Based on this new understanding, a new
  design was made to incorporate two independently driven rings at each
  endcap. Simulations were used to optimize the design by minimizing
  Ekman circulation while remaining within engineering capabilities. The
  new apparatus, which has been constructed and assembled, is currently
  being tested with water and will be ready for the MRI experiment
  with gallium soon. This development process illustrates the value of
  interplay between experiment, simulation, and analytic insight.

---------------------------------------------------------
Title: Princeton Magnetorotational Instability Experiment ---
    Background and Overview
Authors: Ji, H.; Burin, M.; Schartman, E.; Raftopoulos, S.; Cutler,
   R.; Heitzenroeder, P.; Liu, W.; Goodman, J.; Stone, J.; Kageyama, A.
2004APS..DPPEP1004J    Altcode:
  The magnetorotational instability (MRI) has been proposed as
  a dominant mechanism for rapid angular momentum transport in
  electrically-conducting accretion disks ranging from quasars
  and X-ray binaries to cataclysmic variables and perhaps even
  protoplanetary disks. Despite its popularity, however, the MRI has
  never been clearly demonstrated and studied in the laboratory. Based
  on theoretical analysis(H. Ji, J. Goodman, and A. Kageyama,
  Mon. Not. Roy. Astron. Soc. 325), L1(2001); J. Goodman and H. Ji,
  J. Fluid Mech. 462, 365(2002). and the results from prototype water
  experiments and hydrodynamic simulations(A. Kageyama, et al.), to
  be published in J. Phys. Soc. Jpn. (2004)., we have constructed
  a short Couette flow apparatus with two differentially rotating
  rings at each end of the flow to minimize the Ekman effect. Liquid
  gallium alloy is used after initial water tests. A computer-based
  control and data acquisition system is implemented to achieve reliable
  operations. Signatures of the MRI are monitored by diagnostics measuring
  torque coupling between rotating components, as well as magnetic and
  pressure perturbations, and internal velocity. Our main objectives are
  (1) to clearly demonstrate MRI; (2) to study its nonlinear behavior
  and angular momentum transport; (3) to compare with state-of-the-art
  simulations similar to those used in astrophysical disks. This work
  is supported by DoE, NSF, and NASA.

---------------------------------------------------------
Title: RHESSI Observations of a Simple Large X-Ray Flare on 2003
    November 3
Authors: Liu, Wei; Jiang, Yan Wei; Liu, Siming; Petrosian, Vahé
2004ApJ...611L..53L    Altcode: 2004astro.ph..1381L
  We present data analysis and interpretation of a simple X-class flare
  observed with RHESSI on 2003 November 3. In contrast to other X-class
  flares observed previously, this flare shows a very simple morphology
  with well-defined looptop (LT) and footpoint (FP) sources. The almost
  monotonic upward motion of the LT source and increase in separation of
  the two FP sources are consistent with magnetic reconnection models
  proposed for solar flares. In addition, we find that the source
  motions are relatively slower during the more active phases of hard
  X-ray emission; the emission centroid of the LT source shifts toward
  higher altitudes with the increase of energy; and the separation
  between the LT emission centroids at two different photon energies
  is anticorrelated with the FP flux. Nonuniformity of the reconnecting
  magnetic fields could be a possible explanation of these features.

---------------------------------------------------------
Title: The  <SUP>21 </SUP><SUB> </SUB>Na (p,γ) <SUP>22 </SUP><SUB>
    </SUB>Mg  reaction from E<SUB>c.m.</SUB> =200  to  1103 keV  in
    novae and x-ray bursts
Authors: D'Auria, J. M.; Azuma, R. E.; Bishop, S.; Buchmann, L.;
   Chatterjee, M. L.; Chen, A. A.; Engel, S.; Gigliotti, D.; Greife,
   U.; Hunter, D.; Hussein, A.; Hutcheon, D.; Jewett, C. C.; José, J.;
   King, J. D.; Laird, A. M.; Lamey, M.; Lewis, R.; Liu, W.; Olin, A.;
   Ottewell, D.; Parker, P.; Rogers, J.; Ruiz, C.; Trinczek, M.; Wrede, C.
2004PhRvC..69f5803D    Altcode:
  The long-lived radioactive nuclide <SUP>22 </SUP><SUB> </SUB>Na (
  t<SUB>1/2</SUB> =2.6 yr) is an astronomical observable for understanding
  the physical processes of oxygen-neon novae. Yields of <SUP>22</SUP>Na
  in these events are sensitive to the unknown total rate of the <SUP>21
  </SUP><SUB> </SUB>Na (p,γ) <SUP>22 </SUP><SUB> </SUB>Mg reaction. Using
  a high intensity <SUP>21 </SUP><SUB> </SUB>Na beam at the TRIUMF-ISAC
  facility, the strengths of seven resonances in <SUP>22 </SUP><SUB>
  </SUB>Mg , of potential astrophysical importance, have been directly
  measured at center of mass energies from E<SUB>c.m.</SUB> =200 to
  1103 keV . We report the results obtained for these resonances and
  their respective contributions to the <SUP>21 </SUP><SUB> </SUB>Na
  (p,γ) <SUP>22 </SUP><SUB> </SUB>Mg rate in novae and x-ray bursts,
  and their impact on <SUP>22 </SUP><SUB> </SUB>Na production in novae.

---------------------------------------------------------
Title: Evolution of the Loop Top Source of Solar Flares --- Heating
    and Cooling Processes
Authors: Jiang, Y. W.; Liu, S. M.; Liu, W.; Petrosian, V.
2004AAS...204.9805J    Altcode: 2004BAAS...36..985J
  We present a study of the spectral evolution of the loop top (LT)
  sources of a sample of solar flares observed by RHESSI. Distinct LT
  sources are seen in many flares from the pre-heating to the decay
  phase. In most cases, their spectrum can be fitted with either a
  thermal or a power law model. The spectra of preheating phase are
  somewhat complex. While the impulsive phase spectra seem fit a power
  law better. The LT source in decay phase can be well described as a
  thermal source. The temperature obtained from the thermal fit decays
  10 times faster than that expected from radiative cooling but 10 times
  slower than that due to conduction cooling along the loops. This can
  come about as a combined result of continuous heating and suppression
  of conductivity along the loop. Both these effects can be produced
  by turbulence. Implication of this process as the so-called Neupert
  effects will also be discussed.

---------------------------------------------------------
Title: Source Motions and Foot-point Asymmetries in the 2003
    October-November X-class Flares Observed by RHESSI
Authors: Liu, W.; Jiang, Y. W.; Liu, S.; Petrosian, V.
2004AAS...204.4714L    Altcode: 2004BAAS...36..739L
  Motions and flux asymmetries of foot-point (FP) sources and related
  motions of loop-top (LT) sources play essential roles in understanding
  the energy release, particle acceleration, and transport processes
  in solar flares. During the October-November 2003 storms, 12 X-class
  flares, occurring at different locations across the solar disk,
  were observed by the high resolution spectroscopic imager, RHESSI,
  with generally good coverage. This provides an excellent opportunity
  for a comprehensive investigation of these flare characteristics. For
  a selected sample of these flares, we study the motions of the LT and
  FP sources. We use the component maps of images obtained by the CLEAN
  algorithm to determine the brightness-weighted centroids of the HXR
  sources and compare them with the corresponding peak positions. The
  sources are well defined in these maps, where there is no residual
  which is usually added back to the resulting CLEAN images and makes
  it difficult to infer accurate source centroids. The FP motions are
  combined with the SOHO/MDI magnetograms to estimate the electric field
  along the reconnecting current sheet. We also study the flux asymmetries
  between the conjugate FPs, using the more computationally intensive
  PIXON algorithm. A comparison between the results obtained with CLEAN
  and PIXON will be presented, and implications for particle acceleration
  processes and other theoretical aspects of solar flares will be
  discussed as well. The work is supported by NASA grants NAG5-12111,
  NAG5 11918-1, and NSF grant ATM-0312344 at Stanford University.

---------------------------------------------------------
Title: Systematic error of microwave scatterometer wind related to
    the basin-scale plankton bloom
Authors: Hashizume, Hiroshi; Liu, W. Timothy
2004GeoRL..31.6307H    Altcode: 2004GeoRL..3106307H
  Chlorophyll-a concentration derived from satellite ocean color
  sensor are compared with coincident wind speed difference between
  microwave scatterometer QuikSCAT product and reanalysis product
  from the National Center for Environmental Prediction over global
  oceans. The objective is to explore if a natural surface film, which
  originates in biological productivity, causes the underestimation
  of surface wind in scatterometer measurement by damping the small
  capillary wave through the surface tension. The wind speed difference
  (Reanalysis wind - QuikSCAT wind) is found to correlate positively
  with chlorophyll-a over the biologically highly productive areas,
  especially from intra-seasonal to seasonal time scales, indicating
  the surface film effect. The wind speed difference increases from ~-1
  m s<SUP>-1</SUP> to ~0.5 m s<SUP>-1</SUP> as chlorophyll-a increases
  from ~0.1 mg m<SUP>-3</SUP> to ~3 mg m<SUP>-3</SUP>, which is comparable
  with the results of previous laboratory experiments with artificial oil.

---------------------------------------------------------
Title: The Canadian Enhanced Polar Outflow Probe (e-POP) Mission
    in ILWS
Authors: Yau, A. W.; James, H. G.; Liu, W.
2004cosp...35.1871Y    Altcode: 2004cosp.meet.1871Y
  The Enhanced Polar Outflow Probe (e-POP) small satellite mission will be
  Canada's first mission contribution to the International Living with a
  Star (ILWS) initiative. The e-POP project comprises three important and
  interconnected components: a small-satellite component to investigate
  atmospheric and plasma flows and related wave-particle interaction
  processes in the topside ionosphere, coordinated ground-based
  measurements and a theoretical simulation component. Its scientific
  objectives are to quantify the micro-scale characteristics of plasma
  outflow and related micro- and meso-scale plasma processes in the polar
  ionosphere, explore the occurrence morphology of neutral escape in the
  upper atmosphere, and study the effects of auroral currents on plasma
  outflow and those of plasma microstructures on radio propagation. The
  escape of plasma from the polar ionosphere - and its subsequent
  acceleration and transport towards the magnetosphere - is one of the
  most important processes in the Ionosphere-Thermosphere-Magnetosphere
  system. The e-POP science instrument payload will carry a suite of 8
  scientific instruments, including imaging plasma and neutral particle
  sensors, magnetometers, dual-frequency GPS receivers, CCD cameras,
  a radio wave receiver and a beacon transmitter. The imaging plasma
  sensors will measure particle distributions and the magnetometers
  field-aligned currents on a time scale of 10 ms and a spatial scale
  of (100 m. The CCD cameras will perform auroral imaging on a time
  scale of 100 ms. The radio wave and GPS receivers will perform near
  real-time imaging of the ionosphere in conjunction with ground-based
  radars, and the beacon transmitter in conjunction with ground receiving
  stations. The e-POP payload is scheduled for launch in early 2007 as
  part of the Canadian CASSIOPE multi-purpose small satellite, and will
  be placed in a low-altitude, elliptical polar orbit (80( inclination,
  300 km perigee, and 1500 km apogee). e-POP will utilize the companion
  communications technology demonstration payload onboard the satellite
  bus, and use both S-band and Ka-band telemetry downlink at a maximum
  rate of 30 Mbit/s, to support the large volume (up to 20 GBytes/day)
  of high-resolution science data that it generates.

---------------------------------------------------------
Title: Comparison of photometer and global MHD determination of the
    open-closed field line boundary
Authors: Rae, I. J.; Kabin, K.; Rankin, R.; Fenrich, F. R.; Liu, W.;
   Wanliss, J. A.; Ridley, A. J.; Gombosi, T. I.; de Zeeuw, D. L.
2004JGRA..109.1204R    Altcode:
  We compare open-closed field line boundary positions from the
  BATS-R-US Global MHD model and CANOPUS photometer measurements of
  red-line emissions. We choose intervals of steady interplanetary
  and ionospheric conditions in order to adhere to the "steady-state"
  picture that we are trying to address. Nine intervals are chosen that
  correspond to stable IMF and auroral conditions that can be simulated
  with the MHD model. We find that on average, the steady-state BATS-R-US
  MHD model provides an excellent estimate of the open-closed field line
  boundary proxy as determined by the red-line auroral emissions. Typical
  errors between the model calculations of the open-closed field line
  boundary and the observations are within the inherent error in using
  the red-line emissions.

---------------------------------------------------------
Title: International Living With a Star: The road ahead
Authors: Liu, W.
2004cosp...35.2296L    Altcode: 2004cosp.meet.2296L
  Entering into its second year, International Living With a Star has been
  a remarkable success, with approximately 30 member organizations now
  part of the program. As solar-terrestrial science enters into a period
  of uncertainty, the raison d'etre of ILWS has become more compelling,
  and its strategic importance more obvious. In the coming months, ILWS
  will begin work on 1) formulating and advancing the political argument
  for continued support of solar terrestrial science and 2) developing
  a compelling scientific vision which will excite and challenge the
  scientific community on an international scale. To succeed in either,
  ILWS requires active participation and support from the scientists. In
  this talk, I present the major findings and results of the Second ILWS
  Working Group meeting held in Banff, Canada on May 25 and 26, 2004. I
  further invite all scientists to inject their thoughts and suggestions,
  as we move forward on this crucial international collaboration.

---------------------------------------------------------
Title: Excitation of Non-Atmospheric Polar Motion by the Migration
    of the Pacific Warm Pool
Authors: Yan, X.; Zhou, Y.; Zheng, D.; Liao, X.; Ding, X.; Pan, J.;
   Fang, M.; He, M.; Liu, W.
2003AGUFM.G22C0317Y    Altcode:
  Changes in the annual variation of the Earth's polar motion are found to
  be largely caused by the variation of the atmospheric angular momentum
  (AAM). Recent simulation results of oceanic general circulation models
  further suggested global oceanic effects on the annual polar motion
  other than the atmosphere. In parallel to previous model studies
  of global oceanic effect, this research particularly singles out
  an active large-scale ocean anomaly and investigates its effect on
  the annual polar motion, determined from satellite observations of
  the movement of the Western Pacific Warm Pool (WPWP). Although the
  scale of the warm pool is much smaller than that of the solid Earth,
  analysis of the non-atmospheric polar motion excitation has shown that
  the WPWP does contribute non-negligible effects to the annual polar
  motion. The analysis consisted of over thirty years of the WPWP data
  (1970-2000) and shows the polar motion excitation is (2.5mas, -78o)
  for the x-component and (0.1mas, -14o) for the y-component. Comparing
  this result with the total geodetic non-atmospheric polar motion
  excitation of (10.3mas, 59o) for the x-component and (10.6mas, 62o)
  for the y-component, shows the significance of the WPWP. The difference
  between the WPWP's excitation on (x, y) components of the polar motion
  may originate from the WPWP's location and general pattern. Changes
  in the Earth's polar motion has attracted significant attention, not
  only because it is an important geodetic issue, but also because it
  has significant value as a global measure of variations within the
  hydrosphere, atmosphere, cryosphere, and solid Earth; hence global
  changes. Key Words. Polar motion - Western Pacific Warm Pool

---------------------------------------------------------
Title: A Resolved Circumstellar Disk around the Herbig Ae Star HD
    100546 in the Thermal Infrared
Authors: Liu, W. M.; Hinz, P. M.; Meyer, M. R.; Mamajek, E. E.;
   Hoffmann, W. F.; Hora, J. L.
2003AAS...203.1304L    Altcode: 2003BAAS...35.1226L
  We present mid-infrared nulling interferometric and direct imaging
  observations of the Herbig Ae star HD 100546 obtained with the Magellan
  I (Baade) 6.5 m telescope. The observations show resolved circumstellar
  emission at 10.3, 11.7, 12.5, 18.0, and 24.5 microns. Through the
  nulling observations (10.3, 11.7 and 12.5 microns), we detect a
  circumstellar disk, with an inclination of 45 ± 15 degrees with respect
  to a face-on disk, a semimajor axis position angle of 150 ± 10 degrees
  (E of N), and a spatial extent of about 25 AU. The direct images (18.0
  and 24.5 microns) show evidence for cooler dust with a spatial extent
  of 30-40 AU from the star. The direct images also show evidence for an
  inclined disk with a similar position angle as the disk detected by
  nulling. This morphology is consistent with models in which a flared
  circumstellar disk dominates the emission. However, the similarity
  in relative disk size we derive for different wavelengths suggests
  that the disk may have a large inner gap, possibly cleared out by the
  formation of a giant protoplanet. The existence of a protoplanet in the
  system also provides a natural explanation for the observed difference
  between HD 100546 and other Herbig Ae stars.

---------------------------------------------------------
Title: Temporal and Spatial Structure of Substorm Associated High
    Energy Particle Precipitation
Authors: Spanswick, E.; Donovan, E.; Liu, W.; Hiebert, T.; Henderson,
   M.; Wallis, D.; Honary, F.
2003AGUFMSM51B0528S    Altcode:
  The evolution of the high-energy electron population through the
  substorm cycle has been studied directly with in situ observations
  such as those provided by the LANL-SOPA instruments, and indirectly
  through precipitation seen via riometers, X-ray imagers, and other
  instruments. Ground-based and other remote sensing techniques provide
  the advantage of being able to track such disturbances in both space
  and time, with caveats including the fact that information about
  the energy of the precipitating particles is limited. Using data
  from the 13 instrument NORSTAR (formerly CANOPUS) riometer array in
  north-central Canada, we are examining a large number of substorm
  events. We are focussing on a transient “spike” of significant
  absorption that occurs during most substorm expansive phases. Seen
  from any one station, the spike lasts several minutes. More globally,
  it typically takes tens of minutes to propagate across the NORSTAR
  array. The propagation is in general a combination of azimuthal (ie.,
  East or West) and poleward. In this paper, we present a statistical
  comparision between the propagation characteristics of the spike and
  other substorm features such as dipolarization, auroral bulge, Pi2s,
  and injections. As well, we present a detailed analysis of several
  events. Our objective is to determine the magnetospheric source of
  this transient high energy precipitation.

---------------------------------------------------------
Title: Increasing Tracking Bandwidth for Deep-Space Optical
    Communications Using Linear Accelerometers
Authors: Lee, S.; Ortiz, G. G.; Liu, W.; Garkanian, V.
2003IPNPR.155H...1L    Altcode:
  In deep-space optical communications, acquisition, tracking, and
  pointing are all challenging because of the stringent -- on the
  order of submicroradian -- pointing requirement. To achieve this
  level of pointing accuracy, one must maintain high-bandwidth tracking
  control. Feasible tracking sources (beacons) include uplink laser beams
  and celestial objects such as the Earth, Moon, and stars. However,
  these tracking sources do not all provide the kilohertz tracking
  rate needed for pointing in deep space. One approach to enable a high
  tracking rate is to augment the tracking loop with inertial sensors
  to estimate high-frequency beacon movements. In this article, we
  discuss the use of linear accelerometers, mounted in a configuration
  to measure angular displacement, to achieve high-bandwidth tracking
  with dim beacon sources. The advantages of linear accelerometers (or
  angular accelerometers) are their low cost, high bandwidth, and small
  size compared with other inertial sensors such as gyros. Simulation
  and experimental results show good agreement. A tracking bandwidth
  increase of 11 times is demonstrated.

---------------------------------------------------------
Title: Effects of magnetic topology on CME kinematic properties
Authors: Liu, Wei; Zhao, Xue Pu; Wu, S. T.; Scherrer, Philip
2003ESASP.535..459L    Altcode: 2003iscs.symp..459L
  Coronal Mass Ejections (CMEs) exhibit two types of kinematic property:
  fast CMEs with high initial speeds and slow CMEs with low initial speeds
  but gradual accelerations. To account for this dual character. Low and
  Zhang (LZ 2002) proposed that fast and slow CMEs result from initial
  states with magnetic configurations characterized by normal and inverse
  quiescent prominences, respectively. To test their theory and further
  explore the effects of topology on the kinematic properties of CMEs we
  employed a self-consistent magnetohydrodynamic (MHD) model [Guo, Wu, et
  al.] to simulate the evolution of CMEs respectively in the normal and
  inverse prominence environments. The numerical results show that CMEs
  originating from a normal prominence environment do have higher initial
  speeds than those from an inverse one. In addition, our simulations
  demonstrate the distinct roles played by magnetic reconnection in
  these two topologically different magnetic environments to produce
  the two different CME height-time profiles as suggested by LZ 2002.

---------------------------------------------------------
Title: Exact soliton solution and inelastic two-soliton collision
    in a spin chain driven by a time-dependent magnetic field
Authors: Li, Zai-Dong; Li, Lu; Liu, W. M.; Liang, Jiu-Qing; Ziman, T.
2003PhRvE..68c6102L    Altcode: 2005cond.mat..6102L
  We investigate dynamics of exact N-soliton trains in a spin chain driven
  by a time-dependent magnetic field by means of an inverse scattering
  transformation. The one-soliton solution indicates obviously the spin
  precession around the magnetic field and periodic shape variation
  induced by the time-varying field as well. In terms of the general
  soliton solutions, N-soliton interaction and particularly various
  two-soliton collisions are analyzed. The inelastic collision by which
  we mean the soliton shape change before and after collision appears
  is generally due to the time-varying field. We, moreover, show that
  complete inelastic collisions can be achieved by adjusting spectrum
  and field parameters. This may lead to a potential technique of shape
  control of soliton.

---------------------------------------------------------
Title: Air-sea interaction at an oceanic front: Implications for
    frontogenesis and primary production
Authors: Chen, Dake; Liu, W. Timothy; Tang, Wenqing; Wang, Zhiren
2003GeoRL..30.1745C    Altcode: 2003GeoRL..30nOCE3C
  Based on recent satellite observations, we hypothesize that there exists
  a significant air-sea interaction at the shelf-break front in the East
  China Sea. An idealized ocean-atmosphere coupled model was designed
  to test this hypothesis and to study the physical processes involved
  in such an interaction, with emphasis on the oceanic part. A positive
  feedback between ocean and atmosphere was identified in the model and
  its consequences were evaluated. We found that air-sea interaction,
  when combined with sloping topography, could provide a mechanism for
  the genesis of the shelf-break front. The resulting frontal circulation
  and vertical mixing could bring nutrient-rich subsurface water into
  the surface euphotic zone, thus making the frontal region a conspicuous
  place for primary production.

---------------------------------------------------------
Title: First evidence for the detection of natural surface films by
    the QuikSCAT scatterometer
Authors: Lin, I. -I.; Alpers, Werner; Liu, W. Timothy
2003GeoRL..30.1713L    Altcode: 2003GeoRL..30m..46L
  For the first time it is demonstrated that with the QuikSCAT
  scatterometer it is possible to detect natural surface films
  resulting from enhanced biological activity in the ocean. It is
  shown for two regions in the Norwegian and Baltic Sea that areas
  of strongly reduced Normalized Radar Cross Section (NRCS) are
  associated with areas of enhanced chlorophyll-a concentration as
  evidenced by quasi-simultaneously acquired SeaWiFS data. This result
  has two implications. Firstly, it opens up the possibility to map
  globally natural surface film coverage using QuikSCAT data. Secondly,
  it demonstrates that in ocean areas with high biological activity
  the presence of natural surface films can give rise to significant
  errors in wind vector retrieval when using the current QuikSCAT wind
  retrieval algorithm.

---------------------------------------------------------
Title: Breached Pairing Superfluidity: Possible Realization in QCD
Authors: Gubankova, Elena; Liu, W. Vincent; Wilczek, Frank
2003PhRvL..91c2001G    Altcode: 2003hep.ph....4016G
  We propose a wide universality class of gapless superfluids,
  and analyze a limit that might be realized in quark matter at
  intermediate densities. In the breached pairing color superconducting
  phase heavy s quarks, with a small Fermi surface, pair with light
  u or d quarks. The ground state has a superfluid and a normal Fermi
  component simultaneously. We expect a second-order phase transition,
  as a function of increasing density, from the breached pairing phase
  to the conventional color-flavor locked phase.

---------------------------------------------------------
Title: New evidence for enhanced ocean primary production triggered
    by tropical cyclone
Authors: Lin, I.; Liu, W. Timothy; Wu, Chun-Chieh; Wong, George T. F.;
   Hu, Chuanmin; Chen, Zhiqiang; Liang, Wen-Der; Yang, Yih; Liu, Kon-Kee
2003GeoRL..30.1718L    Altcode: 2003GeoRL..30m..51L
  New evidence based on recent satellite data is presented to provide
  a rare opportunity in quantifying the long-speculated contribution of
  tropical cyclones to enhance ocean primary production. In July 2000,
  moderate cyclone Kai-Tak passed over the South China Sea (SCS). During
  its short 3-day stay, Kai-Tak triggered an average 30-fold increase
  in surface chlorophyll-a concentration. The estimated carbon fixation
  resulting from this event alone is 0.8 Mt, or 2-4% of SCS's annual
  new production. Given an average of 14 cyclones passing over the
  SCS annually, we suggest the long-neglected contribution of tropical
  cyclones to SCS's annual new production may be as much as 20-30%.

---------------------------------------------------------
Title: A linear relationship between ENSO intensity and tropical
    instability wave activity in the eastern Pacific Ocean
Authors: Yu, Jin-Yi; Liu, W. Timothy
2003GeoRL..30.1735Y    Altcode: 2003GeoRL..30nCLM5Y
  The interannual variations of tropical instability waves (TIWs) in
  the eastern Pacific Ocean and their relationships with ENSO intensity
  are studied using a 28-year long coupled atmosphere-ocean general
  circulation model (CGCM) simulation. The activity of TIWs is measured by
  the root-mean-square value of the 50-day high-pass filtered sea surface
  temperature (SST) perturbations produced in the simulation. The CGCM
  realistically produces two branches of large TIW activity near the
  equator: one at 2°N and the other at 2°S. It is found that along
  both branches there are linear relationships between the year-to-year
  variations of TIW activity and those of ENSO intensity. TIW activity
  is enhanced or reduced in proportion to the NINO3 SST anomalies, with
  larger activity in La Niña years and smaller activity in El Niño
  years. It is found that ENSO modulates TIW activity in both branches
  primarily by changing the latitudinal SST gradient associated with the
  SST front immediately north of the equator. Weaker correlations are
  found between the year-to-year variations of TIW activity and those of
  the ocean current shears between the south equatorial current and the
  equatorial undercurrent or the north equatorial countercurrent. This
  CGCM study suggests that the baroclinic instability associated with
  the northern SST front is a major generation mechanism for both the
  northern and southern TIW branches in the eastern Pacific Ocean.

---------------------------------------------------------
Title: Erratum: <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg Reaction and
    Oxygen-Neon Novae [Phys. Rev. Lett. 90, 162501 (2003)]
Authors: Bishop, S.; Azuma, R. E.; Buchmann, L.; Chen, A. A.;
   Chatterjee, M. L.; D'Auria, J. M.; Engel, S.; Gigliotti, D.; Greife,
   U.; Hernanz, M.; Hunter, D.; Hussein, A.; Hutcheon, D.; Jewett, C.;
   José, J.; King, J.; Kubono, S.; Laird, A. M.; Lamey, M.; Lewis,
   R.; Liu, W.; Michimasa, S.; Olin, A.; Ottewell, D.; Parker, P. D.;
   Rogers, J. G.; Strieder, F.; Wrede, C.
2003PhRvL..90v9902B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Statistical Study of Limb Flares Observed by RHESSI:
    Relative Spectra of loop top and footpoint sources
Authors: Jiang, Y. W.; Liu, W.; Petrosian, V.; McTiernan, J.
2003SPD....34.1803J    Altcode: 2003BAAS...35..840J
  Hard X-ray observations of YOHKOH/HXT and preliminary data form RHESSI
  have shown that the spectra and intensities from loop top sources
  are different from those at footpoints. These differences provide
  a great insight into the mechanism of the electron acceleration
  process and physical conditions of the flare loop. We have begun the
  investigation of a sample of limb flares observed by RHESSI. Using the
  imaging analysis described in the accompanying paper, we select flares
  with well-defined loop top and footpoint sources and calculate their
  relative intensities and spectra. The results from these and previous
  observations will be compared with the predictions of the stochastic
  acceleration model with the aim of constraining acceleration and its
  model parameters. <P />The work at Stanford is supported by NASA grants
  NAG5-12111, NAG5 11918-1, and SUB2001-402-01 through the University
  of Alabama in Huntsville (PI: J. Miller). J. McTiernan would like to
  acknowledge support from grant NAS5-98033-05/03.

---------------------------------------------------------
Title: The DRAGON facility for nuclear astrophysics at TRIUMF-ISAC
Authors: Hutcheon, D. A.; Bishop, S.; Buchmann, L.; Chatterjee, M. L.;
   Chen, A. A.; D'Auria, J. M.; Engel, S.; Gigliotti, D.; Greifef, U.;
   Hunter, D.; Hussein, A.; Jewett, C.; Khan, N.; Lamey, A.; Liu, W.;
   Olin, A.; Ottewell, D.; Rogers, J. G.; Roy, G.; Sprenger, H.; Wrede, C.
2003NuPhA.718..515H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Statistical Study of Limb Flares Observed by RHESSI: Imaging
Authors: Liu, W.; Jiang, Y. W.; Petrosian, V.; Metcalf, T. R.
2003SPD....34.1802L    Altcode: 2003BAAS...35..839L
  Hard X-ray observations by the Reuven Ramaty High Energy Solar
  Spectroscopic Imager (RHESSI) provide unprecedented opportunities
  to understand the underlying physics driving solar flares. We have
  embarked on an investigation of a sample of \it limb flares observed by
  RHESSI. RHESSI flare images, combined with TRACE EUV observations and
  SoHO/MDI magnetograms, are used to infer flaring loop structures and
  to distinguish between footpoint, loop top and other possible types of
  sources. We will present an analysis of the lightcurves and images for
  these features and will show statistics on the occurrence of loop top
  and footpoint sources. These will be compared with previous studies
  utilizing YOHKOH/HXT observations, and the implications for particle
  acceleration processes and other theoretical aspects of flares will
  be discussed. <P />The work at Stanford is supported by NASA grants
  NAG5-12111, NAG5 11918-1, and SUB2001-402-01 through the University
  of Alabama in Huntsville (PI: J. Miller). T. Metcalf would like to
  acknowledge support from grant NAS-98033-05/03.

---------------------------------------------------------
Title: Measurements with DRAGON on resonances in the
    <SUP>21</SUP>Na(p, γ)<SUP>22</SUP>Mg reaction with a radioactive
    ion beam
Authors: Engel, S.; Bishop, S.; Buchmann, L.; Chatterjee, M. L.; Chen,
   A.; D'Auria, J. M.; Gigliotti, D.; Greife, U.; Hunter, D.; Hussein,
   A.; Lewis, R.; Liu, W.; Olin, A.; Ottewell, D.; Parker, P.; Rogers,
   J.; Strieder, F.; Wrede, C.
2003NuPhA.719..107E    Altcode:
  In the modelling of nucleosynthesis in nova explosions,
  temperature and density are important parameters to describe the
  hydrodynamics. Those parameters are not easy to observe, but specific
  gamma-ray emitters produced in the explosion provide constrains on
  the models, such as <SUP>22</SUP>Na, produced via <SUP>21</SUP>Na(p,
  γ)<SUP>22</SUP>Mg(β<SUP>+</SUP>)<SUP>22</SUP>Na. The new DRAGON
  recoil separator facility, designed and built to measure directly
  the rates of radiative proton and alpha capture reactions, important
  for nuclear astrophysics, is now operational. Experiments have been
  conducted on the <SUP>21</SUP>Na(p, γ)<SUP>22</SUP>Mg reaction using
  a radioactive <SUP>21</SUP>Na beam incident onto a windowless hydrogen
  gas target. Yield measurements have been performed detecting the prompt
  gamma and the reaction recoils at E<SUB>cm</SUB> ~ 821 keV and 204 keV.

---------------------------------------------------------
Title: Nuclear astrophysics studiesat dragon: The
    <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg reaction and oxygen-neon novae
Authors: Bishop, S.; Azuma, R.; Buchmann, L.; Chen, A. A.; Chatterjee,
   M. L.; D'Auria, J. M.; Engel, S.; Gigliotti, D.; Greife, U.; Hunter,
   D.; Hussein, A.; Hutcheon, D.; Jewett, C.; King, J.; Kubono, S.;
   Lamey, M.; Lewis, R.; Liu, W.; Michimasa, S.; Olin, A.; Ottewell,
   D.; Parker, P. D.; Rogers, J.; Wrede, C.
2003NuPhA.718..263B    Altcode:
  The rate of the <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg reaction is
  expected to play a major role in the nucleosynthesis of <SUP>22</SUP>Na
  in Oxygen-Neon novae, leading to the emission of a characteristic 1.28
  MeV gamma-line. This paper reports on preliminary results of the first
  direct measurements of this reaction and its astrophysical implications.

---------------------------------------------------------
Title: Results of <SUP>21</SUP>Na+p experiments at ISAC
Authors: Azuma, R. E.; Bishop, S.; Buchmann, L.; Chatterjee, M. L.;
   Chen, A. A.; D'Auria, J. M.; Davinson, T.; Engel, S.; Fulton, B. R.;
   Gigliotti, D.; Greife, U.; Groombridge, D.; Hunter, D.; Hussein, A.;
   Hutcheon, D.; Jewett, C.; King, J. D.; Khan, N.; Kubono, S.; Laird,
   A. M.; Lamey, M.; Lewis, R.; Ling, L.; Liu, W.; Michimasa, S.; Murphy,
   A. S.; Olin, A.; Ottewell, D.; Parker, P.; Pearson, J.; Roberts, I.;
   Robinson, A.; Rogers, J. G.; Roy, G.; Ruiz, C.; Sarazin, F.; Shotter,
   A. C.; Sprenger, H.; Strieder, F.; Walden, P.; Woods, P. J.; Wrede, C.
2003NuPhA.718..119A    Altcode:
  Several resonances in <SUP>22</SUP>Mg have been observed with a
  radioactive beam of <SUP>21</SUP>Na impinging on a hydrogen target at
  ISAC. Both elastic scattering as well as radiative capture have been
  investigated. Some results together with the experimental methods used
  will be reported.

---------------------------------------------------------
Title: <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg Reaction and Oxygen-Neon
    Novae
Authors: Bishop, S.; Azuma, R. E.; Buchmann, L.; Chen, A. A.;
   Chatterjee, M. L.; D'Auria, J. M.; Engel, S.; Gigliotti, D.; Greife,
   U.; Hernanz, M.; Hunter, D.; Hussein, A.; Hutcheon, D.; Jewett, C.;
   José, J.; King, J.; Kubono, S.; Laird, A. M.; Lamey, M.; Lewis,
   R.; Liu, W.; Michimasa, S.; Olin, A.; Ottewell, D.; Parker, P. D.;
   Rogers, J. G.; Strieder, F.; Wrede, C.
2003PhRvL..90p2501B    Altcode: 2003astro.ph..3285B
  The <PRE><SUP>21</SUP></PRE>Na(p,γ)<PRE><SUP>22</SUP></PRE>Mg
  reaction is expected to play an important role in the nucleosynthesis
  of <PRE><SUP>22</SUP></PRE>Na in oxygen-neon novae. The decay of
  <PRE><SUP>22</SUP></PRE>Na leads to the emission of a characteristic
  1.275MeV gamma-ray line. This report provides the first direct
  measurement of the rate of this reaction using a radioactive
  <PRE><SUP>21</SUP></PRE>Na beam, and discusses its astrophysical
  implications. The energy of the important state was measured
  to be E<SUB>c.m.</SUB>=205.7±0.5 keV with a resonance strength
  ωγ=1.03±0.16<SUB>stat</SUB>±0.14<SUB>sys</SUB> meV.

---------------------------------------------------------
Title: International Living With a Star (ILWS), a new collaborative
    space program in Solar, Heliospheric and Solar-Terrestrial Physics
Authors: Opgenoorth, H. J.; Guhathakurta, M.; Liu, W.; Kosugi, T.;
   Zelenyi, L.
2003EAEJA.....5360O    Altcode:
  International cooperation has long been a vital element in the
  scientific investigation of solar variability and its impact on Earth
  and its space environment. Recently a new international cooeperative
  program in solar terrestrial physics has been established by the
  major space agencies of the world, called the International Living
  With a Star (ILWS) program. ILWS is a follow on to the highly
  successful International Solar Terrestrial Physics (ISTP) program
  which involved international parterners. ISTP, with its steady flow
  of discoveries and new knowledge in solar Terrestrial physics, has
  laid the foundation for the coordinated study of the Sun-Earth sytem
  as a connected stellar-planetary system, system which is humanity's
  home. The first step in establishing ILWS was taken in the fall of
  2000 when funding was approved for the NASA's Living With a Star
  (LWS) program whose goal is to develop the scientific understanding
  necessary to effectively address those aspects of the connected
  Sun-Earth system that directly affect life and society. The scientific
  goals of ILWS are defined in a broader sense, aiming to include future
  solar, heliospheric and solar terrestrial missions of both applied
  and fundamental scientific focus. The ultimate goal of ILWS wil be
  to increase our understanding of how solar variability affects the
  terrestrial and other planetary environments both in the short and
  long term, and in particular how man and society may be affected by
  solar variability and its consequences. The mission charter of ILWS is
  'to stimulate, strengthen and coordinate space research in order to
  understand the governing processes of the connected Sun-Earth System as
  an integrated entity'. More detailed ILWS Objectives are to stimulate
  and facilitate: - The study of the Sun Earth connected system and the
  effects which influence life and society - Collaboration among all
  potential partners in solar-terrestrial space missions - Synergistic
  coordination of international research in solar-terrestrial studies,
  including all relevant data sources as well as theory and modeling. The
  future ILWS program will be supervised by an international steering
  committee, involving representatives from the 4 main space agencies
  NASA, ESA, ISAS, RSA, and, emphasising the importance of ground-based
  instrumentation in the systematic approach of the ILWS programme,
  also from the Canadian Space Agency (CSA). More specific work will be
  carried out through an IWLS Working Group, membership to which is open
  to space organizations committed to contribute to ILWS over the next
  decade. Adequate contributions to ILWS can include any of the following:
  - Space Flight Missions - Mission payloads or subsystems - Mission
  launch or tracking services - Additional data sources supporting S/C
  (sounding rockets, balloon, or ground-based) - Data dissemination,
  storage, distribution and value adding systems In addition topical
  ILWS Task Groups will be established as necessary to support specific
  ILWS-WG projects/studies. This poster will biefly summarize the origins,
  objectives, and provisional organizational structure for ILWS and
  how this program can benifit from and contribute to international
  collaborative efforts towards International Heliospheric Year (IHY).

---------------------------------------------------------
Title: The DRAGON facility for nuclear astrophysics at TRIUMF-ISAC:
    design, construction and operation
Authors: Hutcheon, D. A.; Bishop, S.; Buchmann, L.; Chatterjee, M. L.;
   Chen, A. A.; D'Auria, J. M.; Engel, S.; Gigliotti, D.; Greife, U.;
   Hunter, D.; Hussein, A.; Jewett, C. C.; Khan, N.; Lamey, M.; Laird,
   A. M.; Liu, W.; Olin, A.; Ottewell, D.; Rogers, J. G.; Roy, G.;
   Sprenger, H.; Wrede, C.
2003NIMPA.498..190H    Altcode:
  A facility for measuring cross-sections (resonance strengths)
  for reactions of astrophysical importance involving short-lived,
  radioactive reactants has been designed, built and installed at the
  new TRIUMF-ISAC Radioactive Beams Laboratory in Canada. Named DRAGON
  (Detector of Recoils And Gamma-rays of Nuclear reactions), it has been
  successfully commissioned with stable and radioactive heavy ion beams
  from ISAC. This report presents the main components of the facility,
  namely, the windowless gas target, the surrounding /γ detector
  array, the subsequent electromagnetic recoil mass separator, the
  focal plane detectors for recoils, the detection system for elastics,
  and the modular electronics and computer software used for the data
  acquisition. Examples of the operation of the facility for both
  stable beam reactions and the first radioactive beam reaction study,
  <SUP>21</SUP>Na(p,γ)<SUP>22</SUP>Mg are also presented, along with
  future plans for the program.

---------------------------------------------------------
Title: Satellite observations of modulation of surface winds by
    typhoon-induced upper ocean cooling
Authors: Lin, I. -I.; Liu, W. Timothy; Wu, Chun-Chieh; Chiang,
   J. C. H.; Sui, Chung-Hsiung
2003GeoRL..30.1131L    Altcode: 2003GeoRL..30c..31L
  Two remote sensing data sets, the Tropical Rainfall Measurement Mission
  Sea Surface Temperature (SST) and the NASA QuikSCAT ocean surface wind
  vectors, are analysed to study ocean-atmosphere interactions in cold
  SST regions formed in the trail of two typhoon events. Anomalously
  cold SST patches up to 6°C below the surrounding warm tropical ocean
  SST are found along the trail of typhoon tracks as cold, deep waters
  are entrained up to the mixed layer due to typhoon forcing. In both
  typhoon events, significant and systematic weakening of surface wind
  speed is found over cold SST patches relative to surface wind speed in
  surrounding regions. The wind speed anomalies disappear as the patches
  recover to the level of the surrounding SST. The results are consistent
  with the mechanism proposed by Wallace et al. that surface winds are
  modulated by SST via stability. As wind within the well-mixed boundary
  layer moves over the cold patch, boundary layer stability increases,
  vertical mixing is suppressed, and the vertical wind shear increases;
  reduction in surface wind speed is caused. In particular, our result
  shows that this mechanism can act on relatively small spatial (~100 km)
  and short (~1 day) time scales.

---------------------------------------------------------
Title: Correction to “CO<SUB>2</SUB> exchange coefficients from
remotely sensed wind speed measurements: SSM/I versus QuikSCAT in
    2000” by Mary-Elena Carr, Wenqing Tang, and W. Timothy Liu
Authors: Carr, M. -E.; Tang, W.; Liu, W. T.
2003GeoRL..30.1038C    Altcode: 2003GeoRL..30b..10C
  No abstract at ADS

---------------------------------------------------------
Title: Some projects related to Stanford Solar Physics Group
Authors: Liu, Wei; Liu, Yang; Zhao, Jun-Wei
2003PYunO..93...71L    Altcode:
  Stanford Solar Physics Group has endeavored to pursue the goal of
  understanding the origins of solar variability and its effects on the
  terrestrial environment. To accomplish this objective, we are actively
  involved in a variety of ongoing and upcoming projects. An overview
  of these projects and some of our related activities are presented.

---------------------------------------------------------
Title: Preliminary Results of Video Observations from Sino-Dutch
    2001 Leonids Expedition
Authors: Guan, M.; de Lignie, M.; Zhu, J.; Dijkstra, S.; Gao, J.;
   Haas, R.; Ter Kuile, C.; Liu, W.; Meng, H.; Miskotte, K.; Nijland,
   J.; Qi, R.; Tukkers, A.; Vandeputte, M.; Xia, D.; Yang, B.
2003pimo.conf...12G    Altcode:
  The preliminary 2001 Leonids results of multi-station video observations
  are presented. The observations were obtained at Miyun, Panshan,
  Xinglong and Huairou in China during 2001 November 18-20. Thirty
  Leonid meteors are reduced. The coordinates of the radiant are
  alpha=154.49+-1.80 deg and delta=21.32+-0.74 deg (J2000.0) for mean
  solar longitude of 236.486 deg based on these 30 Leonids.

---------------------------------------------------------
Title: Direct Observations of Atmospheric Boundary Layer Response
    to SST Variations Associated with Tropical Instability Waves over
    the Eastern Equatorial Pacific(.
Authors: Hashizume, Hiroshi; Xie, Shang-Ping; Fujiwara, Masatomo;
   Shiotani, Masato; Watanabe, Tomowo; Tanimoto, Youichi; Liu, W. Timothy;
   Takeuchi, Kensuke
2002JCli...15.3379H    Altcode:
  Tropical instability waves (TIWs), with a typical wavelength of 1000
  km and period of 30 days, cause the equatorial front to meander and
  result in SST variations on the order of 1°-2°C. Vertical soundings
  of temperature, humidity, and wind velocity were obtained on board a
  Japanese research vessel, which sailed through three fully developed SST
  waves from 140° to 110°W along 2°N during 21-28 September 1999. A
  strong temperature inversion is observed throughout the cruise along
  2°N, capping the planetary boundary layer (PBL) that is 1-1.5 km
  deep. Temperature response to TIW-induced SST changes penetrates the
  whole depth of the PBL. In response to an SST increase, air temperature
  rises in the lowest kilometer and shows a strong cooling at the mean
  inversion height. As a result, this temperature dipole is associated
  with little TIW signal in the observed sea level pressure (SLP).The
  cruise mean vertical profiles show a speed maximum at 400-500 m for
  both zonal and meridional velocities. SST-based composite profiles of
  zonal wind velocity show weakened (intensified) vertical shear within
  the PBL that is consistent with enhanced (reduced) vertical mixing,
  causing surface wind to accelerate (decelerate) over warm (cold)
  SSTs. Taken together, the temperature and wind soundings indicate the
  dominance of the vertical mixing over the SLP-driving mechanism. Based
  on the authors' measurements, a physical interpretation of the widely
  used PBL model proposed by Lindzen and Nigam is presented.

---------------------------------------------------------
Title: Direct observations of atmospheric boundary layer response
    to SST variations associated with tropical instability waves over
    the eastern equatorial Pacific
Authors: Hashizume, H.; Xie, S.; Fujiwara, M.; Shiotani, M.; Watanabe,
   T.; Tanimoto, Y.; Liu, W.; Takeuchi, K.
2002AGUFM.A21D..08H    Altcode:
  Tropical instability waves (TIWs), with a typical wavelength of 1000
  km and period of 30 days, cause the equatorial front to meander and
  result in sea surface temperature (SST) variations on the order of
  1-2C. Vertical soundings of temperature, humidity and wind velocity
  were obtained on board of a Japanese research vessel, which sailed
  through three fully developed SST waves from 140W to 110W along 2N
  during September 21-28, 1999. A strong temperature inversion is observed
  throughout the cruise along 2N, capping the planetary boundary layer
  (PBL) that is 1-1.5 km deep. Temperature response to TIW-induced SST
  changes penetrates the whole depth of the PBL. In response to a SST
  increase, air temperature rises in the lowest km and shows a strong
  cooling at the mean inversion height. As a result, this temperature
  dipole is associated with little TIW signal in the observed sea level
  pressure (SLP). The cruise-mean vertical profiles show a speed maximum
  at 400-500 m for both zonal and meridional velocities. SST-based
  composite profiles of zonal wind velocity show weakened (intensified)
  vertical shear within the PBL that is consistent with enhanced (reduced)
  vertical mixing, causing surface wind to accelerate (decelerate) over
  warm (cold) SSTs. Taken together, our temperature and wind soundings
  indicate the dominance of the vertical mixing over the SLP-driving
  mechanism. Based on our measurements, a physical interpretation
  of the widely used PBL model proposed by Lindzen and Nigam (1987,
  J. Atmos. Sci.,p.2418-2436) is presented.

---------------------------------------------------------
Title: HST/NICMOS Observations of NGC 2024: The Emergent Mass
    Distribution and Stellar Multiplicity
Authors: Liu, W. M.; Meyer, M. R.; Cotera, A. S.; Young, E. T.
2002AAS...201.9309L    Altcode: 2002BAAS...34.1260L
  We present an analysis of NICMOS observations of the embedded cluster
  NGC 2024. An analysis of the cluster color-magnitude diagram (CMD)
  using models of D'Antona &amp; Mazzitelli (1998) and Baraffe et
  al. (1998) indicates that the ratio of intermediate mass (1.0 to
  10.0 M<SUB>sun</SUB>) to low mass (0.1 to 1.0 M<SUB>sun</SUB>) stars
  is consistent with a field star IMF. We also present results on the
  multiplicity of stars in the region. Three companions (in a sample of
  94 potential primaries) were found, with an angular separations between
  0".4 and 1".0, translating to a projected linear separation of 184 AU to
  460 AU for an estimated distance of 470 pc. The completeness of binary
  detections is assessed using recovery fractions calculated by a series
  of tests using artificially generated companions to potential primaries
  in the data frames. We find that the binary fraction is similar to
  that of Duquennoy &amp; Mayor (1991) for solar-type stars over the
  range of separations and companion masses appropriate for our survey.

---------------------------------------------------------
Title: Bathymetric effect on the winter sea surface temperature and
    climate of the Yellow and East China Seas
Authors: Xie, Shang-Ping; Hafner, Jan; Tanimoto, Youichi; Liu,
   W. Timothy; Tokinaga, Hiroki; Xu, Haiming
2002GeoRL..29.2228X    Altcode: 2002GeoRL..29x..81X
  Whether and how the atmosphere reacts to changes in extratropical
  sea surface temperature (SST) is under intense debate and this lack
  of understanding has been a major obstacle in the study of non-El
  Nino climate variability. Using new satellite measurements, we detect
  clear ocean-to-atmospheric feedback in the Yellow and East China (YEC)
  Seas that is triggered by the submerged ocean bottom topography. Under
  intense surface cooling in winter, water properties are well mixed
  up to 100 m deep. Ocean depth thus has a strong influence on SST of
  the continental shelf, leading to a remarkable collocation of warm
  tongues and deep channels. High winds and increased cloudiness are
  found over these warm tongues; one such band of ocean-atmospheric
  co-variation meanders through the basin, following a deep channel for
  an amazing distance of 1000 km. In addition to these climatic effects,
  the Kuroshio Front-where the warm current meets the much colder shelf
  water-strengthens the growth of storms.

---------------------------------------------------------
Title: Pacific warm pool excitation, earth rotation and El Niño
    southern oscillations
Authors: Yan, Xiao-Hai; Zhou, Yonghong; Pan, Jiayi; Zheng, Dawei; Fang,
   Mingqiang; Liao, Xinhao; He, Ming-Xia; Liu, W. Timothy; Ding, Xiaoli
2002GeoRL..29.2031Y    Altcode: 2002GeoRL..29u..27Y
  The interannual changes in the Earth's rotation rate, and hence in
  the length of day (LOD), are thought to be caused by the variation
  of the atmospheric angular momentum (AAM). However, there is
  still a considerable portion of the LOD variations that remain
  unexplained. Through analyzing the non-atmospheric LOD excitation
  contributed by the Western Pacific Warm Pool (WPWP) during the period
  of 1970-2000, the positive effects of the WPWP on the interannual
  LOD variation are found, although the scale of the warm pool is much
  smaller than that of the solid Earth. These effects are specifically
  intensified by the El Niño events, since more components of the LOD-AAM
  were accounted for by the warm pool excitation in the strong El Niño
  years. Changes in the Earth's rotation rate has attracted significant
  attention, not only because it is an important geodetic issue but also
  because it has significant value as a global measure of variations
  within the hydrosphere, atmosphere, cryosphere and solid Earth, and
  hence the global changes.

---------------------------------------------------------
Title: Double intertropical convergence zones-a new look using
    scatterometer
Authors: Liu, W. Timothy; Xie, X.
2002GeoRL..29.2072L    Altcode: 2002GeoRL..29v..29L
  The high-resolution wind vectors observed by the space-based
  scatterometer QuikSCAT, from 1999 to 2002, show that the double
  intertropical convergence zones (ITCZ) exist in the Atlantic and the
  eastern Pacific oceans for most of the annual cycle, and are far more
  extensive than previously recognized. For most of the time, the southern
  ITCZ is weaker than the northern one. The stronger ITCZ occurs when the
  northerly trade winds meet the southerly trade winds over warm water,
  resulting in deep convection. The weaker ITCZ over cooler water is
  caused by the deceleration of the surface winds as they approach the
  cold upwelling water near the equator. Decreases in vertical mixing
  and increases in vertical wind shear in the atmospheric boundary layer
  are suggested to be the causes of the deceleration of the trade winds
  as they move from warmer to colder water.

---------------------------------------------------------
Title: Solar mean magnetic field variability: A wavelet approach
    to Wilcox Solar Observatory and SOHO/Michelson Doppler Imager
    observations
Authors: Boberg, Fredrik; Lundstedt, Henrik; Hoeksema, J. Todd;
   Scherrer, Philip H.; Liu, Wei
2002JGRA..107.1318B    Altcode:
  Solar mean magnetic field (SMMF) measurements from the Wilcox
  Solar Observatory and with the SOHO/MDI instrument are described and
  analyzed. Even though two completely different methods of observation
  are used, the two data sets obtained show a strong similarity. Using
  continuous wavelet transforms, SMMF variability is found at a number
  of temporal scales. Detected SMMF signals with a 1-2 year period are
  considered to be linked to variations in the internal rotation of the
  Sun. Intermediate SMMF oscillations with a period of 80-200 days are
  probably connected to the evolution of large active regions. We also
  find evidence for 90 min variations with coronal mass ejections as a
  suggested origin.

---------------------------------------------------------
Title: Present and future studies with DRAGON at ISAC
Authors: Chen, A. A.; Bishop, S.; Buchmann, L.; Chatterjee, M. L.;
   D'Auria, J. M.; Engel, S.; Galovich, C. S.; Gigliotti, D.; Greife,
   U.; Hunter, D.; Hussein, A.; Hutcheon, D. A.; Jewett, C.; King, J.;
   Kubono, S.; Laird, A.; Lamey, M.; Lewis, R.; Liu, W.; Michimasa,
   S.; Olin, A.; Ottewell, D.; Parker, P. D.; Rogers, J.; Strieder, F.;
   Wiescher, M.; Wrede, C.
2002APS..DNP.DE011C    Altcode:
  The isotope ^22Na (T_1/2 2.6 years) in nova ejecta may serve as an
  important target for gamma-ray astronomy with orbiting telescopes. The
  ^21Na(p,γ)^22Mg reaction, in turn, is a key link in the production
  of ^22Na in nova nucleosynthesis. We present recent results from a
  measurement of the ^21Na(p,γ)^22Mg reaction rate, using radioactive
  ^21Na beams from ISAC and the DRAGON recoil separator. We also discuss
  future plans to measure with DRAGON other reactions of importance
  to stellar explosions, such as ^13N(p,γ)^14O, ^19Ne(p,γ)^20Na,
  and ^25Al(p,γ)^26Si, among others.

---------------------------------------------------------
Title: QuikSCAT reveals the surface circulation of the Catalina Eddy
Authors: Hu, Hua; Liu, W. Timothy
2002GeoRL..29.1821H    Altcode: 2002GeoRL..29q...2H
  The Catalina Eddy, a small, recurring cyclonic vortex in the ocean off
  Los Angeles, is of keen interest to local weather forecasters because of
  the moderating oceanic effect it brings to the city. Its small size and
  shallow vertical extent have made it difficult to monitor and predict
  using conventional data. The microwave scatterometer on the QuikSCAT
  spacecraft has generated high-resolution surface wind vectors that
  provide the first visualization of the complete cyclonic flow of the
  eddy. Moreover, the superior performance of the QuikSCAT scatterometer
  demonstrates the relative inaccuracy and inconsistency of predictions
  of the eddy based upon numerical weather prediction models.

---------------------------------------------------------
Title: Observation of western boundary current atmospheric convergence
    zones using scatterometer winds
Authors: Pan, Jiayi; Yan, Xiao-Hai; Zheng, Quanan; Liu, W. Timothy
2002GeoRL..29.1832P    Altcode: 2002GeoRL..29q..13P
  A merged scatterometer wind data set from ERS-1/2, NSCAT, and QuikSCAT
  missions was used to observe the atmospheric convergence zones
  (ACZs) caused by the western boundary currents, the Gulf Stream and
  Kuroshio. The long-term means of the atmospheric convergence show
  the ACZs' spatial features, which are related to the precipitation
  patterns in these regions. Seasonal images of the ACZs were produced
  to show annual cycles of the ACZs, indicating that the intensities
  of the ACZs over these two regions strengthen in winter and weaken
  in summer. Furthermore, we calculated the total convergence over the
  Gulf Stream and Kuroshio ACZs, which is defined as the integral of the
  convergence over the ACZs. The interannual variability of the total
  convergence was extracted by using a multi-stage filter, revealing
  that in response to strong El Niño events in 1991-92 and 1997-98,
  the total convergence reached maxima.

---------------------------------------------------------
Title: Determination of geometrical and kinematical properties of
    halo coronal mass ejections using the cone model
Authors: Zhao, X. P.; Plunkett, S. P.; Liu, W.
2002JGRA..107.1223Z    Altcode:
  Many broadside coronal mass ejections (CMEs) propagate almost radially
  beyond the first couple of solar radii, and their angular widths remain
  nearly constant while propagating through the corona. Assuming that
  these characteristics hold true for halo CMEs that originate far from
  solar limbs, some useful geometric and kinematic properties of halo
  CMEs may be reproduced using a simple geometrical model of a CME as
  a cone. The cone model uses three free parameters, characterizing the
  angular width and the central position of the halo CME. These geometric
  properties can be determined by matching the observed halos at a series
  of times with the modeled halos for a series of radial distances. The
  kinematic properties, the radial velocity and acceleration, of the
  halo CME can also be determined on the basis of the series of times
  and radial distances. These properties are important for predicting
  the geoeffectiveness of a halo CME and cannot be observed directly
  with currently available instrumentation. As a test, the geometric and
  kinematic properties of the 12 May 1997 halo CME have been inferred
  using the cone model. This shows that the cone model does provide a
  new way of testing our understanding of halo CMEs, though there are
  limitations for some halo CMEs.

---------------------------------------------------------
Title: CO<SUB>2</SUB> exchange coefficients from remotely sensed
wind speed measurements: SSM/I versus QuikSCAT in 2000
Authors: Carr, Mary-Elena; Tang, Wenqing; Liu, W. Timothy
2002GeoRL..29.1740C    Altcode: 2002GeoRL..29o..30C
  We compare here the air-sea exchange coefficient for CO<SUB>2</SUB>
  estimated with monthly mean wind speed measured by the Special Sensing
  Microwave Imager (SSM/I), K<SUB>S</SUB>, and by the scatterometer
  QuikSCAT, K<SUB>Q</SUB>, for the year 2000. K<SUB>S</SUB> and
  K<SUB>Q</SUB> present the same patterns, although are larger than in
  ~65% of the world ocean. Zonal mean K<SUB>S</SUB> are consistently
  larger, except ~50°S and north of 10°S in the Indian Ocean. Global
  oceanic uptake, F<SUB>Q</SUB>, estimated using K<SUB>Q</SUB> and
  climatological Δp<SUB>CO2</SUB> ranges from 0.43 (July) to 2.6 Gt
  C y<SUP>-1</SUP> (December). The global sink estimated from SSM/I is
  ~10% larger than F<SUB>Q</SUB> for most of the year. This comparison
  supports the use of SSM/I to quantify interannual variability of the
  global exchange coefficient of CO<SUB>2</SUB>.

---------------------------------------------------------
Title: Effects of Topology on CME Kinematic Properties
Authors: Liu, W.; Zhao, X. P.; Wu, S. T.; Scherrer, P. H.
2002AAS...200.3602L    Altcode: 2002BAAS...34Q.693L
  Coronal Mass Ejections (CMEs) exhibit two types of kinematic property:
  fast CMEs with high initial speeds and slow CMEs with low initial speeds
  but gradual accelerations. Efforts have been made for years to probe
  the underlying physics responsible for this dual character. Within
  these efforts, magnetic topology has gained much attention. Low and
  Zhang (ApJ, 564, L53, 2002) proposed that fast or slow CMEs result from
  initial states with magnetic configurations characterized by the normal
  or inverse quiescent prominences, respectively. To test their theory
  and further explore the effects of topology on kinematic properties
  of CMEs, we employed a 2-D, axisymmetric, resistive MHD model to
  simulate the evolution of CMEs in the normal and inverse prominence
  environments, respectively. The numerical results show that the CMEs
  originating from a normal prominence environment do have higher initial
  speeds than those from an inverse one. In addition, our simulations
  demonstrate the distinct roles played by magnetic reconnection in
  these two topologically different magnetic environments to produce
  the two different CME height-time profiles as suggested by Low and
  Zhang. The implication of the results and discussion on future work
  are described. SOHO is a project of international cooperation between
  ESA and NASA.

---------------------------------------------------------
Title: Photometric monitoring of 12 BL Lacertae objects
Authors: Xie, G. Z.; Zhou, S. B.; Dai, B. Z.; Liang, E. W.; Li, K. H.;
   Bai, J. M.; Xing, S. Y.; Liu, W. W.
2002MNRAS.329..689X    Altcode:
  We present the results of our monitoring the flux variability of 12
  BL Lac objects, which have variabilities on time-scales ranging from
  hours to months. Individual sources are discussed in detail. Three of
  them, OY091, H0548-322 and 0048-097, show significant rapid variation
  (hours). Two of them, 3C 66A and Mrk 501, exhibit significant
  variability on time-scales of months. We find that 3C 66A has a
  variability period of 63+/-5d, supporting the 65-d period obtained
  by Lainela et al. The periodicity seems to be weak according to the
  Jurkevich Vm2 test. We also find a correlation between B-V colour index
  and B magnitude for Mrk 421. We discuss possible physical mechanisms
  on the basis of these observational phenomena.

---------------------------------------------------------
Title: A Cone Model for Coronal Mass Ejections
Authors: Liu, W.; Plunkett, S. P.; Zhao, X. P.
2002stma.conf..267L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The effect of the host galaxy on the short timescale
    variability of γ-ray loud blazars
Authors: Dai, Ben-Zhong; Xie, Guang-Zhong; Jiang, Ze-Jun; Li, Kai-Hua;
   Zhou, Shu-Bai; Liu, Wei-Wei
2002PYunO..90....1D    Altcode:
  We present the optical (V and R) photometry for three GeV and/or TeV
  γ-ray blazars, which were observed from 2000 through 2001, with the 1-m
  telescope at Yunnan Observatory. Through the observational period, the
  GeV γ-ray-loud source, PKS 1510-089, was very active and, it showed a
  significant variability of 2.0 mag within 41 min in the R band. This is
  the most violently rapid variability in our optical monitoring program
  for blazars since 1982. For this source, some physical parameters,
  namely the emission size, Doppler factor δ, the efficiency (η)
  for conversion of accreted matter into energy and luminosity are
  calculated. A η = 59.6 was obtained, strongly implying that the
  relativistic beaming is responsible for the rapid variability of the
  γ-ray loud source. The influence of variable seeing conditions on
  the observations was carefully investigated. There is weak correlation
  between the observed variability and the local seeing conditions for
  the object 1ES 2344+514. The results show that the seeing fluctuations
  would influence the spurious variation in microvariability when the
  variability parameter C&lt;5.

---------------------------------------------------------
Title: Intense phytoplankton bloom induced by typhoon in coastal water
Authors: Lin, I.; Liu, W.
2002cosp...34E1447L    Altcode: 2002cosp.meetE1447L
  Typhoon landfall is devastating to the economy and may cause
  human lives. Yet typhoon may also enhance other forms of life -
  the primary productivity of coastal water. Large human population
  lives near the coast and understands the threat of strong wind and
  heavy rain of marine storms. Coastal water and marginal seas are the
  most productive part of global oceans, but few people realize that
  typhoons may pump nutrients to the surface water and benefit fishery
  after their passages. . The typhoon forcing and oceanic responses over
  coastal water have strong temporal and spatial variability that cannot
  be sufficiently resolved by operational numerical weather prediction
  models and ground measurements. Two spaceborne microwave sensors,
  QuikSCAT and the Tropical Rain Measuring Mission Microwave Imager
  (TMI) allow us to measure ocean surface wind vectors and sea surface
  temperature (SST) under the cloud cover of typhoons day and night,
  and the Sea Viewing Wide-Field-of-View Sensor (SeaWifs) shows us
  the ocean color, and the biological activities it denotes, after the
  typhoon passage. An interdisciplinary study of physical forcing and
  biological response based on synergistic applications of the three space
  missions will be presented. Three typhoons were tracked, through the
  QuikSCAT surface wind field and Ekman pumping, over the coastal water
  and marginal seas of East Asia in the summer of 2000. Super-typhoon
  Bilis left a cold wake in the deep water east of Taiwan as observed by
  TMI, but with no increase in biological activities near the surface as
  observed by SeaWifs. A weaker typhoon Prapirron followed Bilis a week
  later producing a cold wake at the north east tip of Taiwan. SeaWifs
  observed increase in biological activities in this wake after Prapirron
  passage. Climatological in situ measurements show that in the ocean
  east of Taiwan, the nutrients lie deep. They do not rise to the surface
  even with the passage of super-typhoon. However, in the coastal shallow
  water, nutrients are near the surface and they rise to the surface
  even with the passage of a weak typhoon. Typhoon Kai-Tak passed slowly
  through the northern part of South China Sea, which is a semi-enclosed
  marginal sea. TMI and SeaWifs show a 10 C cooling of SST and 100 time
  increases (from 0.1 to 10 mg/m3 ) chlorophyll-a (indicating biological
  activities), confirming that the biological response to Ekman pumping
  by typhoons can be much stronger than generally believed in coastal
  water and marginal seas where nutrients reside in shallow water.

---------------------------------------------------------
Title: The Canadian Space Environment Program and International
    Living With a Star
Authors: Liu, W.
2002cosp...34E3252L    Altcode: 2002cosp.meetE3252L
  The Canadian space environment program involves a number of
  universities, government departments and agencies. The Canadian
  Space Agency acts as the coordinator of many activities in Canada
  and represents Canada in the ILWS working group. The Canadian space
  environment strategy is based on two elements: 1) ensure a strong,
  diverse, and self-sustainable national program capitalizing on Canada's
  existing resources and advantages, and 2) using the national program as
  the core, create and pursue new international collaborations to maximize
  the impact of Canadian scientific activities. In this presentation,
  I will outline the core Canadian national space environment program,
  consisting of Geospace Monitoring and Near- Earth Space Environment
  Study Using Small Satellites. The core Canadian National Program will be
  closely coordinated with the overall ILWS program architecture through
  scientific, as well inter-agency interactions. I will also describe
  the current state of planning and consultation in Canada concerning
  an enhanced ILWS initiative, with a preliminary discussion of some
  mission scenarios and options.

---------------------------------------------------------
Title: Rapid Optical Variability of Gamma-Ray-loud Blazars
Authors: Dai, B. Z.; Xie, G. Z.; Li, K. H.; Zhou, S. B.; Liu, W. W.;
   Jiang, Z. J.
2001AJ....122.2901D    Altcode:
  We present the optical (B, V, and R) photometry for nine GeV and/or TeV
  γ-ray blazars, which were observed from 2000 through 2001 with the 1 m
  telescope at Yunnan Astronomical Observatory. The GeV γ-ray-loud source
  PKS 1510-089 was very active during our observation period, showing an
  apparent variation of 2.0 mag within 41 minutes in the R band. This is
  the most violently rapid variability in our optical monitoring program
  since 1982. Some physics parameters are calculated for this source,
  namely, the emission size, Doppler factor δ, the efficiency (η) for
  conversion of accreted matter into energy, and luminosity. An η=62.2
  was obtained, strongly implying that relativistic beaming is responsible
  for the rapid variability of the γ-ray-loud source. The influence of
  variable seeing conditions on the observations was investigated. There
  is a weak correlation between the observed variability and the local
  seeing conditions for the object 1ES 2344+51.4.

---------------------------------------------------------
Title: Vector empirical orthogonal function modes of the ocean
    surface wind variability derived from satellite scatterometer data
Authors: Pan, Jiayi; Yan, Xiao-Hai; Zheng, Quanan; Liu, W. Timothy
2001GeoRL..28.3951P    Altcode:
  Ocean surface winds derived from NSCAT, QuikSCAT and ERS-1/2
  scatterometer observations during a period from January 1992 to April
  2000 were analyzed using the vector empirical orthogonal function (VEOF)
  method. With the boreal winter and summer oscillation, the first VEOF
  is dominated by the Indian and East Asian monsoons and also shows an
  annual cycle of the trade winds. The second VEOF represents the boreal
  autumn and spring oscillation, and reveals a transition state between
  winter and summer. The third VEOF indicates the wind variability
  associated with El Niño Southern Oscillation (ENSO) events, because
  the temporal mode has a high correlation coefficient of 0.8 with the
  Southern Oscillation Index (SOI). Furthermore, the third mode reveals
  the teleconnection of the Indian monsoon and wind variability over
  high latitude oceans, such as the Aleutian Low system, with ENSO events.

---------------------------------------------------------
Title: Oceanic and atmospheric anomalies of tropical instability waves
Authors: Polito, Paulo S.; Ryan, John P.; Liu, W. Timothy; Chavez,
   Francisco P.
2001GeoRL..28.2233P    Altcode:
  Tropical instability waves (TIWs) are detected in remotely-sensed
  sea surface height (SSH), temperature (SST), and wind records of the
  eastern equatorial Pacific. Analyses of TIW anomaly relationships
  reveal strong dynamical influence of TIWs within approximately 5° of
  the equator. The first influence is advective heat flux. The primary
  forcing of TIW SST anomalies is advection of the meridional temperature
  gradient by TIW currents. The second influence is modification of the
  wind stress and Ekman pumping fields by TIW surface ocean currents. By
  affecting surface stress and hence roughness, TIW currents in this
  low-wind region introduce a significant bias in scatterometer vector
  wind measurement. This bias is evident in both NSCAT and QuikSCAT
  winds. The difference between wind measurements from TAO moorings and
  scatterometers is phase-locked with TIW SST oscillations. These results
  have important implications for scatterometry and for understanding
  tropical dynamics, thermodynamics and biogeochemistry.

---------------------------------------------------------
Title: Are the Signals in the Sun's Mean Magnetic Field Associated
    With Coronal Mass Ejections?
Authors: Liu, W.; Liu, Y.; Zhao, X.; Scherrer, P.
2001AGUSM..SH41A06L    Altcode:
  A study on time-frequency variability of the solar mean magnetic field
  (SMMF) using wavelet analysis is presented. The SMMF data of Michelson
  Doppler Imager (MDI) contain an offset most likely introduced by the
  random error of the exposure time of MDI. Without the offset correction,
  the peaks of wavelet power spectra for the full-disk SMMF time series
  coincide with the onset of coronal mass ejections. It has thus been
  suggested that the peak of wavelet power spectra is associated with
  coronal mass ejections [Boberg and Lundstedt 2000]. To localize the
  source of the peak, the full solar disk has been divided into four
  quadrants. It turns out unexpectedly that the time series for each
  quadrant closely resembles that of the full-disk series. In addition,
  all the five series are nearly in phase. On the other hand, the peaks
  of wavelet power spectra that coincide with coronal mass ejections
  disappear for the full-disk SMMF series obtained after the offset
  correction, suggesting that the signal actually occurs in the offset
  series. These results give rise to the question -- what is the cause
  of the signals detected in the offset series by the wavelet technique?

---------------------------------------------------------
Title: QuikSCAT's sea winds facilitates early identification of
    tropical depressions in 1999 hurricane season
Authors: Katsaros, Kristina B.; Forde, Evan B.; Chang, Paul; Liu,
   W. Timothy
2001GeoRL..28.1043K    Altcode:
  Far from land and surface ship observations, most tropical depressions
  are identified by examining images from geostationary satellites for
  the presence of rotation of the convective cloud masses. During the
  1999 hurricane season, surface wind vectors obtained by the SeaWinds
  scatterometer on the QuikSCAT satellite for the tropical Atlantic and
  Caribbean Sea were examined to test the hypothesis that developing
  tropical depressions (TDs) could be observed with this satellite
  sensor, before identification by the traditional means. QuikSCAT
  was able to detect the presence of closed circulation in the
  surface winds before the systems were designated as depressions. The
  satellite's unprecedented large swath width of 1800 km allows twice
  a day observation of most of the tropical oceans. SeaWinds data can,
  therefore, provide valuable guidance that are an important addition
  to the tools available to the tropical cyclone forecasting community.

---------------------------------------------------------
Title: Search for Short Variability Timescale of the GEV
    Gamma-Ray-Loud Blazars
Authors: Xie, G. Z.; Li, K. H.; Bai, J. M.; Dai, B. Z.; Liu, W. W.;
   Zhang, X.; Xing, S. Y.
2001ApJ...548..200X    Altcode:
  In this paper we report a brief description of 13 γ-ray-loud blazars as
  the second batch of the results of our blazar monitoring program. Six
  of the monitored objects show significant rapid variations. We found
  the typical minimum variability timescale to be about 1 hr. We have
  analyzed the relationships between optical variability and γ-ray
  variability and found that during 1995-1996 the TeV γ-ray emission
  of Mrk 501 correlated to its optical emission, based on our monitoring
  data in the optical band. This result will provide a strong constraint
  to the emission models.

---------------------------------------------------------
Title: The structure of protosolar accretion disk
Authors: Liu, W. J.; Huang, K. L.; Zhou, H. N.
2001AcASn..42....1L    Altcode:
  The structure of protosolar accretion disk during viscous diffusion
  stage is calculated. The standard αmodel is used to describe the
  viscosity in the optically thick protosolar accretion disc. The energy
  transport associated with radial motions is neglected and the vertical
  structure is constructed by assuming a Keplerian rotation and local
  hydrostatic and thermal equilibrium. The disk is heated by viscous
  dissipation and energy is transported by convection or radiation. It
  is found that the dependence of opacity on temperature is important to
  the disk structure. For the cold protosolar accretion disc, convective
  instability will gradually end from the outer region to the center and
  from the surface to central plane. So the formation of planets should
  first take place in the region where convection ends.

---------------------------------------------------------
Title: Bursty bulk flows without a near-Earth neutral line: Generation
    of fast intermittent flow in a highly curved magnetic field
Authors: Liu, W. William
2001JGR...106..289L    Altcode:
  Despite the heightened interest in bursty bulk flows (BBFs) in
  the magnetotail, there have been relatively few studies on how
  these fast intermittent flows occur in a region where slow and
  steady convection is expected. Conventional wisdom attributes
  BBFs to the formation of a near-Earth neutral line (NENL) on the
  appropriate side of the flow. We demonstrate that this view is
  not inevitable or necessary. We develop an alternate mechanism
  of BBFs generation based on the magnetohydrodynamics of a plasma
  situated in a Harris-type current sheet. We find that without a
  NENL or other extraneous assumptions, a highly curved current sheet
  (characterized by a field ratio |B<SUB>z</SUB>/B<SUB>x</SUB>|&lt;&lt;1)
  can generate high-speed cross-field flows of &gt;100 km/s when
  perturbed by modest impulses of ~10 km/s at its boundary. The
  flow has an Earthward sense in a thinning current sheet. The
  dependence on the field ratio of the maximal speed has the form
  c<SUB>1</SUB>+c<SUB>2</SUB>|B<SUB>x</SUB>/B<SUB>z</SUB>|<SUP>2</SUP>,
  where c<SUB>1</SUB> and c<SUB>2</SUB> are constants. For
  reasonable parameters the BBF threshold of 400 km/s is reached when
  B<SUB>z</SUB>/B<SUB>x</SUB> is approximately 0.1. The investigation
  also reveals attendant effects and signatures of the BBF-generating
  process, and these effects and signatures are listed as our theoretical
  predictions, against which better resolved satellite data from upcoming
  missions may be compared. We conclude with discussions on the potential
  role fast intermittent flows might play in the excitation of the
  substorm and other interesting magnetotail phenomena.

---------------------------------------------------------
Title: Coronal Magnetic Flux Rope Equilibria and Magnetic Helicity
Authors: Hu, You-Qiu; Jiang, Yan-Wei; Liu, Wei
2001ChJAA...1...77H    Altcode:
  Using a 2.5-dimensional (2.5-D) ideal MHD model, this paper analyzes
  the equilibrium properties of coronal magnetic flux ropes in a bipolar
  ambient magnetic field. It is found that the geometrical features
  of the magnetic flux rope, including the height of the rope axis,
  the half-width of the rope, and the length of the vertical current
  sheet below the rope, are determined by a single magnetic parameter,
  the magnetic helicity, which is the sum of the self-helicity of the
  rope and the mutual helicity between the rope field and the ambient
  magnetic field. All the geometrical parameters increase monotonically
  with increasing magnetic helicity. The implication of this result in
  solar active phenomena is briefly discussed.

---------------------------------------------------------
Title: A 2.5-dimensional Ideal Magnetohydrodynamic Model for Coronal
    Magnetic Flux Ropes
Authors: Hu, Y. Q.; Liu, W.
2000ApJ...540.1119H    Altcode:
  Coronal magnetic flux ropes are closely related to various solar active
  phenomena such as prominences, flares, and coronal mass ejections. Using
  a 2.5-dimensional (2.5-D), time-dependent ideal MHD model in Cartesian
  coordinates, a numerical study is carried out to find the equilibrium
  solution associated with a magnetic flux rope in the corona, which
  is assumed to emerge as a whole from the photosphere. The rope in
  equilibrium is characterized by its geometrical features such as the
  height of the axis, the half-width of the rope, and the length of the
  vertical current sheet below the rope, and its magnetic properties such
  as the axial and annular magnetic fluxes and the magnetic helicity as
  well, which are conserved quantities of the rope in the frame of ideal
  MHD. It is shown that, for a given bipolar ambient magnetic field, the
  magnetic flux rope is detached from the photosphere, leaving a vertical
  current sheet below, when its axial magnetic flux, annular magnetic
  flux, or magnetic helicity exceeds a certain critical value. The
  magnetic field is nearly force free in the rope but not in the
  prominence region, where the Lorentz force takes an important role in
  supporting the prominence appearing below the rope axis. The geometrical
  features of the rope vary smoothly with its magnetic properties, and
  no catastrophe occurs, a similar conclusion to that reached by Forbes
  &amp; Isenberg for magnetic flux ropes of large radius. Major Project
  19791090 supported by the National Natural Science Foundation of China.

---------------------------------------------------------
Title: Boron concentration and isotopic composition of halite from
    experiments and salt lakes in the Qaidam Basin
Authors: Liu, W. G.; Xiao, Y. K.; Peng, Z. C.; An, Z. S.; He, X. X.
2000GeCoA..64.2177L    Altcode:
  The concentration and isotopic abundance of boron in salt can be used to
  trace paleosalinities and depositional environments for marine and non
  marine evaporites. However, the mechanism of incorporating boron into
  halite during evaporation of salt lake brines is subject to dispute,
  and there have been few studies of boron concentrations and isotopic
  compositions during this process due to the low boron concentration in
  halite. A group of evaporation experiments from artificial solutions
  and salt lake brines have been analyzed in this study. The results of
  boron concentration and isotopic analyses demonstrate that the boron in
  halite comes mainly from fluid inclusions, with a lesser amount from
  coprecipitation. The isotopic fractionation factors between the brine
  and halite are from 0.9857 to 1.0000 for the evaporation experiments,
  and 0.9945 to 1.0009 for natural samples from the salt lake. The δ
  <SUP>11</SUP>B values of halite from the Qaidam Basin salt lakes vary
  from -4.7 to 25.8‰, compared to -4.7 to 31.4‰ in the salt lake
  brines. These values are controlled by the boron isotopic composition
  of the boron sources, pH values and Na/Ca ratios in the salt lake
  brines. The variation of boron isotopes in halite may be used to
  trace the hydrochemical evolution and paleoevaporation environment in
  salt lakes.

---------------------------------------------------------
Title: An SST anomaly dipole in the northern subtropical Pacific
    and its relationships with ENSO
Authors: Yu, Jin-Yi; Liu, W. Timothy; Mechoso, Carlos R.
2000GeoRL..27.1931Y    Altcode:
  This study examines the links between tropical and subtropical sea
  surface temperature (SST) anomalies in the Pacific Ocean during ENSO
  (El Niño-Southern Oscillation) events. A long-term simulation by the
  UCLA coupled atmosphere-ocean general circulation model is used. It is
  found that a zonally-oriented SST anomaly dipole in the subtropical
  Pacific develops almost simultaneously with and is closely related
  to tropical ENSO events. The dipole is located east of the dateline
  between 20°N and 40°N and consists of an anomaly center off the
  coast of the North America and another anomaly center with opposite
  sign further to the west. It is demonstrated that this dipole feature
  is primarily driven by anomalous surface heat fluxes associated with
  the altered atmospheric circulation during ENSO events.

---------------------------------------------------------
Title: Importance of salinity measurements in the heat storage
    estimation from TOPEX/POSEIDON
Authors: Sato, Olga T.; Polito, Paulo S.; Liu, W. Timothy
2000GeoRL..27..549S    Altcode:
  Sea surface height anomalies from satellite altimeter data are used
  to estimate heat storage. Since variability in sea surface height is
  mostly due to expansion and contraction of the water column it can be
  correlated with variations in the heat and salt content. Therefore,
  estimation of heat storage from altimeter data, when compared to in
  situ estimates, requires corrections for the haline effect. Three
  sites with a nearly continuous time series of temperature and salinity
  profiles simultaneous with TOPEX/POSEIDON data are studied: HOT,
  CalCOFI and Hydrostation “S”. Haline corrections based on in
  situ and climatological salinity measurements are contrasted. For the
  studied regions, the haline corrections based on climatology provide
  equivalent or worse results than not applying a correction at all. The
  use of in situ salinity estimates decreased the differences between the
  heat storage estimates (up to 17 × 10<SUP>7</SUP> J m<SUP>-2</SUP>)
  and significantly improved their correlation (up to 0.18).

---------------------------------------------------------
Title: Disturbance of prominence caused by magnetic cancellation
Authors: Liu, Wei; Hu, You-qiu; Xia, Li-dong; Yang, Yu-lin
2000ChA&A..24..365L    Altcode:
  Using a two-dimensional, three-component magnetohydrodynamic model, a
  numerical study is presented on the disturbance of prominence caused by
  photospheric magnetic cancellation. Photospheric magnetic cancellation
  below the prominence transports magnetic flux into the prominence,
  resulting in an increase of both magnetic flux and helicity in the
  prominence. The state of the prominence is related to its accumulated
  magnetic flux (or magnetic helicity). As shown in the numerical results,
  when δ<SUB>F</SUB> (the relative increment of magnetic flux in the
  prominence) or δ<SUB>H</SUB> (the corresponding relative increment
  of magnetic helicity) is small, the prominence rises and expands only
  slightly, and remains in contact with the photosphere. On the other
  hand, when δ<SUB>F</SUB> or δ<SUB>H</SUB> is large, the prominence
  is detached from the photosphere and eventually is suspended in the
  lower corona, leading to the formation of a vertical current sheet
  below the prominence.

---------------------------------------------------------
Title: What Will Happen When an Accelerating Black Hole Touches its
    Rindler Horizon
Authors: Zhao, Z.; Liu, W. B.; Jiang, Y. L.
2000graa.conf..112Z    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Angular Distribution for <SUP>7</SUP>Be(d, n)<SUP>8</SUP>B
    Reaction at E<SUB>c.m.</SUB> = 8.3 MeV and the Astrophysical
    S<SUB>17</SUB>(0) Factor for <SUP>7</SUP>Be(p, γ)<SUP>8</SUP>B
    Reaction
Authors: Wang, You-bao; Liu, Wei-ping; Bai, Xi-xiang; Li, Zhi-chang;
   Li, An-li; Zhou, Shu-hua; Zhu, Xiao-feng; Li, Xiao-mei; He, Gao-kui;
   Guo, Gang; Lian, Gang; Tang, Xiao-dong
1999ChPhL..16..873W    Altcode:
  The differential cross section for <SUP>7</SUP>Be(d, n)<SUP>8</SUP>B
  reaction at E<SUB>c.m.</SUB> = 8.3 MeV has been measured by using
  a <SUP>7</SUP>Be radioactive beam. The reaction cross section was
  determined to be 28 ± 3 mb. The astrophysical S<SUB>17</SUB>(0)
  factor for the <SUP>7</SUP>Be(p,γ)<SUP>8</SUP>B reaction was derived
  to be 24 ± 5 eV b through the asymptotic normalization constant of
  <SUP>8</SUP>B extracted from the experimental data. This result is
  found to be consistent with a previous value obtained from the same
  reaction at E<SUB>c.m.</SUB> = 5.8 MeV, implying the energy independence
  of this indirect method within the uncertainty.

---------------------------------------------------------
Title: CCD time-resolved photometry of four newly discovered CVs.
Authors: Liu, W.; Hu, J. Y.
1999PYunO....S.386L    Altcode:
  The authors present time-resolved optical light curves in R bands
  obtained from differential photometry on sequential CCD frame of 4
  new discovered high galactic latitude CVs, which are discovered by
  spectroscopic observations of the optical identification of ROSAT X-ray
  sources. The analysis of the light curves shows repeatable periodicity
  in these objects. J020348.7+295921 exhibits 0.5 m variation with
  orbital period of 258 min. J062518.2+733433 reveals a 0.3 mag modulation
  with orbital period of 254 min. J230949.6+213523 shows probably both
  orbital period of 207 min and WD spin period of 25 min. J232953.9+062814
  present short period of 32 min, indicating a magnetic system.

---------------------------------------------------------
Title: Optical Monitoring Sample of the GEV Gamma-Ray-loud Blazars
Authors: Xie, G. Z.; Li, K. H.; Zhang, X.; Bai, J. M.; Liu, W. W.
1999ApJ...522..846X    Altcode:
  We present optical monitoring between 1994 February and 1997 December of
  10 γ-ray-loud blazars included in our blazar monitoring program. Most
  of the monitored objects show significant rapid variations. The typical
  minimum variability timescale in the optical range is about 1 hour. We
  have analyzed the relationships between optical variability and γ-ray
  variability, and discussed theoretical models for the γ-ray-loud
  blazar emission.

---------------------------------------------------------
Title: Internal acceleration of relativistic electrons by
    large-amplitude ULF pulsations
Authors: Liu, W. W.; Rostoker, G.; Baker, D. N.
1999JGR...10417391L    Altcode:
  The flux of relativistic electrons in geostationary orbit exhibits a
  variability closely regulated by the solar wind, but the acceleration
  mechanism of relativistic electrons remains poorly understood. Recent
  observational evidence has shown that the intensification of
  relativistic electrons often takes place in a matter of several
  hours. The rapidity is difficult to reconcile with traditional
  diffusion-based models which often take days to produce appropriate
  high-energy electron fluxes and motivates us to search for alternative
  mechanisms of internal acceleration. Elaborating on the observation
  in an earlier paper of Rostoker et al. [1998], we propose that
  global oscillation of magnetosphere in the Pc4-5 range is capable
  of accelerating electrons under the catalysis of random pitch angle
  scattering. This view is developed theoretically and computationally
  in this paper. The most noteworthy result of the investigation is
  the demonstration that magnetic pumping by ULF waves can lead to the
  observed high relativistic electron flux in a time as short as a few
  hours under parameters appropriate for major magnetic storms. Further
  development and test of this theory are discussed.

---------------------------------------------------------
Title: Copper-Chloride Complexing in Hydrothermal Brines
Authors: McPhail, D. C.; Brugger, J.; Liu, W.; Spiccia, L.; Black, J.
1999nag..conf.7354M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Photometric monitoring of three BL Lacertae objects in
    1993-1998
Authors: Bai, J. M.; Xie, G. Z.; Li, K. H.; Zhang, X.; Liu, W. W.
1999A&AS..136..455B    Altcode:
  The results of optical photometric (BVRI) monitoring of three BL Lac
  objects over a time interval of about four years are presented. The
  sources are three classical radio-selected BL Lac objects, BL Lac, OJ
  287 and PKS 0735+178. During our observation OJ 287 was in the stage of
  a large periodic outburst which consisted of at least two peaks. Almost
  all the observations obtained over consecutive nights detected
  intranight variations. In 1995 and 1996 BL Lac kept in faint states,
  with fewer and smaller rapid flares and fluctuations. On the contrary,
  in late 1997 BL Lac was at the stage of a large outburst, accompanied
  with much more large amplitude rapid flares and fluctuations. PKS
  0735+178 was almost at its faint end from 1994 to early 1998. Over
  this time interval, the intraday variations and microvariations in
  PKS 0735+178 were rare and the amplitude was very small, except a
  rapid darkening of ~ 0.4 mag on 24 January 1995. Previous work by
  \cite[Webb et al. (1988);]{web88} \cite[Wagner et al. (1996);]{wag96}
  \cite[Pian et al. (1997)]{pia97} also showed the same behaviour of
  variability as BL Lac and PKS 0735+178 in BL Lac, S5 0716+714, PKS
  2155-304, respectively. We propose that the motion of orientation
  of the relativistic jet in a BL Lac object be responsible for these
  variability behaviours. Table~1 is only available in electronic form
  at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/Abstract.html

---------------------------------------------------------
Title: Spacebased observations of the seasonal changes of south
    Asian monsoons and oceanic responses
Authors: Liu, W. Timothy; Xie, Xiaosu
1999GeoRL..26.1473L    Altcode:
  The seasonal changes of monsoons in the South China Sea and the
  Arabian Sea are compared, using observations by spaceborne microwave
  scatterometers and radiometers. The oceanic responses to the forcing of
  wind stress and latent heat flux resulting from the monsoon changes are
  identified through surface temperature tendency and sea level changes.

---------------------------------------------------------
Title: Australasian Tektites Found in Guangxi Province, China
Authors: Povenmire, H.; Liu, W.; Xianlin, L.
1999LPI....30.1072P    Altcode:
  Newly confirmed Australasian tektites have been found in Guangxi
  Province, China. This is some 500 km NW of Guangdong and represents
  an important extension of this strewn field.

---------------------------------------------------------
Title: Condensation of Carbon in Supernovae: 1. Basic Chemistry
Authors: Liu, W.; Clayton, D. D.
1999LPI....30.1108L    Altcode:
  Contrary to the conventional wisdom on cosmic dust condensation based
  on thermochemical equilibrium theory, kinetic chemistry demonstrates
  that carbon condenses in supernovae even if C&lt;O because radioactivity
  destroys the CO trap.

---------------------------------------------------------
Title: An Experiment Using NSCAT Winds in the Numerical Prediction
    of Tropical Mesoscale Rainfall Systems under the influence of terrain
Authors: Chang, C. -P.; Lin, S. -C.; Liou, C. -S.; Liu, W. Timothy
1999GeoRL..26..311C    Altcode:
  The rich mesoscale information in NSCAT winds over tropical coastal
  regions is used in numerical simulations of two June 1997 monsoonal
  cases occurring over Taiwan. It is shown that transient NSCAT mesoscale
  information over a localized area as small as 120 km × 240 km can
  result in significant improvement in the 24 h heavy rainfall forecast
  due to its effect on monsoonal convection and terrain effects.

---------------------------------------------------------
Title: VizieR Online Data Catalog: BVRI photometry of 3 BL Lac objects
    (Bai+, 1999)
Authors: Bai, J. M.; Xie, G. Z.; Li, K. H.; Zhang, X.; Liu, W. W.
1999yCat..41360455B    Altcode:
  The results of optical photometric (BVRI) monitoring of three BL Lac
  objects over a time interval of about four years are presented. The
  sources are three classical radio-selected BL Lac objects, BL Lac, OJ
  287 and PKS 0735+178. During our observation OJ 287 was in the stage of
  a large periodic outburst which consisted of at least two peaks. Almost
  all the observations obtained over consecutive nights detected
  intranight variations. In 1995 and 1996 BL Lac kept in faint states,
  with fewer and smaller rapid flares and fluctuations. On the contrary,
  in late 1997 BL Lac was at the stage of a large outburst, accompanied
  with much more large amplitude rapid flares and fluctuations. PKS
  0735+178 was almost at its faint end from 1994 to early 1998. Over
  this time interval, the intraday variations and microvariations in
  PKS 0735+178 were rare and the amplitude was very small, except a
  rapid darkening of ~0.4mag on 24 January 1995. Previous work by Webb
  et al. (1988AJ.....95..374W), Wagner et al. (1996AJ....111.2187W)
  and Pian et al. (1997ApJ...486..784P) also showed the same behaviour
  of variability as BL Lac and PKS 0735+178 in BL Lac, S5 0716+714,
  PKS 2155-304, respectively. We propose that the motion of orientation
  of the relativistic jet in a BL Lac object be responsible for these
  variability behaviours. (1 data file).

---------------------------------------------------------
Title: CCD Time-Resolved Photometry of Four Newly Discovered CVs
Authors: Liu, W.; Hu, J. Y.
1999oaaf.conf..386L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: β decay of <SUP>40</SUP>Ti and <SUP>41</SUP>Ti and implication
    for solar-neutrino detection
Authors: Liu, W.; Hellström, M.; Collatz, R.; Benlliure, J.;
   Chulkov, L.; Gil, D. Cortina; Farget, F.; Grawe, H.; Hu, Z.; Iwasa,
   N.; Pfützner, M.; Piechaczek, A.; Raabe, R.; Reusen, I.; Roeckl,
   E.; Vancraeynest, G.; Wöhr, A.
1998PhRvC..58.2677L    Altcode:
  The β decay of <SUP>40</SUP>Ti and <SUP>41</SUP>Ti was studied by
  measuring the β-delayed proton and γ emission. The half-lives for
  <SUP>40</SUP>Ti and <SUP>41</SUP>Ti were determined to be 54(2)
  and 82(3) ms, respectively. The experimental β-decay strengths
  are compared with shell-model calculations and results from other
  measurements. The integrated Gamow-Teller strengths for <SUP>40</SUP>Ti
  and <SUP>41</SUP>Ti were found to be quenched, compared to the
  calculations, by factors of 0.79(3) and 0.93(3), respectively. Based
  on the experimental <SUP>40</SUP>Ti β-decay strength, the neutrino
  absorption cross section and induced neutrino event rates for
  <SUP>40</SUP>Ar were determined to be 14.3(3)×10<SUP>-43</SUP>
  cm<SUP>2</SUP> and 9.4+/-0.2(stat)<SUP>+1.3</SUP><SUB>-1.6</SUB>(syst)
  SNU, respectively.

---------------------------------------------------------
Title: A solitary wave packet in the atmosphere observed from space
Authors: Zheng, Quanan; Yan, Xiao-Hai; Liu, W. Timothy; Klemas, Vic;
   Greger, Dietmar; Wang, Zongming
1998GeoRL..25.3559Z    Altcode:
  A group of parallel cloud lines was identified in seven successive
  space shuttle photographs taken over the Pakistani offshore zone in
  the northern Arabian Sea on April 29, 1993. There are a total of 19
  lines aligned with the length of the leading line longer than 250 km
  and an average separation distance (wavelength) of 1 km. We suggest
  that the lines are generated by an atmospheric solitary wave packet
  characterized by decreases in amplitudes and wavelengths from the front
  to the rear. These features are comparable with the dnoidal soliton
  solution to the Korteweg-de Vries (KdV) equation. The land breeze and
  katabatic flow are proposed as a possible generation mechanism.

---------------------------------------------------------
Title: The intraday variability in the radio-selected and
    X-ray-selected BL Lacertae objects
Authors: Bai, J. M.; Xie, G. Z.; Li, K. H.; Zhang, X.; Liu, W. W.
1998A&AS..132...83B    Altcode:
  Seven BL Lac objects have been photometrically observed in an effort
  to study the difference of optical intraday variability between the
  radio-selected BL Lac objects (RBLs) and X-ray-selected BL Lac objects
  (XBLs). The objects we observed are selected arbitrarily. They are four
  RBLs, PKS 0735+178, PKS 0754+101, OJ 287 and BL Lac, and three XBLs,
  H 0323+022, H 0548-322 and H 2154-304. During the observation all of
  them exhibited microvariation, and H 0323+022 and H 0548-322 sometimes
  showed brightness oscillation. PKS 0735+178 and BL Lac were in their
  faint states and not very active. It seems that RBLs do not show
  microvariability more frequently than XBLs. Table 2 is only available
  in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr
  (130.79.128.5)

---------------------------------------------------------
Title: The impact of upper tropospheric humidity from microwave limb
    sounder on the midlatitude greenhouse effect
Authors: Hu, Hua; Liu, W. Timothy
1998GeoRL..25.3151H    Altcode:
  This paper presents an analysis of upper tropospheric humidity,
  as measured by the Microwave Limb Sounder, and the impact of the
  humidity on the greenhouse effect in the midlatitudes. Enhanced upper
  tropospheric humidity and an enhanced greenhouse effect occur over the
  storm tracks in the North Pacific and North Atlantic. In these areas,
  strong baroclinic activity and the large number of deep convective
  clouds transport more water vapor to the upper troposphere, and hence
  increase greenhouse trapping. The greenhouse effect increases with upper
  tropospheric humidity in areas with a moist upper troposphere (such as
  areas over storm tracks), but it is not sensitive to changes in upper
  tropospheric humidity in regions with a dry upper troposphere, clearly
  demonstrating that there are different mechanisms controlling the
  geographical distribution of the greenhouse effect in the midlatitudes.

---------------------------------------------------------
Title: VizieR Online Data Catalog: BVRI photometry of 7 BL Lac objects
    (Bai+ 1998)
Authors: Bai, J. M.; Xie, G. Z.; Li, K. H.; Zhang, X.; Liu, W. W.
1998yCat..41320083B    Altcode:
  Seven BL Lac objects have been photometrically observed in an effort
  to study the difference of optical intraday variability between the
  radio-selected BL Lac objects (RBLs) and X-ray-selected BL Lac objects
  (XBLs). The objects we observed are selected arbitrarily. They are
  four RBLs, PKS 0735+178, PKS 0754+101, OJ 287 and BL Lac, and three
  XBLs, H 0323+022, H 0548-322 and H 2154-304. During the observation
  all of them exhibited microvariation, and H 0323+022 and H 0548-322
  sometimes showed brightness oscillation. PKS 0735+178 and BL Lac were
  in their faint states and not very active. It seems that RBLs do not
  show microvariability more frequently than XBLs. (1 data file).

---------------------------------------------------------
Title: NASA scatterometer provides global ocean-surface wind fields
    with more structures than numerical weather prediction
Authors: Liu, W. Timothy; Tang, Wenqing; Polito, Paulo S.
1998GeoRL..25..761L    Altcode:
  The major differences between monthly-mean ocean-surface wind fields
  derived from the observations of the National Aeronautics and Space
  Administration (NASA) Scatterometer (NSCAT) and produced by the
  operational numerical weather prediction (NWP) model of the European
  Center for Medium-Range Weather Forecasts are found in coastal and
  equatorial regions, where the sharp changes are smoothed over in NWP
  products; these wind differences are explained to be the result of the
  superior spatial resolution of NSCAT winds. Objective interpolation of
  NSCAT data alleviates errors caused by the uneven satellite sampling
  and retains greater energy content of NSCAT winds at high wavenumbers.

---------------------------------------------------------
Title: Centrifugally driven instability of a rotationally dominated
    magnetodisc
Authors: Liu, W. W.
1998JGR...103.4707L    Altcode:
  The dynamics of a rotationally dominated magnetodisc is considered
  on the basis of linearized MHD. The treatment is prompted by the
  concern that the dominant theoretical view on this subject is based
  on the reduced framework of interchange motion, in which changes in
  magnetic field are suppressed. A realistic perturbation of a magnetodisc
  generally does not satisfy this constraint, and the changing magnetic
  field is expected to stabilize any small-amplitude perturbation. We
  reexamine the problem in an idealized slab magnetodisc geometry but
  with dynamical terms fully installed in the MHD equations. We find that
  the traditional interchange instability, essentially a centrifugal
  buoyancy regulated by the ionosphere, is not a proper solution for
  a thin magnetodisc. For short-wavelength modes the actual situation
  of instability comes to resemble what is known in the literature as
  magnetic buoyancy, i.e., a centrifugally driven motion moderated by
  the strong local magnetic field. Physically, the instability results
  as the rotational effects couple the Alfvén and slow modes; density
  perturbations formed by the latter are in turn driven radially
  by centrifugal buoyancy. The instability is manifest even for a
  perfectly uniform density distribution and for the characteristic
  parameters near the Io torus, dominates over the contribution from a
  radial density gradient. The theory of centrifugally driven radial
  diffusion is considered with this instability as the mechanism of
  eddy formation. This consideration gives a mass transport rate of
  ~10<SUP>3</SUP>kg/s and a density profile n~L<SUP>-4</SUP> near the Io
  torus, both in good agreement with observations. Further computational
  works need to be carried out to compare our model with more detailed
  in situ observations.

---------------------------------------------------------
Title: Precipitation of hot protons from a stretched near-earth
    current sheet
Authors: Liu, W. W.; Rostoker, G.; Samson, J. C.
1998mrat.conf..165L    Altcode:
  Recent observational evidences indicate that the near-Earth tail current
  sheet at approximately ten earth radii often experiences substantial
  and sudden changes which some researchers consider to be related to
  the substorm expansive phase onset. Observations of the ionosphere
  have revealed that auroral substorm activity is often preceded by
  an enhancement of precipitation of &gt;20 keV protons causing Hβ
  emissions. Protons in this energy range are most likely to be found
  in the near-Earth plasma sheet, giving support to the interpretation
  of a near-Earth source of substorm onset. However, the reason why
  proton precipitation intensifies during the auroral substorm has not
  yet been clarified. We propose that a possible explanation of this
  observation lies in the nonadiabatic dynamics of energetic protons in
  the stretched near-Earth current sheet formed in the late growth phase
  of the substorm. While pitch-angle scattering associated with such
  nonadiabatic dynamics has been considered before, there have been few
  studies which determine quantitatively how this process might contribute
  to proton precipitation. We have carried out numerical integrations
  of proton orbits in a magnetic field consisting of the Earth's main
  field and that due to a Harris current sheet. We find that, in the
  regime of highly nonadiabatic dynamics, the proton precipitation rate
  can exceed the already strong limit of isotropically filled loss-cone
  precipitation by an order of magnitude. This finding both contributes
  to our understanding of nonadiabatic effects on precipitation and fits
  nicely into the overall scheme of near-Earth onset theory.

---------------------------------------------------------
Title: Atomic and molecular supernovae
Authors: Liu, W.
1998sese.conf..649L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Atomic and Molecular Physics and Data Activities for
    Astrophysics at Oak Ridge National Laboratory
Authors: Jeffery, D. J.; Krstic, P. S.; Liu, W.; Schultz, D. R.;
   Stancil, P. C.
1998lss..work..101J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Supernova Chemistry
Authors: Liu, W.
1998ISAA....4..415L    Altcode: 1998masg.conf..415L
  No abstract at ADS

---------------------------------------------------------
Title: Supernova 1997dc in NGC 7678
Authors: Li, W. -D.; Liu, W.; Qiao, Q. -Y.; Esamdin, A.
1997IAUC.6716....1L    Altcode: 1997IAUC.6716Q...1L; 1997IAUC.6716A...1L
  W.-d. Li, Beijing Astronomical Observatory, reports that
  a low-resolution spectrogram (20 nm/mm, range 380-830 nm) of SN
  1997dc was obtained with the 2.16-m telescope at Xinglong station
  by Li, W. Liu, Q.-y. Qiao, and A. Esamdin. The spectrum shows broad
  emission and absorption lines typical of a type-Ic supernova at maximum
  light. The whole spectrum is very similar to that of SN 1994I at maximum
  light (Filippenko et al. 1995, Ap.J. 450, L11). Strong spectral lines
  include the Ca II infrared triplet and H and K lines; O I at 774 nm;
  Na I D/He I at 580 nm; Si II at 630 nm; and Fe II lines at 445, 490,
  and 508 nm. There is no distinct evidence of H Balmer lines.

---------------------------------------------------------
Title: Disruption of thin current sheets: A two-fluid theory
Authors: Liu, W. William
1997JGR...10214331L    Altcode:
  A growing list of observations and arguments has located the source
  region of magnetospheric substorms at the near-Earth plasma sheet within
  10R<SUB>E</SUB>. A popular descriptive paradigm conceptualizes the
  substorm initiation as a sudden disruption of a severely stretched
  magnetic field in the active region. The physical mechanism(s)
  responsible for the disruption have evoked intense theoretical and
  computational interests. In this paper we emphasize the macroscopic
  aspect of substorm onsets and propose to tackle the problem as a
  two-fluid instability of a plasma significantly polarized by an
  intense current. It is found that, for a center-maximized current
  distribution, a drift-wave instability with westward phase speed can
  grow on a timescale -10s when the current sheet thins to 1500-3000
  km. The phase speed, when mapped to the ionosphere, amounts to 3-5
  km/s and is directed westward. The longitudinal size (wavelength)
  of the fastest growing mode, when similarly mapped, is about 250-500
  km. These numbers agree with the morphology of current disruptions
  and westward traveling surges.

---------------------------------------------------------
Title: Eg Cancri: A New Wz Sge Type Dwarf Nova
Authors: Liu, W.; Li, Z. Y.; Hu, J. Y.
1997Ap&SS.257..183L    Altcode:
  We present the optical light curve of EG Cancri during its outburst
  in 1996-1997. It displayed some brightness fluctuations in the phase
  of decline. Mini-outbursts were detected. Optical spectra obtained
  during the decline showed it to be a dwarf nova on account of its broad
  absorption lines superimposed on a blue continuum. Optical spectra near
  minimum brightness revealed doubled Balmer lines in emission, over
  broad absorptions, but no HeII4686. An additional heating presented
  in the last stage of decline. CCD time-resolved photometry showed a
  possible orbital period 0.0575(26) day. Superhumps was observed during
  outburst byMatsumoto(1996). EG Cancri is a short-period CV which has
  a large-amplitude outburst(∼ 7 mag), a slow decline from outburst,
  and a long interval between outburst. From the above properties,
  a classification as a WZ Sge type DN is plausible.

---------------------------------------------------------
Title: Supernova 1997aa in IC 2102
Authors: Li, W. -D.; Qiu, Y. -L.; Qiaom, Q. -Y.; Hu, J. -Y.; Yuan,
   Q. -R.; Liu, W.
1997IAUC.6572....2L    Altcode: 1997IAUC.6572B...1L; 1997IAUC.6572R...1L
  W.-d. Li, Y.-l. Qiu, Q.-y. Qiaom and J.-y. Hu, Beijing Astronomical
  Observatory (BAO), on behalf of the BAO supernova survey, report the
  discovery of a supernova on CCD images of IC 2102 taken on Mar. 1.5
  UT with the BAO 0.60-m reflector. SN 1997aa is located at R.A. =
  4h51m53s.6, Decl. = -4 57'36" (equinox 2000.0), which is 25" west
  and 29" south of the center of IC 2102. Available unfiltered CCD
  magnitudes: Mar. 1.5, about 17.0; 2.5, about 16.7. A low-resolution
  spectrum (40 nm/mm, range 350-930 nm) obtained by Q.-r. Yuan (Nanjing
  Normal University) and W. Liu and W.-d. Li (BAO) on Mar. 2.5 with the
  BAO 2.16-m telescope at Xinglong station shows that this is an type-II
  supernova prior to optical maximum. There are weak, yet conspicuous,
  H Balmer lines superimposed on a very blue continuum. The expansion
  velocity of the photosphere is 15 000 km/s (as derived from the H-alpha
  line). H-beta could be seen only marginally.

---------------------------------------------------------
Title: Physics of the explosive growth phase: Ballooning instability
    revisited
Authors: Liu, W. William
1997JGR...102.4927L    Altcode:
  In situ observations have led to the notion of the explosive growth
  phase when the cross-tail current sheet inside L~10 suddenly thins in a
  time of ~1min. A theoretical explanation of the current intensification
  envisages the ballooning instability of magnetospheric plasma. In this
  paper, this theoretical notion is reanalyzed mathematically. In contrast
  to some previous work, we find that for a high-plasma, the ballooning
  instability can be excited easily by an earthward pressure gradient
  of any magnitude and for perturbations having parallel wavenumbers
  comparable to the field line curvature. The instability is compounded
  by its own development, leading ultimately to the extreme condition
  of a thin current sheet of a few ion gyroradius thick.

---------------------------------------------------------
Title: Seasonal and interannual variability of atmospheric convergence
    zones in the tropical Pacific observed with ERS-1 scatterometer
Authors: Zheng, Quanan; Yan, Xiao-Hai; Liu, W. Timothy; Tang, Wenqing;
   Kurz, Dragan
1997GeoRL..24..261Z    Altcode:
  Monthly images of atmospheric convergence zones in the tropical Pacific
  were produced with 1992-1994 ERS-1 scatterometer wind vectors. From the
  images, the position, width, and intensity of the convergence zones can
  be determined. Latitude-time sections of ocean surface wind divergence
  show that the summer position of the ITCZ in the eastern Pacific during
  the observed period exceeded the normal position northward by 3°-6°
  latitude, and the annual cycle in the western Pacific for 1994 was
  quite weak, implying a persistently unusual case.

---------------------------------------------------------
Title: Application of ERS scatterometer winds to typhoon, monsoon,
    rain &amp; EL Niño studies
Authors: Liu, W. T.; Tang, W. Q.
1997ESASP.414.1585L    Altcode: 1997sse..symp.1585L
  No abstract at ADS

---------------------------------------------------------
Title: Laboratory Evaluations of a CCD System For the Balloon-borne
    Solar Telescope
Authors: Song, Q.; Liu, W.; Ji, K.; Cao, W.; Huan, Z.
1997IAUJD..19E..49S    Altcode:
  The CCD camera, DALSA/CA-D7-1024, which is a commercial CCD system,
  is selected as the main detector for the BAO's Balloon-borne Solar
  Telescope. The principal parameters were tested by the YNAO, CCD-Testing
  Laboratory in the early September, 1996. The equipment of the lab and
  the method of the evaluations are described in the Poster. Evaluations
  show that the overall behavior of the camera is superb among the
  non-cooling commercial CCD systems. Nevertheless, there are some flaws
  in the image-collecting system which must be solved before launch.

---------------------------------------------------------
Title: A note on the interchange stability criterion
Authors: Liu, W. William
1996JGR...10127443L    Altcode:
  The correct stability criterion of interchange motions in the
  magnetosphere has been a question of some controversy. Many researchers
  hold the view first espoused by Gold [1959]. For a low-β plasma in a
  dipole magnetic field, Gold argued that the gradient of pV<SUP>γ</SUP>,
  where p is the plasma pressure, V is the unit flux tube volume, and
  γ is the adiabatic polytropic index, determines the interchange
  stability. This notion was further developed by Chandrasekhar
  [1960]. This common belief was questioned by Cheng [1985], who was
  subsequently questioned by Rogers and Sonnerup [1986] and Southwood and
  Kivelson [1987] on the issue. Is Gold's criterion the necessary and
  sufficient condition for interchange stability? We shall demonstrate
  that the answer is “no” and provide a more accurate criterion for
  the dipole magnetic field. We shall also discuss the interchange
  instability in a plasma distribution with a longitudinal gradient.

---------------------------------------------------------
Title: Effect of Hall conductivity on time-dependent convection
Authors: Liu, W. William
1996GeoRL..23.2903L    Altcode:
  Magnetospheric convection can be seen as a form of interchange motions,
  but unlike in an ideal MHD system, is subject to the ionospheric
  boundary condition. For general time-dependent interchanges, the Hall
  current in the ionosphere generates a field-aligned current independent
  of any background gradients. The effect of the Hall conductivity on
  time-dependent convection is isolated through a simple box model where
  pressure gradient and field line curvature are suppressed. Mathematical
  analysis suggests that the Hall conductivity can destabilize interchange
  modes with long longitudinal wavelength. The finding comes at the
  expense of a high degree of geometrical idealization. More realistic
  computations are needed to test the theory.

---------------------------------------------------------
Title: Photoelectric properties of a voltage-tunable two-color
    quantum well infrared photodetector
Authors: Cui, Liqiu; Jiang, De Sheng; Zhang, Yaohui; Wu, Wengang;
   Song, Chunying; Liu, Wei; Wang, Ruozhen
1996SPIE.2894...59C    Altcode:
  A new voltage-tunable two-order GaAs/AlGaAs multistacks quantum
  well infrared photodetector (QWIP) has been investigated in this
  work. The infrared photodetector consists of GaAs/AlAs/AlGaAs double
  barrier quantum wells (DBQWs) and GaAs/AlGaAs square quantum wells
  (SQWs) with photovoltaic and photoconductive dual-mode operation
  in the 3 approximately 5.3 micrometers and 7.5 approximately 12
  atmosphere windows. Experimental and theoretical studies have been
  conducted on the device physics of the intersubband transitions based
  on photoexcitation from ground state to different upper subbands
  including quasibound subband in DBQWs to virtual energy levels within
  the continuum in SQWs. These allow a better understanding of the
  optical and transport behaviors of the QWIP. The unique performance
  and very simple voltage-tunable switching behavior of the two-color
  GaAs/AlGaAs QWIP are expected to be quite competitive with HgCdTe
  and InSb infrared photodetectors for large area staring array imaging
  and two- color or multi-color detecting applications where material
  uniformity and simple device technology are important.

---------------------------------------------------------
Title: Optically coupled quantum well infrared detectors
Authors: Wu, Wengang; Cui, Liqiu; Jiang, De Sheng; Liu, Wei; Song,
   Chunying
1996SPIE.2894...48W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Low Energy Cosmic Ray Electrons and Diffuse Warm Ionized Medium
Authors: Liu, W.; Dalgarno, A.
1996AAS...188.4306L    Altcode: 1996BAAS...28..889L
  We propose that low energy cosmic ray electrons can maintain the
  diffuse warm ionized medium (DWIM), the principal component of the
  interstellar medium at high Galactic latitudes. We present a model
  of propagation of these electrons in the vertical direction of the
  Galactic disk and halo. These electrons lose energy by ionizing and
  exciting H, He, and He(+) , and as heat in the Coulomb scattering
  by the ambient thermal electrons as well as in the scattering by
  hydromagnetic waves. The resulting ionization and thermal structure
  is in good agreement with that of the interstellar medium indicated by
  pulsar dispersion measures and by observations of diffuse optical and 21
  cm emission and ultraviolet absorption. The gas is ionized and heated
  mainly by the low energy secondary electrons produced as the energetic
  electrons ionize the gas. Effects of the hydromagnetic waves on the
  ionization structure are small, especially for clumpy medium. It is
  predicted that helium is doubly ionized in the DWIM, consistent with
  the recent negative search for the He I recombination line at 5876
  Angstroms in the DWIM. The gas is cooled by electron-impact-induced
  emission of abundant atoms and ions. At small distances from the
  Galactic midplane, it is mainly by the forbidden line emission of S(+)
  and by the fine structure line emission of C(+) and Si(+) , and at
  large distances it is dominated by the two photon continuum emission
  of neutral hydrogen and by the forbidden line emission of C(+) , N(+) ,
  and O(+) . The temperature of the DWIM is determined to be about 10(4)
  K, in agreement with observations. There appears to be a progression
  toward reducing clumpiness from the Galactic disk to the halo.

---------------------------------------------------------
Title: Some new perspectives on quasi-static convection formalism
Authors: Liu, W. William
1996JGR...101.7891L    Altcode:
  Magnetospheric convection occurs in response to a combination of
  factors. It is driven by the solar wind-magnetosphere interaction,
  causes Joule heating in the ionosphere, and energizes particles as
  they convect earthward. While the equation governing magnetospheric
  convection under the quasi-static condition is well known, there
  is a lack of a formal proof that the energy processes named above
  are properly balanced in the convection formalism. In particular,
  the question has not been answered concerning the conservation of
  energy in a steady state convection. In this paper, I prove that
  energy conservation holds for steady state convection of an isotropic
  plasma. The consideration of energetics also sheds light on the nature
  of and relationship between region 1 and region 2 currents. It is
  further proven that the quasistatic convection formalism is conformal
  invariant, a property which can be exploited to develop more efficient
  algorithms for modeling magnetospheric convection. Several examples
  are presented to illustrate the conformal transformation method.

---------------------------------------------------------
Title: Application of spaceborne scatterometer to study typhoon,
    tropical hydrologic balance, and EL Nino
Authors: Liu, W. T.
1995SPIE.2583..228L    Altcode:
  The high spatial resolution and global coverage of a spaceborne
  microwave scatterometer make it a powerful instrument to study
  phenomena ranging from typhoons to El Nino Southern Oscillations
  which have regional and short term economic and ecological impacts
  as well as effects on long term and global climate changes. In this
  report, the application of scatterometer data, by itself, to study
  the intensity and the evolution of a typhoon is demonstrated. The
  potential of combining wind vector and precipitable water derived
  from two spaceborne sensors to study the hydrologic balance in the
  tropics is discussed. The role of westerly wind bursts as a precursor
  of anomalous warming in the equatorial Pacific is investigated with
  coincident data from microwave scatterometer, altimeter, and radiometer.

---------------------------------------------------------
Title: Energetic ring current particles generated by recurring
    substorm cycles
Authors: Liu, W. W.; Rostoker, G.
1995JGR...10021897L    Altcode:
  It is now generally accepted that substorm expansive phase activity
  involves a release of magnetotail energy, part of which is available
  for the acceleration of highly energetic particles (E&gt;100 keV) that
  play a role in ring current and radiation belt formation. However, the
  physical process whereby this acceleration takes place is not yet fully
  understood. In this paper we consider the physics of the acceleration
  process based on the tenet that acceleration of particles to E&gt;100
  keV occurs as a cumulative process involving a sequence of substorm
  expansive phases. In our view, nonadiabatic particle dynamics plays
  a key role in the energization process. We present both a qualitative
  description and quantitative treatment which starts with a consideration
  of a single particle and is then extended to track the evolution of the
  particle distribution function over several substorm expansive phase
  cycles. We stress two salient features of the evolution of particle
  distribution function, namely the rapid formation of a non-Maxwellian
  high-energy tail and the saturation of this tail distribution toward
  a kappa distribution in the asymptotic limit.

---------------------------------------------------------
Title: The Ultraviolet Spectrum of the Jovian Dayglow
Authors: Liu, W.; Dalgarno, A.
1995DPS....27.3013L    Altcode: 1995BAAS...27R1141L
  No abstract at ADS

---------------------------------------------------------
Title: The Ultraviolet Spectrum of the Jovian Dayglow
Authors: Liu, W.; Dalgarno, A.
1995AAS...186.3303L    Altcode: 1995BAAS...27..857L
  The ultraviolet spectra of the molecules H<SUB>2</SUB> and HD by
  solar fluorescence and photoelectron excitation are calculated and
  compared with the Jovian equatorial dayglow spectrum obtained by
  the Hopkins Ultraviolet Telescope at 3 Angstroms resolution near the
  maximicrons of solar cycle 22. The Jovian dayglow is accounted for
  in both the brightness and the spectral shape by solar fluorescence
  and photoelectron excitation, and no additional energy source is
  required. It is characterized by an H<SUB>2</SUB> rotational-vibrational
  temperature of 540 K and an H<SUB>2</SUB> column density of 7 times
  10(19) cm(-2) . The dayglow spectrum is in agreement with the presence
  of cascade contribution to the Lyman band emission from the high-lying
  E,F(1) Sigma_ {g}(+) states. The incorrectly perceived absence of
  appreciable cascade effects from comparison of the dayglow spectrum
  with the room-temperature laboratory spectrum of H<SUB>2</SUB> is
  caused by the fact that the spectrum of H<SUB>2</SUB> is sensitive
  to the temperature and the Jovian atmosphere is hotter. The observed
  weakness of the dayglow emission at short wavelengths is mainly caused
  by self-absorption by H<SUB>2</SUB>. The dayglow spectrum suggests
  minimal absorption by hydrocarbon on Jupiter. Wavelength coincidences
  of solar emission lines and absorption lines of H<SUB>2</SUB> and HD
  occur, resulting in strong fluorescence of H<SUB>2</SUB> and HD. The
  strong coincidence of the solar Lyman-beta line at 1025.72 Angstroms
  and the P(1) line of the (6,0) Lyman band of H<SUB>2</SUB> at 1025.93
  Angstroms together with other line coincidences produce unique line
  spectra which are identified in the dayglow spectrum. The fluorescence
  due to absorption of the solar O VI line at 1031.91 Angstroms by
  the vibrationally excited H<SUB>2</SUB> via the Q(3) line of the
  (1,1) Werner band at 1031.86 Angstroms is a sensitive measure of the
  atmospheric temperature. Despite strong coincidence of the solar O VI
  line at 1031.91 Angstroms and the R(0) line of the (6,0) Lyman band of
  HD at 1031.91 Angstroms, the molecule HD remains to be detected due to
  the weakness of the HD signature and the dominance of the H<SUB>2</SUB>
  emission.

---------------------------------------------------------
Title: Theory and observation of auroral substorms: A
    magnetohydrodynamic approach
Authors: Liu, W. W.; Xu, B. -L.; Samson, J. C.; Rostoker, G.
1995JGR...100...79L    Altcode:
  A theory of auroral substorm dynamics is constructed on the basis
  of MHD wave processes in the ionosphere-magnetosphere system. The
  basic view is that the substorm commences in the nightside near-Earth
  magnetosphere through a collapse of plasma equilibrium. The collapse
  releases a significant amount of free energy embedded initially in
  a collection of compressional waves. It is suggested that substorm
  dynamics after the collapse are determined by the evolution of these
  waves. We first investigate the quantitative ramifications of the
  waves in a two-dimensional box in the GSM yz cross section of the
  magnetotail. The model is constructed to allow the study of radiation
  of substorm wave energy into the solar wind and also encompasses the
  essential elements of resonant interaction in the plasma sheet boundary
  layer. The natural boundary condition leading to radiative loss is
  introduced. It is found that wave radiation into the solar wind can
  relax the magnetospheric system in less than a hour. The resonant
  Alfvén models driven by the normal compressional modes in the box
  are studied through the construction of proper dispersion equation. By
  studying the field-aligned current generated by resonances, we establish
  the auroral pattern expected to result from the coupling. Following
  the theoretical study, we examine an auroral substorm observed by
  the CANOPUS photometer array on February 20, 1990. It is found that,
  among the testable theoretical predictions, there exists a general
  agreement with the observations. We did find, however, that electron-
  and proton-induced aurora oscillate essentially in phase, thus implying
  a more complicated precipitation process.

---------------------------------------------------------
Title: The Oxygen Temperature of SN 1987A
Authors: Liu, W.; Dalgarno, A.
1994AAS...185.3304L    Altcode: 1994BAAS...26.1362L
  The temperature of the oxygen core of SN 1987A is determined
  by analyzing the processes that heat and cool the gas and the
  processes that form and destroy carbon monoxide. The heating and
  ionization rates are calculated by examining the processes by which
  the energetic electrons created following the radioactive decay of
  (56) Co lose energy in a mixed gas of atomic oxygen and carbon and
  carbon monoxide. The effects of non-uniform energy distribution in the
  supernova ejecta at early times due to the large optical depths of
  the gamma -rays of (56) Co are accounted for by reducing the energy
  input rate in the oxygen core according to the observed emission of
  CO. There is a large inhomogeneity in the thermal structure of the
  oxygen core because different cooling mechanisms are operative in
  different regions with different chemical compositions. The oxygen
  core contains a cold CO-emitting region which is effectively cooled
  by the vibrational emission of CO but heated by the O and C atoms
  as the result of nonthermal excitations by the energetic electrons,
  and a hot O-emitting region which contains neither CO nor SiO and
  is cooled by the metastable transitions of O. The temperature of the
  CO-emitting region is roughly a constant of 1800 K in the first year
  and drops to 700 K at 800 days, consistent with the observed spectral
  shapes of CO. The temperature of the O-emitting region is relatively
  high and ranges from 4800 K at 100 days to 2200 K at 800 days, in
  agreement with that inferred from the observations of the [OI]lambda
  lambda 6300,6364 emission doublet. The masses of CO predicted by the
  thermal-chemical model and derived from the observations agree well and
  permit no microscopic mixing of helium into the oxygen core. This work
  was supported by NSF grant AST-89-21939 and by NASA grant NAGW-1561.

---------------------------------------------------------
Title: Supernova 1994Y in NGC 5371
Authors: Clocchiatti, A.; Garcia-Lopez, R.; Barker, E. S.; Wren,
   W.; Wheeler, J. C.; Jiang, X. J.; Liu, W.; Hu, J. Y.; Boattini, A.;
   Tombelli, M.
1994IAUC.6065....1C    Altcode:
  A. Clocchiatti, R. Garcia-Lopez, E. S. Barker, W. Wren,
  and J. C. Wheeler, University of Texas, report: "A fully-reduced
  spectrogram (range 380-640 nm, resolution 1.3 nm) of SN 1994Y, obtained
  on Aug. 27.15 UT at the 2.7-m telescope of McDonald Observatory, shows
  the lines of the Balmer series and Na D in emission superimposed on
  a blue continuum. In the low-S/N spectrum, the emission lines do not
  show a P-Cyg absorption counterpart with the possible exception of
  Na D, but consist of a narrow core and a broad base, both centered at
  the velocity of NGC 5371. The FWHM of the broader components implies
  an expansion velocity of about 2600 km/s, while the FWZI implies a
  maximum expansion of about 7000 km/s. SN 1994Y apparently belongs to the
  'Seyfert 1' subclass of type-II supernovae (Filippenko 1989, A.J. 97,
  726), called type-IIn by Schlegel (1990, MNRAS 244, 269). Continuous
  monitoring of this event is strongly recommended." X. J. Jiang,
  W. Liu, and J. Y. Hu, Beijing Observatory, communicate: "A spectrogram
  (range 450-700 nm, resolution 0.53 nm/pixel) of SN 1994Y has been
  obtained using the 2.2-m telescope at Beijing Observatory, Xinglong,
  on Aug. 25. The spectrum shows strong Balmer emission, confirming it
  to be a type-II supernova. The wavelengths of the H-alpha and H-beta
  emission lines coincide with the radial velocity of the host galaxy
  NGC 5371 (2550 km/s). The emission lines are narrow compared with
  normal type-II supernovae; the FWHM of H-alpha and H-beta are about
  1200 km/s. Another dominating wide emission feature peaks at 592.9
  nm, possibly due to He I (587.6 nm) and Na I (589.3 nm). A feature at
  673.0 nm is from He I (667.8 nm). The spectrum is similar to that of
  SN 1994W, but without narrow absorption features at the blue side of
  the Balmer emission lines." A. Boattini and M. Tombelli, Florence,
  provide an accurate position for this object: R.A. = 13h53m30s.57,
  Decl. = +40o42'32".8 (equinox 1950.0).

---------------------------------------------------------
Title: An explicit bounce average calculation of adiabatic particle
    drifts
Authors: Liu, W. William
1994JGR....99.2383L    Altcode:
  The explicit method of bounce averaging the adiabatic drift of a
  charged particle is generalized, and the relationship of this method
  to earlier results derived from more implicitly based approaches is
  briefly discussed.

---------------------------------------------------------
Title: On the origin of auroral fingers
Authors: Liu, W. W.; Rostoker, G.
1993JGR....9817401L    Altcode:
  During the development of large-scale magnetospheric substorm expansive
  phase activity, the auroral oval may become very wide. During such
  episodes, clear discrete arc structures appear from time to time in
  the equatorward portion of the evening sector oval in a region of space
  normally thought to feature structureless diffuse auroras. On occasion,
  these discrete auroral forms acquire a north-south orientation and
  remain as identifiable forms for up to several minutes. Most auroral
  theories attempt to describe the origin of the normally east-west
  aligned features. In this paper we propose that the particles
  responsible for north-south aligned arc structures originate as plasma
  blobs injected into the central plasma sheet (CPS) from the adjacent
  low-latitude boundary layer, as a result of enhanced wave activity
  at the interface between the two regions during active times. We show
  that the characteristics geometric forms of the CPS auroral structures
  follow from tracking the drift paths of the particles in the injected
  plasma blob as they convect earthward, heating adiabatically in the
  process. We also outline outstanding issues pertaining to the proposal
  as motivation for a continued study.

---------------------------------------------------------
Title: Field-aligned flow in a centrifugally confined magnetodisc
Authors: Liu, W. W.
1993JGR....9815365L    Altcode:
  Significant magnetic field-aligned flows were detected by Voyager 1
  during its encounter with Jupiter. We try to understand the origin and
  dynamics of the field-aligned flow in the presence of a slow corotating
  convection. We find that the field-aligned flow is a necessary part
  in the preservation of the magnetodisc geometry and mass conservation
  in the disc. We further investigate the dynamical origin of the flow
  on the basis of a phenomenological equation, which indicates that the
  field-aligned dynamics is likely to be chaotic.

---------------------------------------------------------
Title: Observations of optical aurora modulated by resonant Alfvén
    waves
Authors: Xu, B. -L.; Samson, J. C.; Liu, W. W.; Creutzberg, F.;
   Hughes, T. J.
1993JGR....9811531X    Altcode:
  Optical aurora and magnetometer data from the Canadian Auroral Network
  for the OPEN Unified Study (CANOPUS) array in Canada are used in the
  study of the modulation of optical aurora in the 5577-Å and 4709-Å
  emission lines, by resonant shear Alfvén waves, in the frequency
  range of 1-4 mHz. A total of four events, carefully chosen to represent
  different characteristics of timing and location, are analyzed. Typical
  of these events, the power spectra featured discrete spectral peaks
  usually near 1.3, 1.9, and 3.1 mHz. Furthermore, latitudinal phase
  shifts of about 180° were typically observed across the latitudinal
  maximum of a given frequency peak. These observations point irrevocably
  to the field line resonance as a major factor in the modulation of
  precipitation and possibly in the acceleration of electrons in forming
  auroral arcs. Our study demonstrates that the modulation phenomena
  are common features occurring in the auroral oval, observable in an
  extensive latitude range, from 66° to 73° invariant latitude. Of the
  events, one shows the modulation process accompanied by an inverted V
  structure of electron precipitation in the evening sector near 72°. Two
  events are observed in the equatorward region of the auroral oval just
  before substorms onset, and maybe related to the energetic electron arcs
  which are the precursor of substorm intensification. The fourth event is
  seen in the morning sector at an equatorward latitude and occurs in the
  recovery phase of a substorm. The diversity of these modulation events
  allows us to further infer that resonant Alfvén waves play a direct
  role in controlling the luminosity variation of the optical aurora.

---------------------------------------------------------
Title: Ambipolar limit of electron precipitation
Authors: Liu, W. W.
1993GeoRL..20..343L    Altcode:
  In a magnetospheric condition, particles are often precipitated into
  the ionosphere of the host planet. When a flux tube is not interacting
  with those neighboring it, charge lost through its open ends to the
  ionosphere must vanish to ensure charge quasi-neutrality in the flux
  tube as a whole. To achieve this, a parallel electric field must
  be present to impede the faster electron motion. Electric fields so
  arisen are usually referred to as ambipolar fields. In this paper,
  we discuss a number of specific aspects of the ambipolar coupling,
  including the value of the ambipolar potential drop, the effects of
  loss cone depletion, the outflow of ionospheric electrons extracted
  by the ambipolar field, and point-to-point distribution of the
  potential. Although the noninteractive assumption for the flux tube
  restricts the validity of the treatment to cases where field-aligned
  currents are very weak, the construction of the model sheds new light
  on an important problem in magnetospheric physics.

---------------------------------------------------------
Title: Reaction rates for <SUP>8</SUP>Li(p, α) and <SUP>8</SUP>Li(p,
    n, α) and their effect on primordial nucleosynthesis
Authors: Becchetti, F. D.; Brown, J. A.; Liu, W. Z.; Jänecke, J. W.;
   Roberts, D. A.; Kolata, J. J.; Smith, R. J.; Lamkin, K.; Morsad, A.;
   Warner, R. E.; Boyd, R. N.; Kalen, J. D.
1992NuPhA.550..507B    Altcode:
  Differential-cross-section data are presented for the <SUP>8</SUP>Li(p,
  α)<SUP>5</SUP>He reaction at 1.5 MeV center-of-mass energy, measured
  with a (radioactive) <SUP>8</SUP>Li beam. The data are used to calculate
  one of the terms of the thermonuclear reaction rate for destruction of
  <SUP>8</SUP>Li. In addition, other data are used to estimate the total
  reaction rate for p+<SUP>8</SUP>Li, which is found to be comparable
  to that used in previous calculations of abundances from primordial
  nucleosynthesis.

---------------------------------------------------------
Title: Rotating magnetic anomalies as a possible accelerator of
    charged particles
Authors: Liu, W. W.
1992JGR....97.8145L    Altcode:
  We show, through the formulation of a simple theoretical model,
  that there exists a possibility that a significant number of a
  energetic ions in the Jovian magnetosphere, and presumably in other
  astrophysical environments beyond our direct access, owe their origin to
  a large-scale longitudinal magnetic anomaly corotating with the central
  body anchoring the magnetosphere, if the invoked magnetic anomaly has
  a typical boundary thickness comparable to an ion gyroradius, which
  for a preheated 10-kev heavy ion in the outer Jovian magnetosphere
  may be of the order of a few Jovian radii. The energy source for
  the acceleration is a torque from the central planet arising from a
  differential rotation between the ionosphere and the magnetosphere. The
  premise and outstanding issues pertaining to the present proposal are
  further discussed as motivating points for future studies.

---------------------------------------------------------
Title: Molecules in the Ejecta of Supernova 1987A
Authors: Dalgarno, A.; Liu, W.; Lepp, S.
1992csim.conf..221D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Radioactive Ion Beam Rates from Inverse Kinematics Reaction
    Yields at 0DEGREE
Authors: Tribble, R. E.; Liu, W.; Lui, Y. W.
1992unia.work..245T    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Molecules in Supernova 1987A
Authors: Liu, W.; Dalgarno, A.
1991BAAS...23.1352L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Chaos driven by kinetic Alfven waves
Authors: Liu, W. W.
1991GeoRL..18.1611L    Altcode:
  We present a simple model describing the effect of a kinetic Alfvén
  wave on the motion of a test electron along a closed magnetic field
  line. We show that the electron motion can be strongly chaotic for a
  wide range of conditions. The chaos exhibits a broad-band power spectrum
  in the frequency domain, although only three principal frequencies are
  involved in the model. Phase space density of electrons exhibits complex
  but physically interesting evolution in response to the KAW. Typical
  of a chaotic situation, the scale of the electron distribution in
  phase space descends rapidly over the scale hierarchy to give rise
  to a growing set of irregularities, which may in turn generate strong
  electrostatic turbulences. This chain of events suggests a fundamental
  mechanism that couples physical processes of different scales.

---------------------------------------------------------
Title: Effect of dawn-dusk pressure asymmetry on convection in the
    central plasma sheet
Authors: Liu, W. W.; Rostoker, G.
1991JGR....9611501L    Altcode:
  The central plasma sheet (CPS) of the Earth's magnetosphere contains
  a thermally differentiated plasma, whose ion temperature exceeds
  severalfold its electron temperature. The gradient/curvature drift of
  ions and electrons of the CPS plasma tend to separate the two species
  in the dawn-dusk direction. Because of the temperature difference, the
  dusk CPS, which gains a surplus of hotter ions, is expected to have
  a larger plasma pressure than its dawnside counterpart. Preliminary
  analysis of ISEE 1 plasma data confirmed the pressence of such a
  pressure asymmetry in the CPS during the quiet and the growth-of-driven
  conditions. The closure of the electric current created by this pressure
  asymmetry usually requires the flow of a field-aligned current, whose
  effects of the E×B drift of the CPS plasma are the central focus of
  this paper. The dawn-dusk asymmetry in the magnetosphere generally
  leads to an azimuthally asymmetric ionospheric convection, with close
  resemblance to the streamline structure first identified by Heppner
  (1977). The field-aligned current associated with the asymmetry has
  a strong effect in shielding the inner magnetosphere, in which the
  imposed electric field decreases exponentially for polytropic indices
  greater than 1. The asymmetry also affects the location of the inner
  edge of the plasma sheet. We present a simplified model in this paper,
  using an analytic paradigm to portrary the general properties of the
  asymmetry-induced effects. A limited attempt is made to examine how
  a departure from the idealized condition would change the solution of
  the problem.

---------------------------------------------------------
Title: MARS: a status report
Authors: Tribble, R. E.; Gagliardi, C. A.; Liu, W.
1991NIMPB..56..956T    Altcode:
  We are building a momentum achromat recoil spectrometer (MARS)
  for use with the new K500 superconducting cyclotron at Texas
  A&amp;M University. MARS uses a unique optical design utilizing two
  dispersive planes to combine a momentum achromat with a recoil mass
  spectrometer. This configuration makes MARS applicable to a broad range
  of nuclear reaction studies utilizing inverse kinematics. It also leads
  to a system that is well matched to the range of secondary particle
  energies that will be produced in reactions with K500 beam. MARS
  will have a typical mass resolution of δM/M ~ 1/300, with an energy
  acceptance of +/- 9% ΔE/E and a geometric solid angle of up to 9
  msr. A beam swinger system will allow reaction products in the angular
  range 0° to 30° to be studied. MARS will be used to study both the
  excited states and decay properties of very proton- and neutron-rich
  nuclei. MARS will also be used to provide a reaction mechanism filter
  to assist investigations of the dynamics of heavy ion collisions and
  to produce secondary radioactive beams for reaction and spectroscopic
  studies of particular interest for nuclear astrophysics. We briefly
  describe the design of MARS, give a status report on its construction
  and an overview of the scientific program planned for it.

---------------------------------------------------------
Title: Synthetic Observation and Analysis of the Strong Flare
    Events 1989AUG
Authors: Liu, W. T.; Huang, Z.; Zheng, R. M.
1990PYunO...4..227L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Effect of plasma mantle injection on the dynamics of the
    distant magnetotail
Authors: Liu, W. W.; Hill, T. W.
1990JGR....9518849L    Altcode:
  We investigate the role of the plasma mantle in the dynamics of the
  Earth's distant magnetotail. The plasma mantle can exert a substantial
  influence on the current-sheet force equilibrium by transporting both
  momentum and mass from the dayside magnetopause to the tail current
  sheet. Such influences are particularly strong when the interplanetary
  magnetic field contains a significant southward component for a
  prolonged period. We find that a number of processes characterizing a
  substorm growth phase can be attributed, at least in part, to the plasma
  mantle. Among these processes are the thinning of the plasma sheet,
  storage of magnetic energy in the tail, and formation of plasmoids. The
  rates of these processes are found to increase nonlinearly with the
  momentum density of the mantle plasma. The present model applies only
  to the distant magnetotail (x&lt;~-30R<SUB>E</SUB>) because of various
  approximations that we make to allow an analytical treatment of the
  governing equations.

---------------------------------------------------------
Title: Ionospheric outflow of plasma and compression relationship
    in the plasma sheet
Authors: Liu, W. W.; Rostoker, G.
1990GeoRL..17.1849L    Altcode:
  We are concerned in this article with the curious finding of Huang
  et al. [1989] which suggests a polytropic index of plasma compression
  of about 0.7 in the quiet time central plasma sheet. We show that the
  reduction of this index from its adiabatic value (=5/3) can be achieved
  through an ionospheric outflow of plasma which lowers the plasma
  temperature by virtue of energy partition. The observed correlation
  between the plasma temperature and density is best reproduced by
  an ionospheric source of ∼5×10<SUP>25</SUP> ions/s, consistent
  with independent experinental estimates and smaller than the average
  solar wind source by a factor of two or more. Despite the change in
  the polytropic relationship, we find that the global energy equation
  PV<SUP>5/3</SUP>=constant (V=volume of a unit flux tube) still holds
  approximately (in the absence of other energy-loss mechanisms).

---------------------------------------------------------
Title: Radial diffusion of iogenic plasma in a centrifugally-driven
    turbulence
Authors: Liu, W. W.
1990P&SS...38..995L    Altcode:
  A quantitative model of plasma diffusion from the Io torus, driven
  by the centrifugal force of Jupiter's rotation, is developed. It is
  argued that the unstable mode of perturbation, which would lead to a
  system of deterministic motion of plasma, should be dominated by a more
  turbulent mode of motion in order to effect a longer trapping time of
  the Iogenic plasma as implied by the observations. The energy of the
  turbulent motion is derived internally from the centrifugal potential
  of the planetary rotation. The length scale of the turbulence cells is
  determined by the interaction between the magnetospheric plasma and the
  dissipative ionosphere, and found to be of order 0.1 R<SUB>J</SUB> for
  the Jovian magnetosphere. Since the cells are smaller than the dimension
  of the system, the transport of the plasma can be studied as a problem
  of eddy diffusion, governed by the Fokker-Planck equation. A specific
  model is established based on the above considerations. Investigation of
  this model shows that the nominal L<SUP>-5</SUP> dependence of plasma
  density can be reproduced in an appropriate limit. Other details
  of the density distribution (e.g. the density ramp located at L =
  7.5) can be attributed to the spatial variation of the ionospheric
  Pedersen conductance. The density ramp implies a conductivity peak
  in its magnetically conjugate ionosphere. The conductivity profile
  consistent with the observed density distribution is solved. The inward
  expansion of the Io torus effected by fringing electric field of the
  outer torus is also briefly discussed.

---------------------------------------------------------
Title: Convective transport of plasma in the inner Jovian
    magnetosphere
Authors: Liu, W. W.; Hill, T. W.
1990JGR....95.4017L    Altcode:
  We investigate the transport of plasma in the inner Jovian magnetosphere
  according to the corotating model of Hill et al. [1981], emphasizing
  mathematical aspects of the theory. We employ a simplified but
  physically plausible boundary condition at the inner Io torus,
  representing a 5% density enhancement of S<SUP>+</SUP> ions in an
  “active sector” that is fixed in Jovian (systems III) longitude. We
  first investigate the convection electric field pattern resulting from
  this longitudinal mass anomaly alone, and then generalize the theory
  to include the effects of Coriolis force and plasma acceleration. We
  find that even a small (~5%) longitudinal asymmetry of the inner torus
  produces a convection system capable of removing torus plasma from
  the magnetosphere on a time scale of order one month.

---------------------------------------------------------
Title: Some Special Phenomena on Ionograms at Wuchang China
Authors: Liu, W.
1990PYunO.199....1L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Corotation lag and magnetospheric energetics of Jupiter
Authors: Liu, W. W.
1989P&SS...37.1393L    Altcode:
  Jupiter exerts an enormous torque upon its magnetospheric plasma to
  force the latter to corotate. However, the corotation is generally
  not perfect due to internal production of plasma and/or its outward
  transport. In a steady state in which the magnetosphere rotationally
  lags behind the ionosphere, a Birkeland current system is formed to
  couple the two regions. This current is found to play a dual role in
  the magnetospheric energetics of Jupiter. On the one hand, it transfers
  energy from the planetary rotation to the magnetosphere; on the other
  hand, it returns part of this transferred energy back to the ionosphere
  to drive the ionospheric current required for the maintenance of the
  current system. Owing to this partition of energy, the magnetosphere
  gets only about one third of the energy extracted from the planetary
  rotation, with the rest going to the ionosphere as Joule heating. The
  total energy delivery from the planetary rotation amounts to over 10
  <SUP>14</SUP> W, considerably larger than the solar wind contribution.

---------------------------------------------------------
Title: A Radioactive Beam Facility Using a Large Superconducting
    Solenoid
Authors: Becchetti, F. D.; Liu, W. Z.; Roberts, D. A.; Jänecke,
   J. W.; Kolata, J. J.; Morsad, A.; Kong, X. J.; Warner, R. E.
1989hipn.conf..277B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Supporting Electronics System for New Hydrogen Maser H7
Authors: Lin, C. F.; Liu, W. J.; Wu, Y.
1989AnShO..10..229L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Paleomagnetism of sedimentary rocks from and near the DOSECC
    Cajon Pass Well, southern California
Authors: Liu, Wei; Kirschvink, Joseph L.; Weldon, Ray J.
1988GeoRL..15.1065L    Altcode:
  As part of a larger study of the geologic and tectonic history of the
  Cajon Pass area, we conducted paleomagnetic studies on sedimentary
  rocks recovered from the Cajon Pass DOSECC well, and adjacent surface
  exposures from unit 5 of the late Early to Middle Miocene Cajon Fm. A
  comparison of the magnetic polarity stratigraphy of the surface and
  the core sections suggests that they do not match well, which may imply
  that the rocks at depth have been deformed so that simple extrapolation
  from the surficial geology to depth is not possible. Although tectonic
  rotation cannot be inferred from the samples from the core, a clockwise
  rotation of 30 ± 8.9° was found in unit 5 of the Cajon Fm near the
  well site at the surface, which is consistent with the results from the
  same unit 2 km to the west. In contrast, the early Late to late Early
  Miocene Crowder Fm across the Squaw Peak fault and the youngest unit,
  unit 6, of the Cajon Fm at the northwestern end of the formation have
  not been rotated. The rotation of unit 5 near the Squaw Peak fault is
  thus probably local, caused by drag associated with the fault.

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Title: Quark-number susceptibility of high-temperature QCD
Authors: Gottlieb, Steven; Liu, W.; Toussaint, D.; Renken, R. L.;
   Sugar, R. L.
1987PhRvL..59.2247G    Altcode:
  We measure the response of the quark number to an infinitesimal chemical
  potential in high-temperature QCD with two light flavors of dynamical
  fermions. In the chirally symmetric phase the susceptibilities for quark
  number density and for the density of the third component of isospin are
  large and equal within statistics, which is consistent with a plasma
  of light quarks. In the broken-symmetry phase the susceptibility for
  quark number density is small, as expected from quark confinement.

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Title: Corotating convection revisited
Authors: Hill, T. W.; Liu, W. W.
1987GeoRL..14..178H    Altcode:
  The corotating convection model invokes a systematic large-scale
  pattern of plasma motion through the Jovian magnetosphere, a pattern
  fixed in corotating (System III) coordinates and established by an
  observed longitudinal asymmetry of the S<SUP>+</SUP> ion distribution
  in the inner Io torus. In its various versions published to date,
  the corotating convection model would preserve this longitudinal
  asymmetry throughout the magnetospheric convection system; the model
  is thus in conflict with the high degree of longitudinal symmetry
  that is observed to exist in the hot outer Io torus and presumed to
  exist also in the magnetosphere outside the torus. We propose to solve
  this difficulty by superimposing on the corotating convection system
  a strong retrograde flow confined to the torus region, representing
  the corotation lag associated with ion production and charge exchange
  in the Io torus. The addition of this azimuthal flow in the torus
  region renders the plasma density distribution almost symmetric with
  respect to longitude in the outer torus and beyond (as required by
  direct observation), while retaining a corotating convection pattern
  outside the torus (whose existence is supported indirectly by a number
  of observations). Serendipitously, the condition of approximate
  azimuthal symmetry of the plasma density distribution permits an
  analytic solution of the otherwise intractable equations governing
  the corotating convection pattern.

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Title: Velocity filter effect and dynamics of distant magnetotail
Authors: Liu, W. W.; Hill, T. W.
1986P&SS...34..197L    Altcode:
  The velocity filter effect produces a persistent time variation
  of the self-consistent magnetic-field configuration in the Earth's
  distant magnetotail. In the presence of a mantle source of plasma,
  a steady-state configuration cannot be attained, even if the source
  supply is constant in time. The velocity filter effect produces an
  evolution of the magnetotail such that the plasma sheet thins throughout
  the region accessible to the incoming plasma. This thinning process,
  widely observed and theoretically predicted, leads to current-sheet
  disruption when the thickness of the plasma sheet shrinks to a critical
  value. The whole process lasts 1-2 h, consistent with the observed
  duration of a typical substorm growth phase.

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Title: Synthetic aperture radar observation of ocean roughness from
    rolls in an unstable marine boundary layer
Authors: Thompson, T. W.; Liu, W. T.; Weissman, D. E.
1983GeoRL..10.1172T    Altcode:
  Simultaneous synthetic aperture radar (SAR) and cloud photographic
  observations of the Atlantic Ocean off the coast of Florida were made
  from a high-altitude aircraft when there was an unstable marine boundary
  layer. The synthetic aperture radar images show unusual kilometer-sized
  features on the ocean surface which are related to clouds. The ocean
  near shore was cloud-free and had no radar features, while from 30
  to 330 km offshore there were clouds and prominent kilometer-sized
  features in the SAR image. These radar features are most prominent
  when the radar was looking upwind, are less prominent when the radar
  was looking downwind, and disappear entirely when the radar was
  looking crosswind. Since ocean radar echo strengths are believed to
  be controlled primarily by ocean waves satisfying the Bragg relation,
  these radar features most likely resulted from local enhancements of
  short gravity waves with 17- to 34-cm wavelengths, which in turn are
  surface expressions of roll convections in a kilometer-thick unstable
  marine boundary layer.

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Title: An Operational Large-Scale Marine Planetary Boundary Layer
    Model.
Authors: Brown, R. A.; Liu, W. Timothy
1982JApMe..21..261B    Altcode:
  An operational planetary boundary layer model (Brown, 1974,1978, 1981)
  for determining surface winds and stress from free-stream flow has been
  modified for the marine layer by including surface roughness feedback,
  variable humidity and interfacial layer effects. The surface winds
  determined from synoptic-scale pressure and temperature fields are
  compared to surface measurements in GOASEX and JASIN.

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Title: Precise determination of the difference between path delays
    in clock synchronization using TV signals.
Authors: Liu, W. -Z.; Luo, D. -C.
1981ssa..confQ.366L    Altcode:
  No abstract at ADS

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Title: Precise Determination of the Difference between Path Delays
    in Clock Synchronization Using TV Signal
Authors: Liu, W. Z.; et al.
1980ssa..confQ.366L    Altcode:
  No abstract at ADS

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Title: A Frequency Calibrator by Subcarrier of PAL TV System
Authors: Zhang, M. Y.; Lo, D. C.; Liu, W. Z.
1979PBeiO...4...64Z    Altcode:
  No abstract at ADS

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Title: An experimental determination of the gravitational constant
    at distances around ten meters.
Authors: Yu, H. -T.; Ni, W. -T.; Hu, C. -C.; Liu, F. -H.; Yang,
   C. -H.; Liu, W. -N.
1979ChJPh..16..201Y    Altcode:
  No abstract at ADS

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Title: Temperature profile in the molecular sublayer near the
    interface of a fluid in turbulent motion
Authors: Liu, W. Timothy; Businger, Joost A.
1975GeoRL...2..403L    Altcode:
  The molecular sublayers adjacent to the air-sea interface are assumed
  to undergo cyclic growth and destruction in order to explain the
  exponential temperature profiles measured by Khundzhua and Andreyev. The
  duration of such cycles is taken to be randomly distributed in forced
  convection and a constant period is used to determine the temperature
  profile in free convection.