explanation      blue bibcodes open ADS page with paths to full text
Author name code: kano
ADS astronomy entries on 2022-09-14
author:"Kano, Ryouhei" 

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Title: Quiet Sun Center to Limb Variation of the Linear Polarization
    Observed by CLASP2 Across the Mg II h and k Lines
Authors: Rachmeler, L. A.; Bueno, J. Trujillo; McKenzie, D. E.;
   Ishikawa, R.; Auchère, F.; Kobayashi, K.; Kano, R.; Okamoto,
   T. J.; Bethge, C. W.; Song, D.; Ballester, E. Alsina; Belluzzi,
   L.; Pino Alemán, T. del; Ramos, A. Asensio; Yoshida, M.; Shimizu,
   T.; Winebarger, A.; Kobelski, A. R.; Vigil, G. D.; Pontieu, B. De;
   Narukage, N.; Kubo, M.; Sakao, T.; Hara, H.; Suematsu, Y.; Štěpán,
   J.; Carlsson, M.; Leenaarts, J.
2022ApJ...936...67R    Altcode: 2022arXiv220701788R
  The CLASP2 (Chromospheric LAyer Spectro-Polarimeter 2) sounding rocket
  mission was launched on 2019 April 11. CLASP2 measured the four Stokes
  parameters of the Mg II h and k spectral region around 2800 Å along a
  200″ slit at three locations on the solar disk, achieving the first
  spatially and spectrally resolved observations of the solar polarization
  in this near-ultraviolet region. The focus of the work presented here
  is the center-to-limb variation of the linear polarization across these
  resonance lines, which is produced by the scattering of anisotropic
  radiation in the solar atmosphere. The linear polarization signals of
  the Mg II h and k lines are sensitive to the magnetic field from the
  low to the upper chromosphere through the Hanle and magneto-optical
  effects. We compare the observations to theoretical predictions
  from radiative transfer calculations in unmagnetized semiempirical
  models, arguing that magnetic fields and horizontal inhomogeneities
  are needed to explain the observed polarization signals and spatial
  variations. This comparison is an important step in both validating and
  refining our understanding of the physical origin of these polarization
  signatures, and also in paving the way toward future space telescopes
  for probing the magnetic fields of the solar upper atmosphere via
  ultraviolet spectropolarimetry.

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Title: CASPER: A mission to study the time-dependent evolution of
    the magnetic solar chromosphere and transition regions
Authors: Orozco Suárez, D.; del Toro Iniesta, J. C.; Bailén, F. J.;
   López Jiménez, A.; Balaguez Jiménez, M.; Bellot Rubio, L. R.;
   Ishikawa, R.; Katsukawa, Y.; Kano, R.; Shimizu, T.; Trujillo Bueno,
   J.; Asensio Ramos, A.; del Pino Alemán, T.
2022ExA...tmp...26O    Altcode:
  Our knowledge about the solar chromosphere and transition region (TR)
  has increased in the last decade thanks to the huge scientific return
  of space-borne observatories like SDO, IRIS, and Hinode, and suborbital
  rocket experiments like CLASP1, CLASP2, and Hi-C. However, the magnetic
  nature of those solar regions remain barely explored. The chromosphere
  and TR of the Sun harbor weak fields and are in a low ionization stage
  both having critical effects on their thermodynamic behavior. Relatively
  cold gas structures, such as spicules and prominences, are located in
  these two regions and display a dynamic evolution in high-resolution
  observations that static and instantaneous 3D-magnetohydrodynamic (MHD)
  models are not able to reproduce. The role of the chromosphere and TR
  as the necessary path to a (largely unexplained) very hot corona calls
  for the generation of observationally based, time-dependent models
  of these two layers that include essential, up to now disregarded,
  ingredients in the modeling such as the vector magnetic field. We
  believe that the community is convinced that the origin of both the
  heat and kinetic energy observed in the upper layers of the solar
  atmosphere is of magnetic origin, but reliable magnetic field
  measurements are missing. The access to sensitive polarimetric
  measurements in the ultraviolet wavelengths has been elusive until
  recently due to limitations in the available technology. We propose a
  low-risk and high-Technology Readiness Level (TRL) mission to explore
  the magnetism and dynamics of the solar chromosphere and TR. The mission
  baseline is a low-Earth, Sun-synchronous orbit at an altitude between
  600 and 800 km. The proposed scientific payload consists of a 30 cm
  aperture telescope with a spectropolarimeter covering the hydrogen
  Ly-alpha and the Mg II h&k ultraviolet lines. The instrument shall
  record high-cadence, full spectropolarimetric observations of the
  solar upper atmosphere. Besides the answers to a fundamental solar
  problem the mission has a broader scientific return. For example,
  the time-dependent modeling of the chromospheres of stars harboring
  exoplanets is fundamental for estimating the planetary radiation
  environment. The mission is based on technologies that are mature
  enough for space and will provide scientific measurements that are
  not available by other means.

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Title: Empirical relations between the intensities of Lyman lines
    of H and He<SUP>+</SUP>
Authors: Gordino, M.; Auchère, F.; Vial, J. -C.; Bocchialini, K.;
   Hassler, D. M.; Bando, T.; Ishikawa, R.; Kano, R.; Kobayashi, K.;
   Narukage, N.; Trujillo Bueno, J.; Winebarger, A.
2022A&A...657A..86G    Altcode: 2022arXiv220101519G
  Context. Empirical relations between major UV and extreme UV spectral
  lines are one of the inputs for models of chromospheric and coronal
  spectral radiances and irradiances. They are also needed for the
  interpretation of some of the observations of the Solar Orbiter
  mission. <BR /> Aims: We aim to determine an empirical relation between
  the intensities of the H I 121.6 nm and He II 30.4 nm Ly-α lines. <BR
  /> Methods: Images at 121.6 nm from the Chromospheric Lyman-Alpha
  Spectro Polarimeter (CLASP) and Multiple XUV Imager (MXUVI) sounding
  rockets were co-registered with simultaneous images at 30.4 nm from the
  EIT and AIA orbital telescopes in order to derive a spatially resolved
  relationship between the intensities. <BR /> Results: We have obtained
  a relationship between the H I 121.6 nm and He II 30.4 nm intensities
  that is valid for a wide range of solar features, intensities, and
  activity levels. Additional SUMER data have allowed the derivation of
  another relation between the H I 102.5 nm (Ly-β) and He II 30.4 nm
  lines for quiet-Sun regions. We combined these two relationships to
  obtain a Ly-α/Ly-β intensity ratio that is comparable to the few
  previously published results. <BR /> Conclusions: The relationship
  between the H I 121.6 nm and He II 30.4 nm lines is consistent with the
  one previously obtained using irradiance data. We have also observed
  that this relation is stable in time but that its accuracy depends on
  the spatial resolution of the observations. The derived Ly-α/Ly-β
  intensity ratio is also compatible with previous results.

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Title: Demonstration of Chromospheric Magnetic Mapping with CLASP2.1
Authors: McKenzie, David; Ishikawa, Ryohko; Trujillo Bueno, Javier;
   Auchere, F.; Kobayashi, Ken; Winebarger, Amy; Kano, Ryouhei; Song,
   Donguk; Okamoto, Joten; Rachmeler, Laurel; De Pontieu, Bart; Vigil,
   Genevieve; Belluzzi, Luca; Alsina Ballester, Ernest; del Pino Aleman,
   Tanausu; Bethge, Christian; Sakao, Taro; Stepan, Jiri
2021AGUFMSH52A..06M    Altcode:
  Probing the magnetic nature of the Suns atmosphere requires measurement
  of the Stokes I, Q, U and V profiles of relevant spectral lines (of
  which Q, U and V encode the magnetic field information). Many of the
  magnetically sensitive lines formed in the chromosphere and transition
  region are in the ultraviolet spectrum, necessitating observations
  above the absorbing terrestrial atmosphere. The Chromospheric
  Layer Spectro-Polarimeter (CLASP2) sounding rocket was flown
  successfully in April 2019, as a follow-on to the successful flight in
  September 2015 of the Chromospheric Lyman-Alpha Spectro-Polarimeter
  (CLASP). Both projects were funded by NASAs Heliophysics Technology
  and Instrument Development for Science (H-TIDeS) program to develop
  and test a technique for observing the Sun in ultraviolet light,
  and for quantifying the polarization of that light. By demonstrating
  successful measurement and interpretation of the polarization in
  hydrogen Lyman-alpha and the Mg II h and k spectral lines, the CLASP
  and CLASP2 missions are vital first steps towards routine quantitative
  characterization of the local thermal and magnetic conditions in the
  solar chromosphere. In October of 2021, we re-flew the CLASP2 payload
  with a modified observing program to further demonstrate the maturity
  of the UV spectropolarimetry techniques, and readiness for development
  into a satellite observatory. During the reflight, called CLASP2.1,
  the spectrograph slit was scanned across an active region plage to
  acquire a two-dimensional map of Stokes V/I, to demonstrate the ability
  of UV spectropolarimetry to yield chromospheric magnetic fields over
  a large area. This presentation will display preliminary results from
  the flight of CLASP2.1.

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Title: Determination of Large Scale Plasma Properties of Solar Corona
Using the X-Ray Telescope onboard Hinode: IV. Detailed Calibration
    of the Off-Axis Data
Authors: Shin, J.; Kano, R.; Sakurai, T.; Kim, Y.; Moon, Y.
2021AAS...23831307S    Altcode:
  Coronal hole is important not only in the field of solar physics but
  also of space weather because it is known as the origin of the fast
  solar wind. However, the detailed mechanism of coronal heating leading
  to the acceleration of solar wind is still unknown to us. Theoretical
  modeling of the three-dimensional coronal structures is sensitive
  to the values of plasma properties at the base of solar corona and
  thus requires in advance accurate empirical description of those
  properties. Therefore, the study on the physical conditions of solar
  plasma in the coronal holes and near the off-limb areas will give us an
  essential clue to understand the boundary conditions on the mechanism
  of heating the coronal plasma. The X-Ray Telescope (XRT) onboard Hinode
  equips the modified grazing incidence (GI) mirror whose FOV is 34 x
  34 arcmin covering the full solar disk and its neighboring regions,
  and as a result, the targets near the limb area are usually placed
  far from the center. For this reason, the imaging artefacts shown in
  the off-axis region should be calibrated carefully in order for the
  observed data to be properly interpreted. <P />We will introduce in
  this presentation the methods of how to calibrate the data taken near
  the periphery of Hinode/XRT full FOV, which include the restoration
  of the scattered light and the reduction of vignetting effect. We
  have analyzed over-exposed in-flight images during the solar flare
  to estimate the amount of scattered light inherent in the observed
  data. It is revealed the light scattered due to the roughness of GI
  mirror surface has a power-law distribution and its amount depends on
  the energy considered, which allows us to complete a PSF profile from
  the core to the scattering wing. We have also evaluated the vignetting
  effect in Hinode/XRT by analyzing the 2D distribution of effective area
  in the FOV taken from pre-launch experiments. Many interesting results
  on the optical characteristics will be introduced in our presentation.

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Title: Mapping of Solar Magnetic Fields from the Photosphere to the
    Top of the Chromosphere with CLASP2
Authors: McKenzie, D.; Ishikawa, R.; Trujillo Bueno, J.; Auchere, F.;
   del Pino Aleman, T.; Okamoto, T.; Kano, R.; Song, D.; Yoshida, M.;
   Rachmeler, L.; Kobayashi, K.; Narukage, N.; Kubo, M.; Ishikawa, S.;
   Hara, H.; Suematsu, Y.; Sakao, T.; Bethge, C.; De Pontieu, B.; Vigil,
   G.; Winebarger, A.; Alsina Ballester, E.; Belluzzi, L.; Stepan, J.;
   Asensio Ramos, A.; Carlsson, M.; Leenaarts, J.
2021AAS...23810603M    Altcode:
  Coronal heating, chromospheric heating, and the heating &amp;
  acceleration of the solar wind, are well-known problems in solar
  physics. Additionally, knowledge of the magnetic energy that
  powers solar flares and coronal mass ejections, important drivers
  of space weather, is handicapped by imperfect determination of the
  magnetic field in the sun's atmosphere. Extrapolation of photospheric
  magnetic measurements into the corona is fraught with difficulties and
  uncertainties, partly due to the vastly different plasma beta between
  the photosphere and the corona. Better results in understanding
  the coronal magnetic field should be derived from measurements of
  the magnetic field in the chromosphere. To that end, we are pursuing
  quantitative determination of the magnetic field in the chromosphere,
  where plasma beta transitions from greater than unity to less than
  unity, via ultraviolet spectropolarimetry. The CLASP2 mission, flown
  on a sounding rocket in April 2019, succeeded in measuring all four
  Stokes polarization parameters in UV spectral lines formed by singly
  ionized Magnesium and neutral Manganese. Because these ions produce
  spectral lines under different conditions, CLASP2 thus was able to
  quantify the magnetic field properties at multiple heights in the
  chromosphere simultaneously, as shown in the recent paper by Ishikawa
  et al. In this presentation we will report the findings of CLASP2,
  demonstrating the variation of magnetic fields along a track on
  the solar surface and as a function of height in the chromosphere;
  and we will illustrate what is next for the CLASP missions and the
  demonstration of UV spectropolarimetry in the solar chromosphere.

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Title: Detailed Calibration of the Off-Axis Optical Characteristics
    for the X-Ray Telescope onboard Hinode
Authors: Shin, Junho; Kano, Ryouhei; Sakurai, Takashi; Kim, Yeon-Han;
   Moon, Yong-Jae
2021EGUGA..2313004S    Altcode:
  The X-Ray Telescope (XRT) onboard the Hinode satellite has a
  specially designed Wolter type grazing-incidence (GI) optics with a
  paraboloid-hyperboloid mirror assembly to measure the solar coronal
  plasma of temperatures up to 10 MK with a resolution of about one
  arc sec. One of the main purposes of this scientific mission is to
  investigate the detailed mechanism of energy transfer processes from
  the photosphere to the upper coronal region leading to its heating and
  the solar wind acceleration. An astronomical telescope is in general
  designed such that the best-focused image of an object is achieved at or
  very close to the optical axis, and inevitably the optical performance
  deteriorates away from the on-axis position. The Sun is, however, a
  large astronomical object and thus targets near the limb of full-disk
  images are placed at the outskirt of the field of view. The design of a
  solar telescope should thus consider the uniformity of imaging quality
  over a wide FOV, and it is particularly so for X-ray telescopes whose
  targets can be in the corona high above the limb. We will explain in
  this presentation the importance of detailed calibration of the off-axis
  optical characteristics for Hinode/XRT. It have been revealed that
  the scattered light caused by the GI mirror surface has a power-law
  distribution and shows an energy dependence. We will also introduce
  the basic scheme of how the level of scattering wing is determined and
  connected to the core from the analysis of highly saturated in-flight
  data. Vignetting is another important optical characteristics for
  describing the telescope's performance, which reflects the ability to
  collect incoming light at different locations and photon energies. We
  have evaluated the vignetting effect in Hinode/XRT by analyzing
  the ground experimental data and found that the degree of vignetting
  varies linearly from the optical center and its pattern shows an energy
  dependence. Many interesting results on the calibration of Hinode/XRT
  optical characteristics will be introduced and discussed thoroughly.

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Title: Mapping solar magnetic fields from the photosphere to the
    base of the corona
Authors: Ishikawa, Ryohko; Bueno, Javier Trujillo; del Pino Alemán,
   Tanausú; Okamoto, Takenori J.; McKenzie, David E.; Auchère,
   Frédéric; Kano, Ryouhei; Song, Donguk; Yoshida, Masaki; Rachmeler,
   Laurel A.; Kobayashi, Ken; Hara, Hirohisa; Kubo, Masahito; Narukage,
   Noriyuki; Sakao, Taro; Shimizu, Toshifumi; Suematsu, Yoshinori; Bethge,
   Christian; De Pontieu, Bart; Dalda, Alberto Sainz; Vigil, Genevieve D.;
   Winebarger, Amy; Ballester, Ernest Alsina; Belluzzi, Luca; Štěpán,
   Jiří; Ramos, Andrés Asensio; Carlsson, Mats; Leenaarts, Jorrit
2021SciA....7.8406I    Altcode: 2021arXiv210301583I
  Routine ultraviolet imaging of the Sun's upper atmosphere shows the
  spectacular manifestation of solar activity; yet we remain blind to
  its main driver, the magnetic field. Here we report unprecedented
  spectropolarimetric observations of an active region plage and
  its surrounding enhanced network, showing circular polarization in
  ultraviolet (Mg II $h$ &amp; $k$ and Mn I) and visible (Fe I) lines. We
  infer the longitudinal magnetic field from the photosphere to the
  very upper chromosphere. At the top of the plage chromosphere the
  field strengths reach more than 300 gauss, strongly correlated with
  the Mg II $k$ line core intensity and the electron pressure. This
  unique mapping shows how the magnetic field couples the different
  atmospheric layers and reveals the magnetic origin of the heating in
  the plage chromosphere.

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Title: Determination of Large Scale Plasma Properties of Solar
Corona Using the X-Ray Telescope onboard Hinode: III. PSF and Image
    Calibration
Authors: Shin, Junho; Sakurai, Takashi; Kano, Ryouhei; Kim, Yeon-Han;
   Moon, Yong-Jae
2021cosp...43E1049S    Altcode:
  To theoretically model the three dimensional coronal structures is
  sensitive to the values of plasma properties at the base of solar
  corona and thus requires beforehand accurate empirical description of
  those properties. Detailed studies on the physical state of coronal
  plasma near the off-limb areas will therefore lead us to understand
  the mechanism of energy transfer processes from the photosphere to
  the upper coronal region leading to its heating and the solar wind
  acceleration. The Hinode X-Ray Telescope (XRT) has contributed to
  the progress in our understanding of coronal physics for more than a
  decade. Since the telescope was designed to observe the Sun in the wide
  field of view covering full solar disk, targets near the limb area are
  placed at the outskirt of FOV. The optical performance of the instrument
  gradually deteriorates as it goes away from the optical center and thus
  the off-axis characteristics of Hinode/XRT should be examined with care
  in order to precisely interpret the coronal plasma properties near
  the solar limb area. This presentation will explain the importance
  of accurate calibration of the optical characteristics, especially
  for the data taken in the off-axis region. Our previous research has
  shown that the light scattered by the XRT mirror surface roughness has
  a power-law distribution and also shows an energy dependence, with
  which the PSF profile from the core to the scattering wing has been
  completed. We will introduce in this study how the level of scattering
  wing can be determined quantitatively for each focal plane filter
  from in-flight data analysis. We have also evaluated the vignetting
  effect in Hinode/XRT by analyzing the distribution of effective area
  taken from MSFC/XRCF pre-launch experiment. More interesting results
  on the calibration of Hinode/XRT scattered light and the correction
  of vignetting effect will be introduced and discussed thoroughly.

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Title: Optical design of the Chromospheric LAyer Spectro-Polarimeter
    (CLASP2)
Authors: Tsuzuki, Toshihiro; Ishikawa, Ryohko; Kano, Ryouhei; Narukage,
   Noriyuki; Song, Donguk; Yoshida, Masaki; Uraguchi, Fumihiro; Okamoto,
   Takenori J.; McKenzie, David; Kobayashi, Ken; Rachmeler, Laurel;
   Auchere, Frederic; Trujillo Bueno, Javier
2020SPIE11444E..6WT    Altcode:
  Chromospheric LAyer Spectro-Polarimeter (CLASP2) was a sounding
  rocket experiment, which is a follow-up mission to the Chromospheric
  Lyman-Alpha Spectro-Polarimeter (CLASP1) in 2015. To measure the
  magnetic fields in the upper solar atmosphere in a highly quantitative
  manner, CLASP2 changes the target wavelengths from the hydrogen Ly-α
  line (121.567 nm) to Mg II lines near 280 nm. We reused the main
  structure and most of the optical components in the CLASP1 instrument,
  which reduced the turnaround time and cost. We added a magnifying
  optical system to maintain the wavelength resolution, even at the
  longer wavelength of CLASP2. Here, we describe the optical design and
  performance of the CLASP2 instrument.

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Title: Sunrise Chromospheric Infrared SpectroPolarimeter (SCIP)
for sunrise III: system design and capability
Authors: Katsukawa, Y.; del Toro Iniesta, J. C.; Solanki, S. K.;
   Kubo, M.; Hara, H.; Shimizu, T.; Oba, T.; Kawabata, Y.; Tsuzuki,
   T.; Uraguchi, F.; Nodomi, Y.; Shinoda, K.; Tamura, T.; Suematsu,
   Y.; Ishikawa, R.; Kano, R.; Matsumoto, T.; Ichimoto, K.; Nagata, S.;
   Quintero Noda, C.; Anan, T.; Orozco Suárez, D.; Balaguer Jiménez,
   M.; López Jiménez, A. C.; Cobos Carrascosa, J. P.; Feller, A.;
   Riethmueller, T.; Gandorfer, A.; Lagg, A.
2020SPIE11447E..0YK    Altcode:
  The Sunrise balloon-borne solar observatory carries a 1 m aperture
  optical telescope and provides us a unique platform to conduct
  continuous seeing-free observations at UV-visible-IR wavelengths from
  an altitude of higher than 35 km. For the next flight planned for
  2022, the post-focus instrumentation is upgraded with new spectro-
  polarimeters for the near UV (SUSI) and the near-IR (SCIP), whereas
  the imaging spectro-polarimeter Tunable Magnetograph (TuMag) is capable
  of observing multiple spectral lines within the visible wavelength. A
  new spectro-polarimeter called the Sunrise Chromospheric Infrared
  spectroPolarimeter (SCIP) is under development for observing near-IR
  wavelength ranges of around 770 nm and 850 nm. These wavelength ranges
  contain many spectral lines sensitive to solar magnetic fields and
  SCIP will be able to obtain magnetic and velocity structures in the
  solar atmosphere with a sufficient height resolution by combining
  spectro-polarimetric data of these lines. Polarimetric measurements are
  conducted using a rotating waveplate as a modulator and polarizing beam
  splitters in front of the cameras. The spatial and spectral resolutions
  are 0.2" and 2 105, respectively, and a polarimetric sensitivity of
  0.03 % (1σ) is achieved within a 10 s integration time. To detect
  minute polarization signals with good precision, we carefully designed
  the opto-mechanical system, polarization optics and modulation, and
  onboard data processing.

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Title: Detailed Calibration of the Off-Axis Optical Characteristics
    for the X-Ray Telescope onboard Hinode
Authors: Shin, Junho; Sakurai, Takashi; Kano, Ryouhei; Moon, Yong-Jae;
   Kim, Yeon-Han
2020EGUGA..2210225S    Altcode:
  The X-Ray Telescope (XRT) onboard the Hinode satellite has a
  specially designed Wolter type grazing-incidence (GI) optics with a
  paraboloid-hyperboloid mirror assembly to measure the solar coronal
  plasma of temperatures up to 10 MK with a resolution of about one
  arcsec. One of the main purposes of this scientific mission is to
  investigate the detailed mechanism of energy transfer processes from the
  photosphere to the upper coronal region leading to its heating and the
  solar wind acceleration. To theoretically model the three-dimensional
  coronal structures is sensitive to the values of plasma properties at
  the base of solar corona and thus requires beforehand accurate empirical
  description of those properties. Though the telescope has provided
  unprecedented observations of solar corona for more than a decade,
  due to a wide field of view of 34 x 34 arcmin covering the full Sun,
  the optical performance of the instrument gradually deteriorates as
  it goes away from the optical center. For this reason, the off-axis
  characteristics of Hinode/XRT should be examined with care in order
  to precisely interpret the coronal plasma properties near the solar
  limb area.This presentation will explain the importance of accurate
  calibration of the optical characteristics, especially for the data
  taken in the off-axis region. Our previous study has shown that
  the scattered light caused by the XRT mirror surface roughness has
  a power-law distribution and also shows an energy dependence, with
  which the PSF profile from the core to the scattering wing has been
  completed. We will introduce in this study how the level of scattering
  wing can be determined quantitatively for each focal plane filter from
  in-flight data analysis. We have also evaluated the vignetting effect
  in Hinode/XRT by analyzing the 2D distribution of effective area in
  the field of view taken from MSFC/XRCF pre-launch experiment. It is
  revealed that, unlike the case of Yohkoh/SXT, the degree of offset of
  an optical center is not serious and thus shows little deviation from
  rotational symmetry. Also important is that the vignetting pattern
  in XRT shows an energy dependence, which has never been considered
  before for the analyses of XRT data. More interesting results on
  the calibration of Hinode/XRT scattered light and the correction of
  vignetting effect will be introduced and discussed thoroughly.

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Title: The Chromospheric Layer Spectro-Polarimeter (CLASP2) Sounding
Rocket Mission: First Results
Authors: McKenzie, D. E.; Ishikawa, R.; Trujillo Bueno, J.; Auchere,
   F.; Rachmeler, L.; Kano, R.; Song, D.; Okamoto, J.; Kobayashi, K.;
   Yoshida, M.
2019AGUFMSH44A..06M    Altcode:
  A major challenge for heliophysics is to decipher the magnetic structure
  of the chromosphere, because of its vital role in the transport of
  energy into the corona and solar wind. Routine satellite measurements
  of the chromospheric magnetic field will dramatically improve our
  understanding of the chromosphere and its connection to the rest of
  the solar atmosphere. Before such a satellite can be considered for
  flight, we must refine the measurement techniques by exploring emission
  lines with a range of magnetic sensitivities. In 2015, CLASP achieved
  the first measurement of linear polarization produced by scattering
  processes in a far UV resonance line (hydrogen Lyman­-α), and the
  first exploration of the magnetic field (via the Hanle effect) and
  geometrical complexity in quiet regions of the chromosphere/­corona
  transition region. These measurements are a first step towards
  routine quantitative characterization of the local thermal and magnetic
  conditions in this key layer of the solar atmosphere. <P />Nonetheless,
  Lyman­-α is only one of the magnetically sensitive spectral lines in
  the UV spectrum. CLASP2 extends the capability of UV spectropolarimetry
  by acquiring ground­breaking measurements in the Mg II h and k spectral
  lines near 280 nm, whose cores form about 100 km below the Lyman-­α
  core. These lines are sensitive to a larger range of field strengths
  than Lyman­-α, through both the Hanle and Zeeman effects. CLASP2
  captures measurements of linear and circular polarization to enable
  the first determination of all 4 Stokes parameters in chromospheric
  UV radiation. Coupled with numerical modeling of the observed spectral
  line polarization (anisotropic radiation pumping with Hanle, Zeeman and
  magneto-­optical effects), CLASP2 is a pathfinder for determination
  of the magnetic field's strength and direction, as well as of the
  geometry of the plasma in the upper solar chromosphere. <P />CLASP2
  was launched from White Sands Missile Range in April 2019. In this
  presentation, we will summarize the characteristics of the CLASP2
  flight, the performance of the UV telescope and spectropolarimeter,
  and our preliminary findings.

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Title: Center-to-Limb Variation of the polarization of Mg II h &amp;
    k lines as measured by CLASP2
Authors: Rachmeler, L.; McKenzie, D. E.; Ishikawa, R.; Kano, R.;
   Trujillo Bueno, J.; Kobayashi, K.; Song, D.; Yoshida, M.; Auchere,
   F.; Okamoto, J.
2019AGUFMSH11D3380R    Altcode:
  The Chromospheric LAyer SpectroPolarimeter 2 (CLASP2) is a sounding
  rocket that was launched from White Sands Missile Range in April
  2019. CLASP2 is a reflight of the CLASP instrument, and has been
  modified to observe the polarization of the Magnesium II h &amp; k
  lines in the solar chromosphere. The instrument contains a slit-jaw
  context imager at Lyman Alpha (~121.6nm) and two spectropolarimetric
  cameras that capture Mg II h &amp; k near 280nm. A rotating polarization
  modulation unit allows us to capture the full polarization state of
  Mg II h &amp; k; the measured polarization signals are sensitive
  to the Hanle and the Zeeman magnetic effects, and magneto-optical
  effects. The center-to-limb variations (CLV) of the intensity of
  these lines has been measured, but the CLV of the polarization signals
  has only been investigated theoretically. The first flight of CLASP,
  which measured the linear polarization of the Lyman alpha line, found
  a surprising lack of CLV in the line core (Kano et al. 2017), which
  has important implications for the magnetic strength and geometrical
  complexity of the chromosphere-corona transition region (Trujillo Bueno
  et al. 2018). We present here initial results on the CLV of the Mg II
  polarization signals.

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Title: High-frequency Wave Propagation Along a Spicule Observed
    by CLASP
Authors: Yoshida, Masaki; Suematsu, Yoshinori; Ishikawa, Ryohko;
   Okamoto, Takenori J.; Kubo, Masahito; Kano, Ryouhei; Narukage,
   Noriyuki; Bando, Takamasa; Winebarger, Amy R.; Kobayashi, Ken;
   Trujillo Bueno, Javier; Auchère, Frédéric
2019ApJ...887....2Y    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) sounding
  rocket experiment, launched in 2015 September, observed the hydrogen
  Lyα line (121.6 nm) in an unprecedented high temporal cadence of
  0.3 s. CLASP performed sit-and-stare observations of the quiet Sun
  near the limb for 5 minutes with a slit perpendicular to the limb
  and successfully captured an off-limb spicule evolving along the
  slit. The Lyα line is well suited for investigating how spicules
  affect the corona because it is sensitive to higher temperatures than
  other chromospheric lines, owing to its large optical thickness. We
  found high-frequency oscillations of the Doppler velocity with periods
  of 20-50 s and low-frequency oscillation of periods of ∼240 s on
  the spicule. From a wavelet analysis of the time sequence data of
  the Doppler velocity, in the early phase of the spicule evolution,
  we found that waves with a period of ∼30 s and a velocity amplitude
  of 2-3 km s<SUP>-1</SUP> propagated upward along the spicule with a
  phase velocity of ∼470 km s<SUP>-1</SUP>. In contrast, in the later
  phase, possible downward and standing waves with smaller velocity
  amplitudes were also observed. The high-frequency waves observed in
  the early phase of the spicule evolution would be related with the
  dynamics and the formation of the spicules. Our analysis enabled us to
  identify the upward, downward, and standing waves along the spicule
  and to obtain the velocity amplitude of each wave directly from the
  Doppler velocity for the first time. We evaluated the energy flux
  by the upward-propagating waves along the spicule, and discussed the
  impact to the coronal heating.

---------------------------------------------------------
Title: Design of all-reflective space-borne 1-m aperture solar
    optical telescope
Authors: Suematsu, Y.; Hara, H.; Katsukawa, Y.; Kano, R.; Shimizu,
   T.; Ichimoto, K.
2019SPIE11180E..0RS    Altcode:
  A 1-m aperture optical telescope is planned for a future Japanese solar
  mission. The telescope is designed to provide high spatial resolution
  data of solar lower atmosphere from the photosphere to the uppermost
  chromosphere with enhanced spectroscopic and spectro-polarimetric
  capabilities covering a wide wavelength region from UV to near IR where
  many useful spectral lines and continua exist for physical diagnosis of
  the solar magnetized atmosphere. We designed an allreflective telescope
  to fulfill the scientific and engineering requirements. From a thermal
  view point, a Gregorian telescope is the most suitable. To avoid
  chromatic aberration, a tri-aspheric-mirror collimator coupling to
  the Gregorian was designed to give a diffraction-limited performance
  over the FOV by allowing a field curvature. The field curvature can
  be compensated by an off-axis Ritchey Chretien reimaging optics at an
  entrance of focal plane instrument, which has an opposite sign in the
  field curvature to the Gregorian. We also briefly studied structural
  design of all-reflective 1-m aperture solar optical telescope for the
  space solar mission.

---------------------------------------------------------
Title: The Chromospheric Layer Spectro-Polarimeter (CLASP2) Sounding
Rocket Mission: First Results
Authors: McKenzie, David Eugene; Ishikawa, Ryohko; Kano, Ryouhei;
   Rachmeler, Laurel; Trujillo Bueno, Javier; Kobayashi, Ken; Song,
   Donguk; Yoshida, Masaki; Auchere, Frederic; Okamoto, Takenori
2019AAS...23412601M    Altcode:
  A major challenge for heliophysics is to decipher the magnetic structure
  of the chromosphere, because of its vital role in the transport of
  energy into the corona and solar wind. Routine satellite measurements
  of the chromospheric magnetic field will dramatically improve our
  understanding of the chromosphere and its connection to the rest of
  the solar atmosphere. Before such a satellite can be considered for
  flight, we must refine the measurement techniques by exploring emission
  lines with a range of magnetic sensitivities. In 2015, CLASP achieved
  the first measurement of linear polarization produced by scattering
  processes in a far UV resonance line (hydrogen Lyman-α), and the
  first exploration of the magnetic field (via the Hanle effect) and
  geometrical complexity in quiet regions of the chromosphere-corona
  transition region. These measurements are a first step towards
  routine quantitative characterization of the local thermal and magnetic
  conditions in this key layer of the solar atmosphere. <P />Nonetheless,
  Lyman-α is only one of the magnetically sensitive spectral lines in the
  UV spectrum. CLASP2 extends the capability of UV spectropolarimetry by
  acquiring ground-breaking measurements in the Mg II h and k spectral
  lines near 280 nm, whose cores form about 100 km below the Lyman-α
  core. These lines are sensitive to a larger range of field strengths
  than Lyman-α, through both the Hanle and Zeeman effects. CLASP2 will
  capture measurements of linear and circular polarization to enable the
  first determination of all 4 Stokes parameters in chromospheric UV
  radiation. Coupled with numerical modeling of the observed spectral
  line polarization (anisotropic radiation pumping with Hanle, Zeeman
  and magneto-optical effects), CLASP2 is a pathfinder for determination
  of the magnetic field's strength and direction, as well as of the
  geometry of the plasma in the upper solar chromosphere. <P />CLASP2
  will launch from White Sands Missile Range in April 2019. In this
  presentation, we will summarize the characteristics of the CLASP2
  flight, the performance of the UV telescope and spectropolarimeter,
  and our preliminary findings.

---------------------------------------------------------
Title: Lyman-α imaging polarimetry with the CLASP2 sounding rocket
    mission
Authors: Kano, Ryouhei; Ishikawa, Ryohko; McKenzie, David Eugene;
   Trujillo Bueno, Javier; Song, Donguk; Yoshida, Masaki; Okamoto,
   Takenori; Rachmeler, Laurel; Kobayashi, Ken; Auchere, Frederic
2019AAS...23430216K    Altcode:
  Ultraviolet polarimetry offers a unique opportunity to explore the upper
  solar chromosphere and the transition region (TR) to the million-degree
  corona. These outer atmospheric regions play a key role in the transfer
  of mass and energy from the solar photosphere to the corona. With
  a sounding rocket experiment called the Chromospheric Lyman-Alpha
  Spectro-Polarimeter (CLASP), in September 2015 we succeeded in obtaining
  the first measurement of the linear polarization produced by scattering
  processes in the hydrogen Lyman-α line of the solar disk radiation. The
  analysis and interpretation of such spectro-polarimetric observation
  allowed us to obtain information on the geometrical complexity of
  the corrugated surface that delineates the TR, as well as on the
  magnetic field strength via the Hanle effect. At the same time, the
  CLASP slit-jaw (SJ) optics system, which is a Lyman-α filter imager
  characterized by a FWHM= 7 nm, allowed us to obtain broad-band Stokes-I
  and Q/I images over a large field of view. The obtained broad-band
  Q/I images are dominated by the scattering polarization signals of the
  Lyman-α wings, and not by the much weaker line-center signals where
  the Hanle effect operates. Recently, Alsina Ballester et al. (2019,
  ApJ, in press) showed that the scattering polarization signals of the
  Lyman-α wings are sensitive to chromospheric magnetic fields via the
  magneto-optical effects. Therefore, Lyman-α imaging polarimetry is of
  scientific interest also for magnetic-field investigations. On April
  11, 2019, we performed another sounding rocket experiment, called
  the Chromospheric LAyer Spectro-Polarimeter (CLASP2). We used the
  same instrument after significant modifications in order to obtain
  spectro-polarimetric observations of a plage and a quiet region in
  the ionized magnesium lines around 280 nm (i.e., the Mg II h &amp;
  k lines). At the same time, the CLASP2 SJ optics system allowed us to
  obtain broad-band Q/I and U/I images at the Lyman-α wavelength, in
  addition to the well-known SJ intensity images. In this presentation,
  we provide a first overview of the CLASP2 SJ data.

---------------------------------------------------------
Title: Modeling the Scattering Polarization of the Hydrogen Lyα
    Line Observed by CLASP in a Filament Channel
Authors: Štěpán, J.; Trujillo Bueno, J.; Gunár, S.; Heinzel, P.;
   del Pino Alemán, T.; Kano, R.; Ishikawa, R.; Narukage, N.; Bando,
   T.; Winebarger, A.; Kobayashi, K.; Auchère, F.
2019ASPC..526..165S    Altcode:
  The 400 arcsec spectrograph slit of CLASP crossed mainly quiet
  regions of the solar chromosphere, from the limb towards the solar
  disk center. Interestingly, in the CLASP slit-jaw images and in the
  SDO images of the He II line at 304 Å, we can identify a filament
  channel (FC) extending over more than 60 arcsec crossing the slit of
  the spectrograph. In order to interpret the peculiar spatial variation
  of the Q/I and U/I signals observed by CLASP in the hydrogen Lyα line
  (1216 Å), we perform multi-dimensional radiative transfer modeling
  in given filament models. In this contribution, we show the first
  results of the two-dimensional calculations we have carried out, with
  the aim of determining the filament thermal and magnetic structure by
  comparing the theoretical and the observed polarization signals. Our
  results suggest that the temperature gradients in the filament observed
  by CLASP are significantly larger than previously thought.

---------------------------------------------------------
Title: CLASP2: The Chromospheric LAyer Spectro-Polarimeter
Authors: McKenzie, D. E.; Ishikawa, R.; Trujillo Bueno, J.; Auchére,
   F.; Rachmeler, L. A.; Kubo, M.; Kobayashi, K.; Winebarger, A. R.;
   Bethge, C. W.; Narukage, N.; Kano, R.; Ishikawa, S.; de Pontieu,
   B.; Carlsson, M.; Yoshida, M.; Belluzzi, L.; Štěpán, J.; del Pino
   Alemán, T.; Alsina Ballester, E.; Asensio Ramos, A.
2019ASPC..526..361M    Altcode:
  The hydrogen Lyman-α line at 121.6 nm and the Mg k line at 279.5
  nm are especially relevant for deciphering the magnetic structure
  of the chromosphere since their line-center signals are formed in
  the chromosphere and transition region, with unique sensitivities to
  magnetic fields. We propose the Chromospheric LAyer Spectro-Polarimeter
  (CLASP2), to build upon the success of the first CLASP flight, which
  measured the linear polarization in H I Lyman-α. The existing CLASP
  instrument will be refitted to measure all four Stokes parameters in
  the 280 nm range, including variations due to the anisotropic radiation
  pumping, the Hanle effect, and the Zeeman effect.

---------------------------------------------------------
Title: Comparison of Scattering Polarization Signals Observed by
CLASP: Possible Indication of the Hanle Effect
Authors: Ishikawa, R.; Trujillo Bueno, J.; Uitenbroek, H.; Kubo, M.;
   Tsuneta, S.; Goto, M.; Kano, R.; Narukage, N.; Bando, T.; Katsukawa,
   Y.; Ishikawa, S.; Giono, G.; Suematsu, Y.; Hara, H.; Shimizu, T.;
   Sakao, T.; Winebarger, A.; Kobayashi, K.; Cirtain, J.; Champey, P.;
   Auchère, F.; Štěpán, J.; Belluzzi, L.; Asensio Ramos, A.; Manso
   Sainz, R.; De Pomtieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R.
2019ASPC..526..305I    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP; Kano et
  al. 2012; Kobayashi et al. 2012; Kubo et al. 2014) observed, for the
  first time, the linear polarization produced by scattering processes
  in the hydrogen Lyman-α (121.57 nm) and Si III (120.56 nm) lines of
  the solar disk radiation. The complexity of the observed scattering
  polarization (i.e., conspicuous spatial variations in Q/I and U/I
  at spatial scales of 10″-20″ and the absence of center-to- limb
  variation at the Lyman-α center; see Kano et al. 2017) motivated us
  to search for possible hints of the operation of the Hanle effect by
  comparing: (a) the Lyman-α line center signal, for which the critical
  field strength (B<SUB>H</SUB>) for the onset of the Hanle effect is
  53 G, (b) the Lyman-α wing, which is insensitive to the Hanle effect,
  and (c) the Si III line, whose B<SUB>H</SUB> = 290 G. We focus on four
  regions with different total unsigned photospheric magnetic fluxes
  (estimated from SDO/HMI observations), and compare the corresponding
  U/I spatial variations in the Lyman-α wing, Lyman-α center, and Si III
  line. The U/I signal in the Lyman-α wing shows an antisymmetric spatial
  distribution, which is caused by the presence of a bright structure in
  all the selected regions, regardless of the total unsigned photospheric
  magnetic flux. In an internetwork region, the Lyman-α center shows an
  antisymmetric spatial variation across the selected bright structure,
  but it does not show it in other more magnetized regions. In the Si III
  line, the spatial variation of U/I deviates from the above-mentioned
  antisymmetric shape as the total unsigned photospheric magnetic flux
  increases. We argue that a plausible explanation of this differential
  behavior is the operation of the Hanle effect. <P />This work, presented
  in an oral contribution at this Workshop, has been published on The
  Astrophysical Journal (Ishikawa et al. 2017).

---------------------------------------------------------
Title: Determination of Large Scale Plasma Properties of Solar Corona
Using the X-Ray Telescope onboard Hinode: II. Correction for the
    Scattered Lights
Authors: Shin, Junho; Kano, Ryouhei; Sakurai, Takashi; Kim, Yeon-Han;
   Moon, Yong-Jae
2019EGUGA..21.9726S    Altcode:
  The X-Ray Telescope (XRT) onboard Hinode, which was designed to
  observed a variety of coronal structures with temperature between 1
  and 10 MK in the range of 34x34 arc min field of view (FOV) covering
  the full solar disk, has provided solar X-ray images for more than a
  decade and contributed to the progress in our understanding of coronal
  physics. In particular, long-term observation of coronal hole regions
  covering almost one solar cycle has an important meaning not only in
  the field of solar physics but also in relation to the space weather
  because the coronal hole is known as the source of solar winds. Detailed
  study on the physical conditions of solar plasma in the coronal hole and
  also the off-limb area will give us a clue to understand the boundary
  conditions and constraints on the theoretical mechanism of heating
  the coronal plasma. An astronomical telescope is in general designed
  such that the best-focused image of an object is achieved at or very
  close to the optical axis, and inevitably the optical performance
  deteriorates away from the on-axis position. The Sun is, however, a
  large astronomical object and thus targets near the limb of full-disk
  images are placed at the outskirt of the field of view. Therefore,
  the optical design of a solar telescope should consider with care
  the uniformity of imaging quality over a wide FOV. Even after such
  a design effort, the off-axis performance of the solar telescopes
  should be characterized very carefully in order for the data away from
  the center to be properly interpreted. We have evaluated the amount
  of scattered light inherent in the Hinode/XRT data by analyzing the
  in-flight images highly saturated during the solar flare events. It is
  revealed that, like the case of Yohkoh/SXT, the light scattered due
  to the roughness of mirror surface has a power-law distribution of
  r^-2 and also shows clear energy dependence, which has enabled us to
  complete a full description of XRT PSF profile from the core to the
  scattering wing. A successful restoration of the scattered lights in
  the observed XRT images will provide us with more precise information
  on the physical quantities of solar coronal plasma in the off-limb
  regions. Many interesting results on the correction for Hinode/XRT
  scattered lights will be introduced and discussed thoroughly.

---------------------------------------------------------
Title: CLASP Constraints on the Magnetization and Geometrical
    Complexity of the Chromosphere-Corona Transition Region
Authors: Trujillo Bueno, J.; Štěpán, J.; Belluzzi, L.; Asensio
   Ramos, A.; Manso Sainz, R.; del Pino Alemán, T.; Casini, R.; Ishikawa,
   R.; Kano, R.; Winebarger, A.; Auchère, F.; Narukage, N.; Kobayashi,
   K.; Bando, T.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Giono, G.; Hara,
   H.; Suematsu, Y.; Shimizu, T.; Sakao, T.; Tsuneta, S.; Ichimoto, K.;
   Cirtain, J.; Champey, P.; De Pontieu, B.; Carlsson, M.
2018ApJ...866L..15T    Altcode: 2018arXiv180908865T
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a
  suborbital rocket experiment that on 2015 September 3 measured
  the linear polarization produced by scattering processes in the
  hydrogen Lyα line of the solar disk radiation. The line-center
  photons of this spectral line radiation mostly stem from the
  chromosphere-corona transition region (TR). These unprecedented
  spectropolarimetric observations revealed an interesting surprise,
  namely that there is practically no center-to-limb variation (CLV) in
  the Q/I line-center signals. Using an analytical model, we first show
  that the geometric complexity of the corrugated surface that delineates
  the TR has a crucial impact on the CLV of the Q/I and U/I line-center
  signals. Second, we introduce a statistical description of the solar
  atmosphere based on a 3D model derived from a state-of-the-art radiation
  magnetohydrodynamic simulation. Each realization of the statistical
  ensemble is a 3D model characterized by a given degree of magnetization
  and corrugation of the TR, and for each such realization we solve the
  full 3D radiative transfer problem taking into account the impact
  of the CLASP instrument degradation on the calculated polarization
  signals. Finally, we apply the statistical inference method presented
  in a previous paper to show that the TR of the 3D model that produces
  the best agreement with the CLASP observations has a relatively weak
  magnetic field and a relatively high degree of corrugation. We emphasize
  that a suitable way to validate or refute numerical models of the upper
  solar chromosphere is by confronting calculations and observations
  of the scattering polarization in ultraviolet lines sensitive to the
  Hanle effect.

---------------------------------------------------------
Title: A Statistical Inference Method for Interpreting the CLASP
    Observations
Authors: Štěpán, J.; Trujillo Bueno, J.; Belluzzi, L.; Asensio
   Ramos, A.; Manso Sainz, R.; del Pino Alemán, T.; Casini, R.; Kano, R.;
   Winebarger, A.; Auchère, F.; Ishikawa, R.; Narukage, N.; Kobayashi,
   K.; Bando, T.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Giono, G.; Hara,
   H.; Suematsu, Y.; Shimizu, T.; Sakao, T.; Tsuneta, S.; Ichimoto, K.;
   Cirtain, J.; Champey, P.; De Pontieu, B.; Carlsson, M.
2018ApJ...865...48S    Altcode: 2018arXiv180802725S
  On 2015 September 3, the Chromospheric Lyman-Alpha SpectroPolarimeter
  (CLASP) successfully measured the linear polarization produced by
  scattering processes in the hydrogen Lyα line of the solar disk
  radiation, revealing conspicuous spatial variations in the Q/I and U/I
  signals. Via the Hanle effect, the line-center Q/I and U/I amplitudes
  encode information on the magnetic field of the chromosphere-corona
  transition region, but they are also sensitive to the three-dimensional
  structure of this corrugated interface region. With the help of a simple
  line-formation model, here we propose a statistical inference method
  for interpreting the Lyα line-center polarization observed by CLASP.

---------------------------------------------------------
Title: Sunrise Chromospheric Infrared spectroPolarimeter (SCIP)
    for the SUNRISE balloon-borne solar observatory
Authors: Suematsu, Yoshinori; Katsukawa, Yukio; Hara, Hirohisa;
   Ichimoto, Kiyoshi; Shimizu, Toshifumi; Kubo, Masahito; Barthol,
   Peter; Riethmueller, Tino; Gandorfer, Achim; Feller, Alex; Orozco
   Suárez, David; Del Toro Iniesta, Jose Carlos; Kano, Ryouhei; Ishikawa,
   Shin-nosuke; Ishikawa, Ryohko; Tsuzuki, Toshihiro; Uraguchi, Fumihiro;
   Quintero Noda, Carlos; Tamura, Tomonori; Oba, Takayoshi; Kawabata,
   Yusuke; Nagata, Shinichi; Anan, Tetsu; Cobos Carrascosa, Juan Pedro;
   Lopez Jimenez, Antonio Carlos; Balaguer Jimenez, Maria; Solanki, Sami
2018cosp...42E3285S    Altcode:
  The SUNRISE balloon-borne solar observatory carries a 1 m aperture
  optical telescope, and allows us to perform seeing-free continuous
  observations at visible-IR wavelengths from an altitude higher than
  35 km. In the past two flights, in 2009 and 2013, observations mainly
  focused on fine structures of photospheric magnetic fields. For the
  third flight planned for 2021, we are developing a new instrument
  for conducting spectro-polarimetry of spectral lines formed over a
  larger height range in the solar atmosphere from the photosphere to
  the chromosphere. Targets of the spectro-polarimetric observation
  are (1) to determine 3D magnetic structure from the photosphere to
  the chromosphere, (2) to trace MHD waves from the photosphere to the
  chromosphere, and (3) to reveal the mechanism driving chromospheric
  jets, by measuring height- and time-dependent velocities and magnetic
  fields. To achieve these goals, a spectro-polarimeter called SCIP
  (Sunrise Chromospheric Infrared spectroPolarimeter) is designed to
  observe near-infrared spectrum lines sensitive to solar magnetic
  fields. The spatial and spectral resolutions are 0.2 arcsec and
  200,000, respectively, while 0.03% polarimetric sensitivity is
  achieved within a 10 sec integration time. The optical system employs
  an Echelle grating and off-axis aspheric mirrors to observe the two
  wavelength ranges centered at 850 nm and 770 nm simultaneously by
  two cameras. Polarimetric measurements are performed using a rotating
  waveplate and polarization beam-splitters in front of the cameras. For
  detecting minute polarization signals with good precision, we carefully
  assess the temperature dependence of polarization optics, and make
  the opto-structural design that minimizes the thermal deformation
  of the spectrograph optics. Another key technique is to attain good
  (better than 30 msec) synchronization among the rotating phase of
  the waveplate, read-out timing of cameras, and step timing of a
  slit-scanning mirror. On-board accumulation and data processing are
  also critical because we cannot store all the raw data read-out from the
  cameras. We demonstrate that we can reduce the data down to almost 10%
  with loss-less image compression and without sacrificing polarimetric
  information in the data. The SCIP instrument is developed by internal
  collaboration among Japanese institutes including Japan Aerospace
  Exploration Agency (JAXA), the Spanish Sunrise consortium, and the
  German Max Planck Institute for Solar System Research (MPS) with a
  leadership of the National Astronomical Observatory of Japan (NAOJ).

---------------------------------------------------------
Title: Current State of UV Spectro-Polarimetry and its Future
    Direction
Authors: Ishikawa, Ryohko; Sakao, Taro; Katsukawa, Yukio; Hara,
   Hirohisa; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Kubo, Masahito;
   Auchere, Frederic; De Pontieu, Bart; Winebarger, Amy; Kobayashi,
   . Ken; Kano, Ryouhei; Narukage, Noriyuki; Trujillo Bueno, Javier;
   Song, Dong-uk; Manso Sainz, Rafael; Asensio Ramos, Andres; Leenaarts,
   Jorritt; Carlsson, Mats; Bando, Takamasa; Ishikawa, Shin-nosuke;
   Tsuneta, Saku; Belluzzi, Luca; Suematsu, Yoshinori; Giono, Gabriel;
   Yoshida, Masaki; Goto, Motoshi; Del Pino Aleman, Tanausu; Stepan,
   Jiri; Okamoto, Joten; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Champey,
   Patrick; Alsina Ballester, Ernest; Casini, Roberto; McKenzie, David;
   Rachmeler, Laurel; Bethge, Christian
2018cosp...42E1564I    Altcode:
  To obtain quantitative information on the magnetic field in low beta
  regions (i.e., upper chromosphere and above) has been increasingly
  important to understand the energetic phenomena of the outer
  solar atmosphere such as flare, coronal heating, and the solar wind
  acceleration. In the UV range, there are abundant spectral lines that
  originate in the upper chromosphere and transition region. However,
  the Zeeman effect in these spectral lines does not give rise to easily
  measurable polarization signals because of the weak magnetic field
  strength and the larger Doppler broadening compared with the Zeeman
  effect. Instead, the Hanle effect in UV lines is expected to be a
  suitable diagnostic tool of the magnetic field in the upper atmospheric
  layers. To investigate the validity of UV spectro-polarimetry and
  the Hanle effect, the Chromospheric Lyman-Alpha Spectro-Polarimeter
  (CLASP), which is a NASA sounding- rocket experiment, was launched at
  White Sands in US on September 3, 2015. During its 5 minutes ballistic
  flight, it successfully performed spectro-polarimetric observations
  of the hydrogen Lyman-alpha line (121.57 nm) with an unprecedentedly
  high polarization sensitivity of 0.1% in this wavelength range. CLASP
  observed the linear polarization produced by scattering process in VUV
  lines for the first time and detected the polarization signals which
  indicate the operation of the Hanle effect. Following the success
  of CLASP, we are confident that UV spectro-polarimetry is the way
  to proceed, and we are planning the second flight of CLASP (CLASP2:
  Chromospheric LAyer SpectroPolarimeter 2). For this second flight we
  will carry out spectro-polarimetry in the Mg II h and k lines around
  280 nm, with minimum modifications of the CLASP1 instrument. The linear
  polarization in the Mg II k line is induced by scattering processes and
  the Hanle effect, being sensitive to magnetic field strengths of 5 to 50
  G. In addition, the circular polarizations in the Mg II h and k lines
  induced by the Zeeman effect can be measurable in at least plage and
  active regions. The combination of the Hanle and Zeeman effects could
  help us to more reliably infer the magnetic fields of the upper solar
  chromosphere. CLASP2 was selected for flight and is being developed for
  launch in the spring of 2019.Based on these sounding rocket experiments
  (CLASP1 and 2), we aim at establishing the strategy and refining the
  instrument concept for future space missions to explore the enigmatic
  atmospheric layers via UV spectro-polarimetry.

---------------------------------------------------------
Title: Wavefront error measurements and alignment of CLASP2 telescope
    with a dual-band pass cold mirror coated primary mirror
Authors: Yoshida, Masaki; Song, Donguk; Ishikawa, Ryoko; Kano, Ryouhei;
   Katsukawa, Yukio; Suematsu, Yoshinori; Narukage, Noriyuki; Kubo,
   Masahito; Shinoda, Kazuya; Okamoto, Takenori J.; McKenzie, David E.;
   Rachmeler, Laurel A.; Auchère, Frédéric; Trujillo Bueno, Javier
2018SPIE10699E..30Y    Altcode:
  "Chromospheric LAyer Spectro-Polarimeter (CLASP2)" is the next sounding
  rocket experiment of the "Chromospheric Lyman-Alpha Spectro-Polarimeter
  (CLASP)" that succeeded in observing for the first time the linear
  polarization spectra in the hydrogen Lyman-α line (121.6 nm) and is
  scheduled to be launched in 2019. In CLASP2, we will carry out full
  Stokes-vector spectropolarimetric observations in the Mg ii h and k
  lines near 280 nm with the spectro-polarimeter (SP), while imaging
  observations in the Lyman-α line will be conducted with the slitjaw
  optics (SJ). For the wavelength selection of CLASP2, the primary
  mirror of the telescope uses a new dual-band pass cold mirror coating
  targeting both at 121.6 nm and 280 nm. Therefore, we have to perform
  again the alignment of the telescope after the installation of the
  recoated primary mirror. Before unmounting the primary mirror from
  the telescope structure, we measured the wave-front error (WFE) of the
  telescope. The measured WFE map was consistent with what we had before
  the CLASP flight, clearly indicating that the telescope alignment has
  been maintained even after the flight. After the re-coated primary
  mirror was installed the WFE was measured, and coma aberration was
  found to be larger. Finally, the secondary mirror shim adjustments
  were carried out based on the WFE measurements. In CLASP2 telescope,
  we improved a fitting method of WFE map (applying 8th terms circular
  Zernike polynomial fitting instead of 37th terms circular Zernike
  fitting) and the improved method enables to achieve better performance
  than CLASP telescope. Indeed, WFE map obtained after the final shim
  adjustment indicated that the required specification (&lt; 5.5 μm
  RMS spot radius) that is more stringent than CLASP telescope was met.

---------------------------------------------------------
Title: Optical alignment of the high-precision UV spectro-polarimeter
    (CLASP2)
Authors: Song, Donguk; Ishikawa, Ryohko; Kano, Ryouhei; Yoshida,
   Masaki; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Shinoda, Kazuya;
   Hara, Hirohisa; Okamoto, Takenori J.; Auchère, Frédéric; McKenzie,
   David E.; Rachmeler, Laurel A.; Trujillo Bueno, Javier
2018SPIE10699E..2WS    Altcode:
  Chromospheric LAyer Spectro-Polarimeter (CLASP2) is our next sounding
  rocket experiment after the success of Chromospheric Lyman-Alpha
  Spectro-Polarimeter (CLASP1). CLASP2 is scheduled to launch in 2019,
  and aims to achieve high precision measurements (&lt; 0.1 %) of the
  linear and circular polarizations in the Mg ii h and k lines near the
  280 nm, whose line cores originate in the upper solar chromosphere. The
  CLASP2 spectro-polarimeter follows very successful design concept of
  the CLASP1 instrument with the minimal modification. A new grating was
  fabricated with the same radius of curvature as the CLASP1 grating, but
  with a different ruling density. This allows us to essentially reuse
  the CLASP1 mechanical structures and layout of the optics. However,
  because the observing wavelength of CLASP2 is twice longer than that
  of CLASP1, a magnifier optical system was newly added in front of the
  cameras to double the focal length of CLASP2 and to maintain the same
  wavelength resolution as CLASP1 (0.01 nm). Meanwhile, a careful optical
  alignment of the spectro-polarimeter is required to reach the 0.01 nm
  wavelength resolution. Therefore, we established an efficient alignment
  procedure for the CLASP2 spectro-polarimeter based on an experience
  of CLASP1. Here, we explain in detail the methods for achieving the
  optical alignment of the CLASP2 spectro-polarimeter and discuss our
  results by comparing with the performance requirements.

---------------------------------------------------------
Title: Three-minute Sunspot Oscillations Driven by Magnetic
    Reconnection in a Light Bridge
Authors: Song, Donguk; Chae, Jongchul; Kwak, Hannah; Kano, Ryouhei;
   Yurchyshyn, Vasyl; Moon, Yong-Jae; Lim, Eun-Kyung; Lee, Jeongwoo
2017ApJ...850L..33S    Altcode: 2017arXiv171106489S
  We report a different type of three-minute chromospheric oscillation
  above a sunspot in association with a small-scale impulsive event
  in a light bridge (LB). During our observations, we found a transient
  brightening in the LB. The brightening was composed of elementary bursts
  that may be a manifestation of fast repetitive magnetic reconnections
  in the LB. Interestingly, the oscillations in the nearby sunspot umbra
  were impulsively excited when the intensity of the brightening reached
  its peak. The initial period of the oscillations was about 2.3 minutes
  and then gradually increased to 3.0 minutes with time. In addition,
  we found that the amplitude of the excited oscillations was twice the
  amplitude of oscillations before the brightening. Based on our results,
  we propose that magnetic reconnection occurring in an LB can excite
  oscillations in the nearby sunspot umbra.

---------------------------------------------------------
Title: Comparison of Solar Fine Structure Observed Simultaneously
    in Lyα and Mg II h
Authors: Schmit, D.; Sukhorukov, A. V.; De Pontieu, B.; Leenaarts,
   J.; Bethge, C.; Winebarger, A.; Auchère, F.; Bando, T.; Ishikawa,
   R.; Kano, R.; Kobayashi, K.; Narukage, N.; Trujillo Bueno, J.
2017ApJ...847..141S    Altcode: 2017arXiv170900035S
  The Chromospheric Lyman Alpha Spectropolarimeter (CLASP) observed the
  Sun in H I Lyα during a suborbital rocket flight on 2015 September
  3. The Interface Region Imaging Telescope (IRIS) coordinated with the
  CLASP observations and recorded nearly simultaneous and co-spatial
  observations in the Mg II h and k lines. The Mg II h and Lyα lines
  are important transitions, energetically and diagnostically, in the
  chromosphere. The canonical solar atmosphere model predicts that these
  lines form in close proximity to each other and so we expect that the
  line profiles will exhibit similar variability. In this analysis, we
  present these coordinated observations and discuss how the two profiles
  compare over a region of quiet Sun at viewing angles that approach the
  limb. In addition to the observations, we synthesize both line profiles
  using a 3D radiation-MHD simulation. In the observations, we find that
  the peak width and the peak intensities are well correlated between the
  lines. For the simulation, we do not find the same relationship. We
  have attempted to mitigate the instrumental differences between IRIS
  and CLASP and to reproduce the instrumental factors in the synthetic
  profiles. The model indicates that formation heights of the lines
  differ in a somewhat regular fashion related to magnetic geometry. This
  variation explains to some degree the lack of correlation, observed
  and synthesized, between Mg II and Lyα. Our analysis will aid in the
  definition of future observatories that aim to link dynamics in the
  chromosphere and transition region.

---------------------------------------------------------
Title: CLASP/SJ Observations of Rapid Time Variations in the Lyα
    Emission in a Solar Active Region
Authors: Ishikawa, Shin-nosuke; Kubo, Masahito; Katsukawa, Yukio;
   Kano, Ryouhei; Narukage, Noriyuki; Ishikawa, Ryohko; Bando, Takamasa;
   Winebarger, Amy; Kobayashi, Ken; Trujillo Bueno, Javier; Auchère,
   Frédéric
2017ApJ...846..127I    Altcode:
  The Chromospheric Lyα SpectroPolarimeter (CLASP) is a sounding
  rocket experiment launched on 2015 September 3 to investigate the
  solar chromosphere and transition region. The slit-jaw (SJ) optical
  system captured Lyα images with a high time cadence of 0.6 s. From
  the CLASP/SJ observations, many variations in the solar chromosphere
  and transition region emission with a timescale of &lt;1 minute
  were discovered. In this paper, we focus on the active region within
  the SJ field of view and investigate the relationship between short
  (&lt;30 s) temporal variations in the Lyα emission and the coronal
  structures observed by Solar Dynamics Observatory/Atmospheric Imaging
  Assembly (AIA). We compare the Lyα temporal variations at the coronal
  loop footpoints observed in the AIA 211 Å (≈2 MK) and AIA 171 Å
  (≈0.6 MK) channels with those in the regions with bright Lyα features
  without a clear association with the coronal loop footpoints. We find
  more short (&lt;30 s) temporal variations in the Lyα intensity in the
  footpoint regions. Those variations did not depend on the temperature
  of the coronal loops. Therefore, the temporal variations in the Lyα
  intensity at this timescale range could be related to the heating of
  the coronal structures up to temperatures around the sensitivity peak
  of 171 Å. No signature was found to support the scenario that these
  Lyα intensity variations were related to the nanoflares. Waves or
  jets from the lower layers (lower chromosphere or photosphere) are
  possible causes for this phenomenon.

---------------------------------------------------------
Title: CLASP2: The Chromospheric LAyer Spectro-Polarimeter
Authors: Rachmeler, Laurel; E McKenzie, David; Ishikawa, Ryohko;
   Trujillo Bueno, Javier; Auchère, Frédéric; Kobayashi, Ken;
   Winebarger, Amy; Bethge, Christian; Kano, Ryouhei; Kubo, Masahito;
   Song, Donguk; Narukage, Noriyuki; Ishikawa, Shin-nosuke; De Pontieu,
   Bart; Carlsson, Mats; Yoshida, Masaki; Belluzzi, Luca; Stepan, Jiri;
   del Pino Alemná, Tanausú; Ballester, Ernest Alsina; Asensio Ramos,
   Andres
2017SPD....4811010R    Altcode:
  We present the instrument, science case, and timeline of the CLASP2
  sounding rocket mission. The successful CLASP (Chromospheric Lyman-Alpha
  Spectro-Polarimeter) sounding rocket flight in 2015 resulted in
  the first-ever linear polarization measurements of solar hydrogen
  Lyman-alpha line, which is sensitive to the Hanle effect and can be used
  to constrain the magnetic field and geometric complexity of the upper
  chromosphere. Ly-alpha is one of several upper chromospheric lines that
  contain magnetic information. In the spring of 2019, we will re-fly
  the modified CLASP telescope to measure the full Stokes profile of Mg
  II h &amp; k near 280 nm. This set of lines is sensitive to the upper
  chromospheric magnetic field via both the Hanle and the Zeeman effects.

---------------------------------------------------------
Title: CLASP2: The Chromospheric LAyer Spectro-Polarimeter
Authors: Rachmeler, Laurel A.; McKenzie, D. E.; Ishikawa, R.;
   Trujillo-Bueno, J.; Auchere, F.; Kobayashi, K.; Winebarger, A.;
   Bethge, C.; Kano, R.; Kubo, M.; Song, D.; Narukage, N.; Ishikawa, S.;
   De Pontieu, B.; Carlsson, M.; Yoshida, M.; Belluzzi, L.; Stepan, J.;
   del Pino Alemán, T.; Alsina Ballester, E.; Asensio Ramos, A.
2017shin.confE..79R    Altcode:
  We present the instrument, science case, and timeline of the CLASP2
  sounding rocket mission. The successful CLASP (Chromospheric Lyman-Alpha
  Spectro-Polarimeter) sounding rocket flight in 2015 resulted in
  the first-ever linear polarization measurements of solar hydrogen
  Lyman-alpha line, which is sensitive to the Hanle effect and can be used
  to constrain the magnetic field and geometric complexity of the upper
  chromosphere. Ly-alpha is one of several upper chromospheric lines that
  contain magnetic information. In the spring of 2019, we will re-fly
  the modified CLASP telescope to measure the full Stokes profile of Mg
  II h &amp; k near 280 nm. This set of lines is sensitive to the upper
  chromospheric magnetic field via both the Hanle and the Zeeman effects.

---------------------------------------------------------
Title: Indication of the Hanle Effect by Comparing the Scattering
    Polarization Observed by CLASP in the Lyα and Si III 120.65 nm Lines
Authors: Ishikawa, R.; Trujillo Bueno, J.; Uitenbroek, H.; Kubo, M.;
   Tsuneta, S.; Goto, M.; Kano, R.; Narukage, N.; Bando, T.; Katsukawa,
   Y.; Ishikawa, S.; Giono, G.; Suematsu, Y.; Hara, H.; Shimizu, T.;
   Sakao, T.; Winebarger, A.; Kobayashi, K.; Cirtain, J.; Champey, P.;
   Auchère, F.; Štěpán, J.; Belluzzi, L.; Asensio Ramos, A.; Manso
   Sainz, R.; De Pontieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R.
2017ApJ...841...31I    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter is a sounding
  rocket experiment that has provided the first successful measurement
  of the linear polarization produced by scattering processes in
  the hydrogen Lyα line (121.57 nm) radiation of the solar disk. In
  this paper, we report that the Si III line at 120.65 nm also shows
  scattering polarization and we compare the scattering polarization
  signals observed in the Lyα and Si III lines in order to search for
  observational signatures of the Hanle effect. We focus on four selected
  bright structures and investigate how the U/I spatial variations vary
  between the Lyα wing, the Lyα core, and the Si III line as a function
  of the total unsigned photospheric magnetic flux estimated from Solar
  Dynamics Observatory/Helioseismic and Magnetic Imager observations. In
  an internetwork region, the Lyα core shows an antisymmetric spatial
  variation across the selected bright structure, but it does not show
  it in other more magnetized regions. In the Si III line, the spatial
  variation of U/I deviates from the above-mentioned antisymmetric
  shape as the total unsigned photospheric magnetic flux increases. A
  plausible explanation of this difference is the operation of the Hanle
  effect. We argue that diagnostic techniques based on the scattering
  polarization observed simultaneously in two spectral lines with very
  different sensitivities to the Hanle effect, like Lyα and Si III,
  are of great potential interest for exploring the magnetism of the
  upper solar chromosphere and transition region.

---------------------------------------------------------
Title: Polarization Calibration of the Chromospheric Lyman-Alpha
    SpectroPolarimeter for a 0.1% Polarization Sensitivity in the VUV
Range. Part II: In-Flight Calibration
Authors: Giono, G.; Ishikawa, R.; Narukage, N.; Kano, R.; Katsukawa,
   Y.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.;
   Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J.;
   Tsuneta, S.; Shimizu, T.; Sakao, T.; Cirtain, J.; Champey, P.; Asensio
   Ramos, A.; Štěpán, J.; Belluzzi, L.; Manso Sainz, R.; De Pontieu,
   B.; Ichimoto, K.; Carlsson, M.; Casini, R.; Goto, M.
2017SoPh..292...57G    Altcode:
  The Chromospheric Lyman-Alpha SpectroPolarimeter is a sounding
  rocket instrument designed to measure for the first time the linear
  polarization of the hydrogen Lyman-α line (121.6 nm). The instrument
  was successfully launched on 3 September 2015 and observations were
  conducted at the solar disc center and close to the limb during the
  five-minutes flight. In this article, the disc center observations are
  used to provide an in-flight calibration of the instrument spurious
  polarization. The derived in-flight spurious polarization is consistent
  with the spurious polarization levels determined during the pre-flight
  calibration and a statistical analysis of the polarization fluctuations
  from solar origin is conducted to ensure a 0.014% precision on the
  spurious polarization. The combination of the pre-flight and the
  in-flight polarization calibrations provides a complete picture of
  the instrument response matrix, and a proper error transfer method
  is used to confirm the achieved polarization accuracy. As a result,
  the unprecedented 0.1% polarization accuracy of the instrument in the
  vacuum ultraviolet is ensured by the polarization calibration.

---------------------------------------------------------
Title: Discovery of Scattering Polarization in the Hydrogen Lyα
    Line of the Solar Disk Radiation
Authors: Kano, R.; Trujillo Bueno, J.; Winebarger, A.; Auchère, F.;
   Narukage, N.; Ishikawa, R.; Kobayashi, K.; Bando, T.; Katsukawa, Y.;
   Kubo, M.; Ishikawa, S.; Giono, G.; Hara, H.; Suematsu, Y.; Shimizu,
   T.; Sakao, T.; Tsuneta, S.; Ichimoto, K.; Goto, M.; Belluzzi, L.;
   Štěpán, J.; Asensio Ramos, A.; Manso Sainz, R.; Champey, P.;
   Cirtain, J.; De Pontieu, B.; Casini, R.; Carlsson, M.
2017ApJ...839L..10K    Altcode: 2017arXiv170403228K
  There is a thin transition region (TR) in the solar atmosphere where
  the temperature rises from 10,000 K in the chromosphere to millions
  of degrees in the corona. Little is known about the mechanisms that
  dominate this enigmatic region other than the magnetic field plays a
  key role. The magnetism of the TR can only be detected by polarimetric
  measurements of a few ultraviolet (UV) spectral lines, the Lyα line
  of neutral hydrogen at 121.6 nm (the strongest line of the solar UV
  spectrum) being of particular interest given its sensitivity to the
  Hanle effect (the magnetic-field-induced modification of the scattering
  line polarization). We report the discovery of linear polarization
  produced by scattering processes in the Lyα line, obtained with
  the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) rocket
  experiment. The Stokes profiles observed by CLASP in quiet regions of
  the solar disk show that the Q/I and U/I linear polarization signals are
  of the order of 0.1% in the line core and up to a few percent in the
  nearby wings, and that both have conspicuous spatial variations with
  scales of ∼10 arcsec. These observations help constrain theoretical
  models of the chromosphere-corona TR and extrapolations of the
  magnetic field from photospheric magnetograms. In fact, the observed
  spatial variation from disk to limb of polarization at the line core
  and wings already challenge the predictions from three-dimensional
  magnetohydrodynamical models of the upper solar chromosphere.

---------------------------------------------------------
Title: High-Reflectivity Coatings for a Vacuum Ultraviolet
    Spectropolarimeter
Authors: Narukage, Noriyuki; Kubo, Masahito; Ishikawa, Ryohko;
   Ishikawa, Shin-nosuke; Katsukawa, Yukio; Kobiki, Toshihiko; Giono,
   Gabriel; Kano, Ryouhei; Bando, Takamasa; Tsuneta, Saku; Auchère,
   Frédéric; Kobayashi, Ken; Winebarger, Amy; McCandless, Jim; Chen,
   Jianrong; Choi, Joanne
2017SoPh..292...40N    Altcode:
  Precise polarization measurements in the vacuum ultraviolet (VUV)
  region are expected to be a new tool for inferring the magnetic fields
  in the upper atmosphere of the Sun. High-reflectivity coatings are key
  elements to achieving high-throughput optics for precise polarization
  measurements. We fabricated three types of high-reflectivity coatings
  for a solar spectropolarimeter in the hydrogen Lyman-α (Lyα ; 121.567
  nm) region and evaluated their performance. The first high-reflectivity
  mirror coating offers a reflectivity of more than 80 % in Lyα
  optics. The second is a reflective narrow-band filter coating that has
  a peak reflectivity of 57 % in Lyα , whereas its reflectivity in the
  visible light range is lower than 1/10 of the peak reflectivity (∼5
  % on average). This coating can be used to easily realize a visible
  light rejection system, which is indispensable for a solar telescope,
  while maintaining high throughput in the Lyα line. The third is a
  high-efficiency reflective polarizing coating that almost exclusively
  reflects an s-polarized beam at its Brewster angle of 68° with a
  reflectivity of 55 %. This coating achieves both high polarizing power
  and high throughput. These coatings contributed to the high-throughput
  solar VUV spectropolarimeter called the Chromospheric Lyman-Alpha
  SpectroPolarimeter (CLASP), which was launched on 3 September, 2015.

---------------------------------------------------------
Title: Polarization Calibration of the Chromospheric Lyman-Alpha
    SpectroPolarimeter for a 0.1 % Polarization Sensitivity in the VUV
Range. Part I: Pre-flight Calibration
Authors: Giono, G.; Ishikawa, R.; Narukage, N.; Kano, R.; Katsukawa,
   Y.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.;
   Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J.
2016SoPh..291.3831G    Altcode: 2016SoPh..tmp..177G
  The Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) is a sounding
  rocket experiment designed to measure for the first time the linear
  polarization of the hydrogen Lyman-α line (121.6 nm) and requires
  a 0.1 % polarization sensitivity, which is unprecedented for a
  spectropolarimeter in the vacuum UV (VUV) spectral range.

---------------------------------------------------------
Title: Discovery of Ubiquitous Fast-Propagating Intensity Disturbances
    by the Chromospheric Lyman Alpha Spectropolarimeter (CLASP)
Authors: Kubo, M.; Katsukawa, Y.; Suematsu, Y.; Kano, R.; Bando,
   T.; Narukage, N.; Ishikawa, R.; Hara, H.; Giono, G.; Tsuneta, S.;
   Ishikawa, S.; Shimizu, T.; Sakao, T.; Winebarger, A.; Kobayashi, K.;
   Cirtain, J.; Champey, P.; Auchère, F.; Trujillo Bueno, J.; Asensio
   Ramos, A.; Štěpán, J.; Belluzzi, L.; Manso Sainz, R.; De Pontieu,
   B.; Ichimoto, K.; Carlsson, M.; Casini, R.; Goto, M.
2016ApJ...832..141K    Altcode:
  High-cadence observations by the slit-jaw (SJ) optics system of the
  sounding rocket experiment known as the Chromospheric Lyman Alpha
  Spectropolarimeter (CLASP) reveal ubiquitous intensity disturbances
  that recurrently propagate in either the chromosphere or the transition
  region or both at a speed much higher than the speed of sound. The
  CLASP/SJ instrument provides a time series of two-dimensional images
  taken with broadband filters centered on the Lyα line at a 0.6 s
  cadence. The multiple fast-propagating intensity disturbances appear in
  the quiet Sun and in an active region, and they are clearly detected in
  at least 20 areas in a field of view of 527″ × 527″ during the 5
  minute observing time. The apparent speeds of the intensity disturbances
  range from 150 to 350 km s<SUP>-1</SUP>, and they are comparable
  to the local Alfvén speed in the transition region. The intensity
  disturbances tend to propagate along bright elongated structures away
  from areas with strong photospheric magnetic fields. This suggests
  that the observed fast-propagating intensity disturbances are related
  to the magnetic canopy structures. The maximum distance traveled by
  the intensity disturbances is about 10″, and the widths are a few
  arcseconds, which are almost determined by a pixel size of 1.″03. The
  timescale of each intensity pulse is shorter than 30 s. One possible
  explanation for the fast-propagating intensity disturbances observed
  by CLASP is magnetohydrodynamic fast-mode waves.

---------------------------------------------------------
Title: Optical alignment of the Chromospheric Lyman-Alpha
    Spectro-Polarimeter using sophisticated methods to minimize activities
    under vacuum
Authors: Giono, G.; Katsukawa, Y.; Ishikawa, R.; Narukage, N.;
   Kano, R.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.;
   Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J.
2016SPIE.9905E..3DG    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a
  sounding-rocket instrument developed at the National Astronomical
  Observatory of Japan (NAOJ) as a part of an international
  collaboration. The instrument main scientific goal is to achieve
  polarization measurement of the Lyman-α line at 121.56 nm emitted from
  the solar upper-chromosphere and transition region with an unprecedented
  0.1% accuracy. The optics are composed of a Cassegrain telescope
  coated with a "cold mirror" coating optimized for UV reflection and
  a dual-channel spectrograph allowing for simultaneous observation of
  the two orthogonal states of polarization. Although the polarization
  sensitivity is the most important aspect of the instrument, the spatial
  and spectral resolutions of the instrument are also crucial to observe
  the chromospheric features and resolve the Ly-α profiles. A precise
  alignment of the optics is required to ensure the resolutions, but
  experiments under vacuum conditions are needed since Ly-α is absorbed
  by air, making the alignment experiments difficult. To bypass this
  issue, we developed methods to align the telescope and the spectrograph
  separately in visible light. We explain these methods and present
  the results for the optical alignment of the CLASP telescope and
  spectrograph. We then discuss the combined performances of both parts
  to derive the expected resolutions of the instrument, and compare them
  with the flight observations performed on September 3<SUP>rd</SUP> 2015.

---------------------------------------------------------
Title: Chromospheric LAyer SpectroPolarimeter (CLASP2)
Authors: Narukage, Noriyuki; McKenzie, David E.; Ishikawa, Ryoko;
   Trujillo-Bueno, Javier; De Pontieu, Bart; Kubo, Masahito; Ishikawa,
   Shin-nosuke; Kano, Ryouhei; Suematsu, Yoshinori; Yoshida, Masaki;
   Rachmeler, Laurel A.; Kobayashi, Ken; Cirtain, Jonathan W.; Winebarger,
   Amy R.; Asensio Ramos, Andres; del Pino Aleman, Tanausu; Štępán,
   Jiri; Belluzzi, Luca; Larruquert, Juan Ignacio; Auchère, Frédéric;
   Leenaarts, Jorrit; Carlsson, Mattias J. L.
2016SPIE.9905E..08N    Altcode:
  The sounding rocket Chromospheric Lyman-Alpha SpectroPolarimeter
  (CLASP) was launched on September 3rd, 2015, and successfully detected
  (with a polarization accuracy of 0.1 %) the linear polarization signals
  (Stokes Q and U) that scattering processes were predicted to produce
  in the hydrogen Lyman-alpha line (Lyα 121.567 nm). Via the Hanle
  effect, this unique data set may provide novel information about the
  magnetic structure and energetics in the upper solar chromosphere. The
  CLASP instrument was safely recovered without any damage and we have
  recently proposed to dedicate its second flight to observe the four
  Stokes profiles in the spectral region of the Mg II h and k lines
  around 280 nm; in these lines the polarization signals result from
  scattering processes and the Hanle and Zeeman effects. Here we describe
  the modifications needed to develop this new instrument called the
  "Chromospheric LAyer SpectroPolarimeter" (CLASP2).

---------------------------------------------------------
Title: Spectro-polarimetric observation in UV with CLASP to probe
    the chromosphere and transition region
Authors: Kano, Ryouhei; Ishikawa, Ryohko; Winebarger, Amy R.; Auchère,
   Frédéric; Trujillo Bueno, Javier; Narukage, Noriyuki; Kobayashi,
   Ken; Bando, Takamasa; Katsukawa, Yukio; Kubo, Masahito; Ishikawa,
   Shin-Nosuke; Giono, Gabriel; Hara, Hirohisa; Suematsu, Yoshinori;
   Shimizu, Toshifumi; Sakao, Taro; Tsuneta, Saku; Ichimoto, Kiyoshi;
   Goto, Motoshi; Cirtain, Jonathan W.; De Pontieu, Bart; Casini, Roberto;
   Manso Sainz, Rafael; Asensio Ramos, Andres; Stepan, Jiri; Belluzzi,
   Luca; Carlsson, Mats
2016SPD....4710107K    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a NASA
  sounding-rocket experiment that was performed in White Sands in
  the US on September 3, 2015. During its 5-minute ballistic flight,
  CLASP successfully made the first spectro-polarimetric observation in
  the Lyman-alpha line (121.57 nm) originating in the chromosphere and
  transition region. Since the Lyman-alpha polarization is sensitive
  to magnetic field of 10-100 G by the Hanle effect, we aim to infer
  the magnetic field information in such upper solar atmosphere with
  this experiment.The obtained CLASP data showed that the Lyman-alpha
  scattering polarization is about a few percent in the wings and
  the order of 0.1% in the core near the solar limb, as it had been
  theoretically predicted, and that both polarization signals have a
  conspicuous spatio-temporal variability. CLASP also observed another
  upper-chromospheric line, Si III (120.65 nm), whose critical field
  strength for the Hanle effect is 290 G, and showed a measurable
  scattering polarization of a few % in this line. The polarization
  properties of the Si III line could facilitate the interpretation of
  the scattering polarization observed in the Lyman-alpha line.In this
  presentation, we would like to show how the upper chromosphere and
  transition region are seen in the polarization of these UV lines and
  discuss the possible source of these complicated polarization signals.

---------------------------------------------------------
Title: Development of a Precise Polarization Modulator for UV
    Spectropolarimetry
Authors: Ishikawa, S.; Shimizu, T.; Kano, R.; Bando, T.; Ishikawa,
   R.; Giono, G.; Tsuneta, S.; Nakayama, S.; Tajima, T.
2015SoPh..290.3081I    Altcode: 2015arXiv150905716I; 2015SoPh..tmp..120I
  We developed a polarization modulation unit (PMU) to rotate a
  waveplate continuously in order to observe solar magnetic fields
  by spectropolarimetry. The non-uniformity of the PMU rotation may
  cause errors in the measurement of the degree of linear polarization
  (scale error) and its angle (crosstalk between Stokes-Q and -U ),
  although it does not cause an artificial linear polarization signal
  (spurious polarization). We rotated a waveplate with the PMU to obtain
  a polarization modulation curve and estimated the scale error and
  crosstalk caused by the rotation non-uniformity. The estimated scale
  error and crosstalk were &lt;0.01 % for both. This PMU will be used as
  a waveplate motor for the Chromospheric Lyman-Alpha SpectroPolarimeter
  (CLASP) rocket experiment. We confirm that the PMU performs and
  functions sufficiently well for CLASP.

---------------------------------------------------------
Title: CLASP: A UV Spectropolarimeter on a Sounding Rocket for
    Probing theChromosphere-Corona Transition Regio
Authors: Ishikawa, Ryohko; Kano, Ryouhei; Winebarger, Amy; Auchere,
   Frederic; Trujillo Bueno, Javier; Bando, Takamasa; Narukage,
   Noriyuki; Kobayashi, Ken; Katsukawa, Yukio; Kubo, Masahito; Ishikawa,
   Shin-nosuke; Giono, Gabriel; Tsuneta, Saku; Hara, Hirohisa; Suematsu,
   Yoshinori; Shimizu, Toshifumi; Sakao, Taro; Ichimoto, Kiyoshi;
   Cirtain, Jonathan; De Pontieu, Bart; Casini, Roberto; Manso Sainz,
   Rafael; Asensio Ramos, Andres; Stepan, Jiri; Belluzzi, Luca
2015IAUGA..2254536I    Altcode:
  The wish to understand the energetic phenomena of the outer solar
  atmosphere makes it increasingly important to achieve quantitative
  information on the magnetic field in the chromosphere-corona
  transition region. To this end, we need to measure and model the
  linear polarization produced by scattering processes and the Hanle
  effect in strong UV resonance lines, such as the hydrogen Lyman-alpha
  line. A team consisting of Japan, USA, Spain, France, and Norway has
  been developing a sounding rocket experiment called the Chromospheric
  Lyman-alpha Spectro-Polarimeter (CLASP). The aim is to detect the
  scattering polarization produced by anisotropic radiation pumping in
  the hydrogen Lyman-alpha line (121.6 nm), and via the Hanle effect to
  try to constrain the magnetic field vector in the upper chromosphere
  and transition region. In this talk, we will present an overview
  of our CLASP mission, its scientific objectives, ground tests made,
  and the latest information on the launch planned for the Summer of 2015.

---------------------------------------------------------
Title: Strategy for Realizing High-Precision VUV Spectro-Polarimeter
Authors: Ishikawa, R.; Narukage, N.; Kubo, M.; Ishikawa, S.; Kano,
   R.; Tsuneta, S.
2014SoPh..289.4727I    Altcode: 2014SoPh..tmp..116I
  Spectro-polarimetric observations in the vacuum ultraviolet (VUV)
  range are currently the only means to measure magnetic fields in the
  upper chromosphere and transition region of the solar atmosphere. The
  Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) aims to measure
  linear polarization at the hydrogen Lyman-α line (121.6 nm). This
  measurement requires a polarization sensitivity better than 0.1 %,
  which is unprecedented in the VUV range. We here present a strategy with
  which to realize such high-precision spectro-polarimetry. This involves
  the optimization of instrument design, testing of optical components,
  extensive analyses of polarization errors, polarization calibration
  of the instrument, and calibration with onboard data. We expect that
  this strategy will aid the development of other advanced high-precision
  polarimeters in the UV as well as in other wavelength ranges.

---------------------------------------------------------
Title: Precision VUV Spectro-Polarimetry for Solar Chromospheric
    Magnetic Field Measurements
Authors: Ishikawa, R.; Bando, T.; Hara, H.; Ishikawa, S.; Kano, R.;
   Kubo, M.; Katsukawa, Y.; Kobiki, T.; Narukage, N.; Suematsu, Y.;
   Tsuneta, S.; Aoki, K.; Miyagawa, K.; Ichimoto, K.; Kobayashi, K.;
   Auchère, F.; Clasp Team
2014ASPC..489..319I    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a VUV
  spectro-polarimeter optimized for measuring the linear polarization
  of the Lyman-α line (121.6 nm) to be launched in 2015 with NASA's
  sounding rocket (Ishikawa et al. 2011; Narukage et al. 2011; Kano et
  al. 2012; Kobayashi et al. 2012). With this experiment, we aim to (1)
  observe the scattering polarization in the Lyman-α line, (2) detect
  the Hanle effect, and (3) assess the magnetic fields in the upper
  chromosphere and transition region for the first time. The polarization
  measurement error consists of scale error δ a (error in amplitude
  of linear polarization), azimuth error Δφ (error in the direction
  of linear polarization), and spurious polarization ɛ (false linear
  polarization signals). The error ɛ should be suppressed below 0.1%
  in the Lyman-α core (121.567 nm ±0.02 nm), and 0.5% in the Lyman-α
  wing (121.567 nm ±0.05 nm), based on our scientific requirements shown
  in Table 2 of Kubo et al. (2014). From scientific justification, we
  adopt Δ φ&lt;2° and δ a&lt;10% as the instrument requirements. The
  spectro-polarimeter features a continuously rotating MgF<SUB>2</SUB>
  waveplate (Ishikawa et al. 2013), a dual-beam spectrograph with a
  spherical grating working also as a beam splitter, and two polarization
  analyzers (Bridou et al. 2011), which are mounted at 90 degree from
  each other to measure two orthogonal polarization simultaneously. For
  the optical layout of the CLASP instrument, see Figure 3 in Kubo et
  al. (2014). Considering the continuous rotation of the half-waveplate,
  the modulation efficiency is 0.64 both for Stokes Q and U. All the raw
  data are returned and demodulation (successive addition or subtraction
  of images) is done on the ground. <P />We control the CLASP polarization
  performance in the following three steps. First, we evaluate the
  throughput and polarization properties of each optical component in
  the Lyman-α line, using the Ultraviolet Synchrotron ORbital Radiation
  Facility (UVSOR) at the Institute for Molecular Science. The second
  step is polarization calibration of the spectro-polarimeter after
  alignment. Since the spurious polarization caused by the axisymmetric
  telescope is estimated to be negligibly small because of the symmetry
  (Ishikawa et al. 2014), we do not perform end-to-end polarization
  calibration. As the final step, before the scientific observation near
  the limb, we make a short observation at the Sun center and verify
  the polarization sensitivity, because the scattering polarization
  is expected to be close to zero at the Sun center due to symmetric
  geometry. In order to clarify whether we will be able to achieve the
  required polarization sensitivity and accuracy via these steps, we
  exercise polarization error budget, by investigating all the possible
  causes and their magnitudes of polarization errors, all of which are not
  necessarily verified by the polarization calibration. Based on these
  error budgets, we conclude that a polarization sensitivity of 0.1% in
  the line core, δ a&lt;10% and Δ φ&lt;2° can be achieved combined
  with the polarization calibration of the spectro-polarimeter and the
  onboard calibration at the Sun center(refer to Ishikawa et al. 2014,
  for the detail). <P />We are currently conducting verification tests
  of the flight components and development of the UV light source for
  the polarization calibration. From 2014 spring, we will begin the
  integration, alignment, and calibration. We will update the error
  budgets throughout the course of these tests.

---------------------------------------------------------
Title: A Sounding Rocket Experiment for the Chromospheric Lyman-Alpha
    Spectro-Polarimeter (CLASP)
Authors: Kubo, M.; Kano, R.; Kobayashi, K.; Bando, T.; Narukage, N.;
   Ishikawa, R.; Tsuneta, S.; Katsukawa, Y.; Ishikawa, S.; Suematsu, Y.;
   Hara, H.; Shimizu, T.; Sakao, T.; Ichimoto, K.; Goto, M.; Holloway,
   T.; Winebarger, A.; Cirtain, J.; De Pontieu, B.; Casini, R.; Auchère,
   F.; Trujillo Bueno, J.; Manso Sainz, R.; Belluzzi, L.; Asensio Ramos,
   A.; Štěpán, J.; Carlsson, M.
2014ASPC..489..307K    Altcode:
  A sounding-rocket experiment called the Chromospheric Lyman-Alpha
  Spectro-Polarimeter (CLASP) is presently under development to measure
  the linear polarization profiles in the hydrogen Lyman-alpha (Lyα)
  line at 121.567 nm. CLASP is a vacuum-UV (VUV) spectropolarimeter to aim
  for first detection of the linear polarizations caused by scattering
  processes and the Hanle effect in the Lyα line with high accuracy
  (0.1%). This is a fist step for exploration of magnetic fields in
  the upper chromosphere and transition region of the Sun. Accurate
  measurements of the linear polarization signals caused by scattering
  processes and the Hanle effect in strong UV lines like Lyα are
  essential to explore with future solar telescopes the strength
  and structures of the magnetic field in the upper chromosphere and
  transition region of the Sun. The CLASP proposal has been accepted by
  NASA in 2012, and the flight is planned in 2015.

---------------------------------------------------------
Title: Large aperture solar optical telescope and instruments for
    the SOLAR-C mission
Authors: Suematsu, Y.; Katsukawa, Y.; Hara, H.; Kano, R.; Shimizu,
   T.; Ichimoto, K.
2014SPIE.9143E..1PS    Altcode:
  A large aperture solar optical telescope and its instruments
  for the SOLAR-C mission are under study to provide the critical
  physical parameters in the lower solar atmosphere and to resolve the
  mechanism of magnetic dynamic events happening there and in the upper
  atmosphere as well. For the precise magnetic field measurements and
  high angular resolution in wide wavelength region, covering FOV of 3
  arcmin x3 arcmin, an entrance aperture of 1.4 m Gregorian telescope is
  proposed. Filtergraphs are designed to realize high resolution imaging
  and pseudo 2D spectro-polarimetry in several magnetic sensitive lines of
  both photosphere and chromosphere. A full stokes polarimetry is carried
  out at three magnetic sensitive lines with a four-slit spectrograph
  of 2D image scanning mechanism. We present a progress in optical and
  structural design of SOLAR-C large aperture optical telescope and its
  observing instruments which fulfill science requirements.

---------------------------------------------------------
Title: Current progress of optical alignment procedure of CLASP's
    Lyman-alpha polarimetry instrument
Authors: Giono, G.; Ishikawa, R.; Katsukawa, Y.; Bando, T.; Kano, R.;
   Suematsu, Y.; Narukage, N.; Sakao, Taro; Kobayashi, K.; Auchère, F.
2014SPIE.9144E..3EG    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a
  sounding-rocket instrument currently under development at the
  National Astronomical Observatory of Japan (NAOJ) as a part of an
  international collaboration. CLASP's optics are composed of a Cassegrain
  telescope and a spectro-polarimeter which are designed to achieve an
  unprecedentedly accurate polarization measurement of the Ly-α line
  at 121.6nm emitted from the solar upper-chromosphere and transition
  region. CLASP's first flight is scheduled for August 2015. Reaching
  such accuracy requires a careful alignment of the optical elements
  to optimize the image quality at 121.6 nm. However Ly-α is absorbed
  by air and therefore the optics alignment has to be done under vacuum
  condition which makes any experiment difficult. To bypass this issue,
  we proposed to align the telescope and the spectrograph separately
  in visible light. Hence we present our alignment procedure for both
  telescope and spectro-polarimeter. We will explain details about the
  telescope preliminary alignment before mirrors coating, which was done
  in April 2014, present the telescope combined optical performance
  and compare them to CLASP tolerance. Then we will present details
  about an experiment designed to confirm our alignment procedure for
  the CLASP spectro-polarimeter. We will discuss the resulting image
  quality achieved during this experiment and the lessons learned.

---------------------------------------------------------
Title: Coronal-Temperature-Diagnostic Capability of the Hinode/ X-Ray
    Telescope Based on Self-consistent Calibration. II. Calibration with
    On-Orbit Data
Authors: Narukage, N.; Sakao, T.; Kano, R.; Shimojo, M.; Winebarger,
   A.; Weber, M.; Reeves, K. K.
2014SoPh..289.1029N    Altcode: 2013arXiv1307.4489N
  The X-Ray Telescope (XRT) onboard the Hinode satellite is an
  X-ray imager that observes the solar corona with the capability of
  diagnosing coronal temperatures from less than 1 MK to more than
  10 MK. To make full use of this capability, Narukage et al. (Solar
  Phys.269, 169, 2011) determined the thickness of each of the X-ray
  focal-plane analysis filters based on calibration measurements
  from the ground-based end-to-end test. However, in their paper,
  the calibration of the thicker filters for observations of active
  regions and flares, namely the med-Be, med-Al, thick-Al and thick-Be
  filters, was insufficient due to the insufficient X-ray flux used in
  the measurements. In this work, we recalibrate those thicker filters
  using quiescent active region data taken with multiple filters of
  XRT. On the basis of our updated calibration results, we present the
  revised coronal-temperature-diagnostic capability of XRT.

---------------------------------------------------------
Title: Photospheric Properties of Warm EUV Loops and Hot X-Ray Loops
Authors: Kano, R.; Ueda, K.; Tsuneta, S.
2014ApJ...782L..32K    Altcode:
  We investigate the photospheric properties (vector magnetic fields and
  horizontal velocity) of a well-developed active region, NOAA AR 10978,
  using the Hinode Solar Optical Telescope specifically to determine
  what gives rise to the temperature difference between "warm loops"
  (1-2 MK), which are coronal loops observed in EUV wavelengths, and
  "hot loops" (&gt;3 MK), coronal loops observed in X-rays. We found
  that outside sunspots, the magnetic filling factor in the solar network
  varies with location and is anti-correlated with the horizontal random
  velocity. If we accept that the observed magnetic features consist of
  unresolved magnetic flux tubes, this anti-correlation can be explained
  by the ensemble average of flux-tube motion driven by small-scale random
  flows. The observed data are consistent with a flux tube width of ~77
  km and horizontal flow at ~2.6 km s<SUP>-1</SUP> with a spatial scale
  of ~120 km. We also found that outside sunspots, there is no significant
  difference between warm and hot loops either in the magnetic properties
  (except for the inclination) or in the horizontal random velocity
  at their footpoints, which are identified with the Hinode X-Ray
  Telescope and the Transition Region and Coronal Explorer. The energy
  flux injected into the coronal loops by the observed photospheric
  motion of the magnetic fields is estimated to be 2 × 10<SUP>6</SUP>
  erg s<SUP>-1</SUP> cm<SUP>-2</SUP>, which is the same for both warm and
  hot loops. This suggests that coronal properties (e.g., loop length)
  play a more important role in giving rise to temperature differences
  of active-region coronal loops than photospheric parameters.

---------------------------------------------------------
Title: Chromospheric Lyman-alpha spectro-polarimeter (CLASP)
Authors: Kano, Ryouhei; Katsukawa, Yukio; Kubo, Masahito; Auchere,
   Frederic; Ishikawa, Ryohko; Kobayashi, Ken; Narukage, Noriyuki;
   Trujillo Bueno, Javier; Bando, Takamasa; Ishikawa, Shin-nosuke
2014cosp...40E1383K    Altcode:
  In the solar chromosphere, magneto-hydrodynamic waves and super-sonic
  jets ubiquitously happen as revealed by the Japanese solar satellite
  Hinode. Now, we understand that the solar chromosphere is not a simple
  intermediate layer smoothly connecting the photosphere and corona,
  but a site where those dynamics may play an important role in the
  chromospheric and coronal heating. Such discoveries imply that the
  next frontier in solar physics lies in simultaneous observations
  between the dynamics and magnetic structures in the chromosphere and
  transition region, where the gas-dominant photosphere changes to the
  magnetic-dominant corona. Therefore, we promote the Chromospheric
  Lyman-Alpha SpectroPolarimeter (CLASP), which is a NASA's sounding
  rocket experiment scheduled in 2015 for aiming to infer the magnetic
  field information in the solar chromosphere and transition region. CLASP
  makes precise measurement (0.1%) of the polarization profile of the
  Lyman-alpha line, and aims to make the first ever measurement of the
  Hanle effect polarization caused by magnetic fields in the upper solar
  atmosphere. It is also a pathfinder to establish a new measurement
  tool for chromospheric and transition-region magnetic fields, and to
  make progress on chromospheric studies in future missions.

---------------------------------------------------------
Title: UV spectropolarimeter design for precise polarization
    measurement and its application to the CLASP for exploration of
    magnetic fields in solar atmosphere
Authors: Narukage, Noriyuki; Katsukawa, Yukio; Hara, Hirohisa; Kubo,
   Masahito; Auchere, Frederic; Ishikawa, Ryohko; Kano, Ryouhei; Bando,
   Takamasa; Ishikawa, Shin-nosuke; Suematsu, Yoshinori; Tsuneta, Saku
2014cosp...40E2232N    Altcode:
  In order to measure the magnetic field in the region where the
  hot plasma from 10 (4) K to 10 (6) K is occupied, e.g., for solar
  atmosphere, the polarimetric measurements in ultra violet (UV)
  with 0.1% accuracy are required. In this paper, we propose a new
  UV spectropolarimeter design with 0.1% sensitivity in polarization
  measurement. This spectropolarimeter has two devices for the 0.1%
  accuracy. First, all optical components except the waveplate are the
  reflective type ones that can be equipped with the high reflectivity
  coating for the high throughput. Secondly, it equips the optically
  symmetric dual channels to measure the orthogonal linear polarization
  state simultaneously, using a concave diffraction grating as both the
  spectral dispersion element and the beam splitter. These two devices
  make the spurious polarizations caused by the photon noise, by the
  intensity variation of the observation target, and, by the instrument
  itself, enough small to achieve the 0.1% accuracy in polarization
  measurement. The spectropolarimeter thus designed is currently under
  fabrication for the sounding rocket project of Chromospheric Lyman-Alpha
  SpectroPolarimeter (CLASP) that aims at the direct measurement of the
  magnetic fields in solar atmosphere with Lyman-alpha line (121.6 nm)
  for the first time.

---------------------------------------------------------
Title: Chromospheric Lyman Alpha SpectroPolarimeter: CLASP
Authors: Kobayashi, Ken; Kano, R.; Trujillo Bueno, J.; Winebarger,
   A. R.; Cirtain, J. W.; Bando, T.; De Pontieu, B.; Ishikawa, R.;
   Katsukawa, Y.; Kubo, M.; Narukage, N.; Sakao, T.; Tsuneta, S.;
   Auchère, F.; Asensio Ramos, A.; Belluzzi, L.; Carlsson, M.; Casini,
   R.; Hara, H.; Ichimoto, K.; Manso Sainz, R.; Shimizu, T.; Stepan,
   J.; Suematsu, Y.; Holloway, T.
2013SPD....44..142K    Altcode:
  The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a VUV
  spectropolarimeter optimized for measuring the linear polarization of
  the Lyman-alpha line (121.6 nm). The Lyman-alpha line is predicted to
  show linear polarization caused by atomic scattering in the chromosphere
  and modified by the magnetic field through the Hanle effect. The
  Hanle effect is sensitive to weaker magnetic fields than Zeeman
  effect, and is not canceled by opposing fields, making it sensitive
  to tangled or unresolved magnetic field structures. These factors make
  the Hanle effect a valuable tool for probing the magnetic field in the
  chromosphere above the quiet sun. To meet this goal, CLASP is designed
  to measure linear polarization with 0.1% polarization sensitivity
  at 0.01 nm spectral resolution and 10" spatial resolution. CLASP is
  scheduled to be launched in 2015.

---------------------------------------------------------
Title: Chromospheric Lyman-alpha spectro-polarimeter (CLASP)
Authors: Kano, Ryouhei; Bando, Takamasa; Narukage, Noriyuki; Ishikawa,
   Ryoko; Tsuneta, Saku; Katsukawa, Yukio; Kubo, Masahito; Ishikawa,
   Shin-nosuke; Hara, Hirohisa; Shimizu, Toshifumi; Suematsu, Yoshinori;
   Ichimoto, Kiyoshi; Sakao, Taro; Goto, Motoshi; Kato, Yoshiaki; Imada,
   Shinsuke; Kobayashi, Ken; Holloway, Todd; Winebarger, Amy; Cirtain,
   Jonathan; De Pontieu, Bart; Casini, Roberto; Trujillo Bueno, Javier;
   Štepán, Jiří; Manso Sainz, Rafael; Belluzzi, Luca; Asensio Ramos,
   Andres; Auchère, Frédéric; Carlsson, Mats
2012SPIE.8443E..4FK    Altcode:
  One of the biggest challenges in heliophysics is to decipher the
  magnetic structure of the solar chromosphere. The importance of
  measuring the chromospheric magnetic field is due to both the key role
  the chromosphere plays in energizing and structuring the outer solar
  atmosphere and the inability of extrapolation of photospheric fields to
  adequately describe this key boundary region. Over the last few years,
  significant progress has been made in the spectral line formation
  of UV lines as well as the MHD modeling of the solar atmosphere. It
  is found that the Hanle effect in the Lyman-alpha line (121.567 nm)
  is a most promising diagnostic tool for weaker magnetic fields in
  the chromosphere and transition region. Based on this groundbreaking
  research, we propose the Chromospheric Lyman-Alpha Spectro-Polarimeter
  (CLASP) to NASA as a sounding rocket experiment, for making the first
  measurement of the linear polarization produced by scattering processes
  and the Hanle effect in the Lyman-alpha line (121.567 nm), and making
  the first exploration of the magnetic field in the upper chromosphere
  and transition region of the Sun. The CLASP instrument consists
  of a Cassegrain telescope, a rotating 1/2-wave plate, a dual-beam
  spectrograph assembly with a grating working as a beam splitter, and
  an identical pair of reflective polarization analyzers each equipped
  with a CCD camera. We propose to launch CLASP in December 2014.

---------------------------------------------------------
Title: The Chromospheric Lyman-Alpha SpectroPolarimeter: CLASP
Authors: Kobayashi, K.; Kano, R.; Trujillo-Bueno, J.; Asensio Ramos,
   A.; Bando, T.; Belluzzi, L.; Carlsson, M.; De Pontieu, R. C. B.; Hara,
   H.; Ichimoto, K.; Ishikawa, R.; Katsukawa, Y.; Kubo, M.; Manso Sainz,
   R.; Narukage, N.; Sakao, T.; Stepan, J.; Suematsu, Y.; Tsuneta, S.;
   Watanabe, H.; Winebarger, A.
2012ASPC..456..233K    Altcode:
  The magnetic field plays a crucial role in the chromosphere and the
  transition region, and our poor empirical knowledge of the magnetic
  field in the upper chromosphere and transition region is a major
  impediment to advancing the understanding of the solar atmosphere. The
  Hanle effect promises to be a valuable alternative to Zeeman effect
  as a method of measuring the magnetic field in the chromosphere and
  transition region; it is sensitive to weaker magnetic fields, and
  also sensitive to tangled, unresolved field structures. <P />CLASP
  is a sounding rocket experiment that aims to observe the Hanle effect
  polarization of the Lyman α (1215.67Å) line in the solar chromosphere
  and transition region, and prove the usefulness of this technique in
  placing constraints on the magnetic field strength and orientation
  in the low plasma-β region of the solar atmosphere. The Ly-α line
  has been chosen because it is a chromospheric/transition-region line,
  and because the Hanle effect polarization of this line is predicted to
  be sensitive to 10-250 Gauss, encompassing the range of interest. The
  CLASP instrument is designed to measure linear polarization in the
  Ly-α line with a polarization sensitivity of 0.1%. The instrument is
  currently funded for development. The optical design of the instrument
  has been finalized, and an extensive series of component-level tests
  are underway to validate the design.

---------------------------------------------------------
Title: Nanoflare Evidence from Analysis of the X-Ray Variability of
    an Active Region Observed with Hinode/XRT
Authors: Terzo, S.; Reale, F.; Miceli, M.; Kano, R.; Tsuneta, S.;
   Klimchuk, J. A.
2012ASPC..455..245T    Altcode: 2012arXiv1201.5482T
  The heating of the solar corona is one of the big questions in
  astrophysics. Rapid pulses called nanoflares are among the best
  candidate mechanisms. The analysis of the time variability of coronal
  X-ray emission is potentially a very useful tool to detect impulsive
  events. We analyze the small-scale variability of a solar active
  region in a high cadence Hinode/XRT observation. The dataset allows
  us to detect very small deviations of emission fluctuations from the
  distribution expected for a constant rate. We discuss the deviations
  in the light of the pulsed-heating scenario.

---------------------------------------------------------
Title: Thermal Properties of a Solar Coronal Cavity Observed with
    the X-Ray Telescope on Hinode
Authors: Reeves, Katharine K.; Gibson, Sarah E.; Kucera, Therese A.;
   Hudson, Hugh S.; Kano, Ryouhei
2012ApJ...746..146R    Altcode:
  Coronal cavities are voids in coronal emission often observed above
  high latitude filament channels. Sometimes, these cavities have areas of
  bright X-ray emission in their centers. In this study, we use data from
  the X-ray Telescope (XRT) on the Hinode satellite to examine the thermal
  emission properties of a cavity observed during 2008 July that contains
  bright X-ray emission in its center. Using ratios of XRT filters, we
  find evidence for elevated temperatures in the cavity center. The area
  of elevated temperature evolves from a ring-shaped structure at the
  beginning of the observation, to an elongated structure two days later,
  finally appearing as a compact round source four days after the initial
  observation. We use a morphological model to fit the cavity emission,
  and find that a uniform structure running through the cavity does not
  fit the observations well. Instead, the observations are reproduced
  by modeling several short cylindrical cavity "cores" with different
  parameters on different days. These changing core parameters may be
  due to some observed activity heating different parts of the cavity
  core at different times. We find that core temperatures of 1.75 MK,
  1.7 MK, and 2.0 MK (for July 19, July 21, and July 23, respectively)
  in the model lead to structures that are consistent with the data,
  and that line-of-sight effects serve to lower the effective temperature
  derived from the filter ratio.

---------------------------------------------------------
Title: Ly-alpha polarimeter design for CLASP rocket experiment
Authors: Kubo, M.; Watanabe, H.; Narukage, N.; Ishikawa, R.; Bando,
   T.; Kano, R.; Tsuneta, S.; Kobayashi, K.; Ichimoto, K.; Trujillo Bueno,
   J.; Song, D.
2011AGUFM.P11F1627K    Altcode:
  A sounding-rocket program called the Chromospheric Lyman-Alpha
  Spectro-Polarimeter (CLASP) is proposed to be launched in the Summer
  of 2014. CLASP will observe the upper solar chromosphere in Ly-alpha
  (121.567 nm), aiming to detect the linear polarization signal produced
  by scattering processes and the Hanle effect for the first time. The
  CLASP needs a rotating half-waveplate and a polarization analyzer
  working at the Ly-alpha wavelength to measure the linear polarization
  signal. We select Magnesium Fluoride (MgF2) as a material of the
  optical components because of its birefringent property and high
  transparency at UV wavelength. We have confirmed that the reflection
  at the Brewster's Angle of MgF2 plate is a good polarization analyzer
  for the Ly-alpha line by deriving its ordinary refractive index and
  extinction coefficient along the ordinary and extraordinary axes. These
  optical parameters are calculated with a least-square fitting in such a
  way that the reflectance and transmittance satisfy the Kramers-Kronig
  relation. The reflectance and transmittance against oblique incident
  angles for the s-polarized and the p-polarized light are measured
  using the synchrotron beamline at the Ultraviolet Synchrotron Orbital
  Radiation Facility (UVSOR). We have also measured a retardation of
  a zeroth-order waveplate made of MgF2. The thickness difference of
  the waveplate is 14.57 um.This waveplate works as a half-waveplate at
  121.74 nm. From this measurement, we estimate that a waveplate with
  the thickness difference of 15.71 um will work as a half-waveplate
  at the Ly-alpha wavelength. We have developed a rotating waveplate -
  polarization analyzer system called a prototype of CLASP polarimeter,
  and input the perfect Stokes Q and U signals. The modulation patterns
  that are consistent with the theoretical prediction are successfully
  obtained in both cases.

---------------------------------------------------------
Title: The Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP)j
Authors: Kobayashi, K.; Tsuneta, S.; Trujillo Bueno, J.; Bando, T.;
   Belluzzi, L.; Casini, R.; Carlsson, M.; Cirtain, J. W.; De Pontieu,
   B.; Hara, H.; Ichimoto, K.; Ishikawa, R.; Kano, R.; Katsukawa, Y.;
   Kim, T.; Kubo, M.; Manso Sainz, R.; Narukage, N.; Asensio Ramos,
   A.; Robinson, B.; Sakao, T.; Shimizu, T.; Stepan, J.; Suematsu, Y.;
   Watanabe, H.; West, E.; Winebarger, A. R.
2011AGUFM.P14C..05K    Altcode:
  We present an overview of the Chromospheric Lyman-Alpha
  SpectroPolarimeter (CLASP) program. CLASP is a proposed sounding rocket
  experiment currently under development as collaboration between Japan,
  USA and Spain. The aim is to achieve the first measurement of magnetic
  field in the upper chromosphere and transition region of the Sun
  through the detection and measurement of Hanle effect polarization
  of the Lyman alpha line. The Hanle effect (i.e. the magnetic field
  induced modification of the linear polarization due to scattering
  processes in spectral lines) is believed to be a powerful tool for
  measuring the magnetic field in the upper chromosphere, as it is more
  sensitive to weaker magnetic fields than the Zeeman effect, and also
  sensitive to magnetic fields tangled at spatial scales too small to be
  resolved. The Lyman-alpha (121.567 nm) line has been chosen because
  it is a chromospheric/transition-region line, and because the Hanle
  effect polarization of the Lyman-alpha line is predicted to be sensitive
  to 10-250 Gauss, encompassing the range of interest. Hanle effect is
  predicted to be observable as linear polarization or depolarization,
  depending on the geometry, with a fractional polarization amplitude
  varying between 0.1% and 1% depending on the strength and orientation of
  the magnetic field. This quantification of the chromospheric magnetic
  field requires a highly sensitive polarization measurement. The
  CLASP instrument consists of a large aperture (287 mm) Cassegrain
  telescope mated to a polarizing beamsplitter and a matched pair
  of grating spectrographs. The polarizing beamsplitter consists
  of a continuously rotating waveplate and a linear beamsplitter,
  allowing simultaneous measurement of orthogonal polarizations and
  in-flight self-calibration. Development of the instrument is underway,
  and prototypes of all optical components have been tested using a
  synchrotron beamline. The experiment is proposed for flight in 2014.

---------------------------------------------------------
Title: Ly-alpha polarimeter design for CLASP rocket experiment
Authors: Watanabe, H.; Narukage, N.; Kubo, M.; Ishikawa, R.; Bando, T.;
   Kano, R.; Tsuneta, S.; Kobayashi, K.; Ichimoto, K.; Trujillo-Bueno, J.
2011SPIE.8148E..0TW    Altcode: 2011SPIE.8148E..25W; 2014arXiv1407.4577W
  A sounding-rocket program called the Chromospheric Lyman-Alpha
  Spectro-Polarimeter (CLASP) is proposed to be launched in the summer of
  2014. CLASP will observe the solar chromosphere in Ly-alpha (121.567
  nm), aiming to detect the linear polarization signal produced by
  scattering processes and the Hanle effect for the first time. The
  polarimeter of CLASP consists of a rotating half-waveplate, a beam
  splitter, and a polarization analyzer. Magnesium Fluoride (MgF2) is
  used for these optical components, because MgF2 exhibits birefringent
  property and high transparency at ultraviolet wavelength. The
  development and comprehensive testing program of the optical components
  of the polarimeter is underway using the synchrotron beamline at the
  Ultraviolet Synchrotron Orbital Radiation Facility (UVSOR). The first
  objective is deriving the optical constants of MgF2 by the measurement
  of the reflectance and transmittance against oblique incident angles
  for the s-polarized and the p-polarized light. The ordinary refractive
  index and extinction coefficient along the ordinary and extraordinary
  axes are derived with a least-square fitting in such a way that the
  reflectance and transmittance satisfy the Kramers-Krönig relation. The
  reflection at the Brewster's Angle of MgF2 plate is confirmed to become
  a good polarization analyzer at Ly-alpha. The second objective is the
  retardation measurement of a zeroth-order waveplate made of MgF2. The
  retardation of a waveplate is determined by observing the modulation
  amplitude that comes out of a waveplate and a polarization analyzer. We
  tested a waveplate with the thickness difference of 14.57 um. The 14.57
  um waveplate worked as a half-waveplate at 121.74 nm. We derived that
  a waveplate with the thickness difference of 15.71 um will work as a
  half-waveplate at Ly-alpha wavelength. We developed a prototype of CLASP
  polarimeter using the MgF2 half-waveplate and polarization analyzers,
  and succeeded in obtaining the modulation patterns that are consistent
  with the theoretical prediction. We confirm that the performance of
  the prototype is optimized for measuring linear polarization signal
  with the least effect of the crosstalk from the circular polarization.

---------------------------------------------------------
Title: Overview of Chromospheric Lyman-Alpha SpectroPolarimeter
    (CLASP)
Authors: Narukage, Noriyuki; Tsuneta, Saku; Bando, Takamasa; Kano,
   Ryouhei; Kubo, Masahito; Ishikawa, Ryoko; Hara, Hirohisa; Suematsu,
   Yoshinori; Katsukawa, Yukio; Watanabe, Hiroko; Ichimoto, Kiyoshi;
   Sakao, Taro; Shimizu, Toshifumi; Kobayashi, Ken; Robinson, Brian; Kim,
   Tony; Winebarger, Amy; West, Edward; Cirtain, Jonathan; De Pontieu,
   Bart; Casini, Roberto; Trujillo Bueno, Javier; Stepan, Jiri; Manso
   Sainz, Rafael; Belluzzi, Luca; Asensio Ramos, Andres; Carlsson, Mats
2011SPIE.8148E..0HN    Altcode: 2011SPIE.8148E..16N
  The solar chromosphere is an important boundary, through which all of
  the plasma, magnetic fields and energy in the corona and solar wind
  are supplied. Since the Zeeman splitting is typically smaller than
  the Doppler line broadening in the chromosphere and transition region,
  it is not effective to explore weak magnetic fields. However, this is
  not the case for the Hanle effect, when we have an instrument with
  high polarization sensitivity (~ 0.1%). "Chromospheric Lyman- Alpha
  SpectroPolarimeter (CLASP)" is the sounding rocket experiment to detect
  linear polarization produced by the Hanle effect in Lyman-alpha line
  (121.567 nm) and to make the first direct measurement of magnetic
  fields in the upper chromosphere and lower transition region. To
  achieve the high sensitivity of ~ 0.1% within a rocket flight (5
  minutes) in Lyman-alpha line, which is easily absorbed by materials,
  we design the optical system mainly with reflections. The CLASP
  consists of a classical Cassegrain telescope, a polarimeter and a
  spectrometer. The polarimeter consists of a rotating 1/2-wave plate
  and two reflecting polarization analyzers. One of the analyzer also
  works as a polarization beam splitter to give us two orthogonal linear
  polarizations simultaneously. The CLASP is planned to be launched in
  2014 summer.

---------------------------------------------------------
Title: Widespread Nanoflare Variability Detected with Hinode/X-Ray
    Telescope in a Solar Active Region
Authors: Terzo, Sergio; Reale, Fabio; Miceli, Marco; Klimchuk, James
   A.; Kano, Ryouhei; Tsuneta, Saku
2011ApJ...736..111T    Altcode: 2011arXiv1105.2506T
  It is generally agreed that small impulsive energy bursts called
  nanoflares are responsible for at least some of the Sun's hot corona,
  but whether they are the explanation for most of the multimillion-degree
  plasma has been a matter of ongoing debate. We present here evidence
  that nanoflares are widespread in an active region observed by the X-Ray
  Telescope on board the Hinode mission. The distributions of intensity
  fluctuations have small but important asymmetries, whether taken
  from individual pixels, multipixel subregions, or the entire active
  region. Negative fluctuations (corresponding to reduced intensity)
  are greater in number but weaker in amplitude, so that the median
  fluctuation is negative compared to a mean of zero. Using Monte Carlo
  simulations, we show that only part of this asymmetry can be explained
  by Poisson photon statistics. The remainder is explainable through
  a tendency for exponentially decreasing intensity, such as would be
  expected from a cooling plasma produced from a nanoflare. We suggest
  that nanoflares are a universal heating process within active regions.

---------------------------------------------------------
Title: A Sounding Rocket Experiment for Spectropolarimetric
    Observations with the Ly<SUB>α</SUB> Line at 121.6 nm (CLASP)
Authors: Ishikawa, R.; Bando, T.; Fujimura, D.; Hara, H.; Kano,
   R.; Kobiki, T.; Narukage, N.; Tsuneta, S.; Ueda, K.; Wantanabe,
   H.; Kobayashi, K.; Trujillo Bueno, J.; Manso Sainz, R.; Stepan, J.;
   de Pontieu, B.; Carlsson, M.; Casini, R.
2011ASPC..437..287I    Altcode:
  A team consisting of Japan, USA, Spain, and Norway is developing a
  high-throughput Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP),
  which is proposed to fly with a NASA sounding rocket in 2014. CLASP will
  explore the magnetism of the upper solar chromosphere and transition
  region via the Hanle effect of the Ly<SUB>α</SUB> line for the first
  time. This experiment requires spectropolarimetric observations with
  high polarimetric sensitivity (∼0.1%) and wavelength resolution
  (0.1 Å). The final spatial resolution (slit width) is being discussed
  taking into account the required high signal-to-noise ratio. We have
  demonstrated the performance of the Ly<SUB>α</SUB> polarimeter by
  extensively using the Ultraviolet Synchrotron ORbital Radiation Facility
  (UVSOR) at the Institute for Molecular Sciences. In this contribution,
  we report these measurements at UVSOR together with the current status
  of the CLASP project.

---------------------------------------------------------
Title: Coronal-Temperature-Diagnostic Capability of the Hinode/
    X-Ray Telescope Based on Self-Consistent Calibration
Authors: Narukage, N.; Sakao, T.; Kano, R.; Hara, H.; Shimojo, M.;
   Bando, T.; Urayama, F.; DeLuca, E.; Golub, L.; Weber, M.; Grigis,
   P.; Cirtain, J.; Tsuneta, S.
2011SoPh..269..169N    Altcode: 2010arXiv1011.2867N; 2011SoPh..tmp....1N
  The X-Ray Telescope (XRT) onboard the Hinode satellite is an X-ray
  imager that observes the solar corona with unprecedentedly high angular
  resolution (consistent with its 1″ pixel size). XRT has nine X-ray
  analysis filters with different temperature responses. One of the most
  significant scientific features of this telescope is its capability
  of diagnosing coronal temperatures from less than 1 MK to more than
  10 MK, which has never been accomplished before. To make full use
  of this capability, accurate calibration of the coronal temperature
  response of XRT is indispensable and is presented in this article. The
  effect of on-orbit contamination is also taken into account in the
  calibration. On the basis of our calibration results, we review the
  coronal-temperature-diagnostic capability of XRT.

---------------------------------------------------------
Title: The Chromospheric Lyman Alpha SpectroPolarimeter (CLASP)
Authors: Kobayashi, K.; Tsuneta, S.; Trujillo Bueno, J.; Cirtain,
   J. W.; Bando, T.; Kano, R.; Hara, H.; Fujimura, D.; Ueda, K.; Ishikawa,
   R.; Watanabe, H.; Ichimoto, K.; Sakao, T.; de Pontieu, B.; Carlsson,
   M.; Casini, R.
2010AGUFMSH11B1632K    Altcode:
  Magnetic fields in the solar chromosphere play a key role in the
  energy transfer and dynamics of the solar atmosphere. Yet a direct
  observation of the chromospheric magnetic field remains one of the
  greatest challenges in solar physics. While some advances have been
  made for observing the Zeeman effect in strong chromospheric lines,
  the effect is small and difficult to detect outside sunspots. The
  Hanle effect offers a promising alternative; it is sensitive to weaker
  magnetic fields (e.g., 5-500 G for Ly-Alpha), and while its magnitude
  saturates at stronger magnetic fields, the linear polarization signals
  remain sensitive to the magnetic field orientation. The Hanle effect
  is not only limited to off-limb observations. Because the chromosphere
  is illuminated by an anisotropic radiation field, the Ly-Alpha line is
  predicted to show linear polarization for on-disk, near-limb regions,
  and magnetic field is predicted to cause a measurable depolarization. At
  disk center, the Ly-Alpha radiation is predicted to be negligible
  in the absence of magnetic field, and linearly polarized to an order
  of 0.3% in the presence of an inclined magnetic field. The proposed
  CLASP sounding rocket instrument is designed to detect 0.3% linear
  polarization of the Ly-Alpha line at 1.5 arcsecond spatial resolution
  (0.7’’ pixel size) and 10 pm spectral resolution. The instrument
  consists of a 30 cm aperture Cassegrain telescope and a dual-beam
  spectropolarimeter. The telescope employs a “cold mirror’’ design
  that uses multilayer coatings to reflect only the target wavelength
  range into the spectropolarimeter. The polarization analyzer consists of
  a rotating waveplate and a polarizing beamsplitter that comprises MgF2
  plates placed at Brewster’s Angle. Each output beam of the polarizing
  beamsplitter, representing two orthogonal linear polarizations, is
  dispersed and focused using a separate spherical varied-line-space
  grating, and imaged with a separate 512x512 CCD camera. Prototypes
  of key optical components have been fabricated and tested. Instrument
  design is being finalized, and the experiment will be proposed for a
  2014 flight aboard a NASA sounding rocket.

---------------------------------------------------------
Title: Hinode Observation of Photospheric Magnetic Activities
    Triggering X-ray Microflares Around a Well-developed Sunspot
Authors: Kano, R.; Shimizu, T.; Tarbell, T. D.
2010ApJ...720.1136K    Altcode:
  Microflares, which are small energetic events in the solar corona, are
  an example of dynamical phenomena suitable for understanding energy
  release processes in the solar corona. We identified 55 microflares
  around a well-developed sunspot surrounded by a moat with high-cadence
  X-ray images from the Hinode X-ray Telescope, and searched for their
  photospheric counterparts in line-of-sight magnetograms taken with the
  Hinode Solar Optical Telescope. We found opposite magnetic polarities
  encountering each other around the footpoints of 28 microflares,
  while we could not find such encounters around the footpoints of the
  other 27 microflares. Emerging magnetic fluxes in the moat were the
  dominant origin causing the encounters of opposite polarities (21 of
  28 events). Unipolar moving magnetic features (MMFs) with negative
  polarities the same as the sunspot definitely caused the encounters of
  opposite polarities for five microflares. The decrease of magnetic flux,
  i.e., magnetic flux cancellation, was confirmed at the encountering site
  in typical examples of microflares. Microflares were not isotropically
  distributed around the spot; the microflares with emerging magnetic
  fluxes (EMFs) were observed in the direction where magnetic islands
  with the same polarity as the spot were located at the outer boundary
  of the moat, while the microflares with negative MMFs were observed
  in the direction where magnetic islands with polarity opposite to the
  spot were located at the outer boundary of the moat. We also found that
  EMFs in the moat had a unique orientation in which those with the same
  polarity as the spot is closer to the spot than the other one that had
  the opposite polarity to the spot. These observational results lead
  to two magnetic configurations including magnetic reconnection for
  triggering energy release at least in half of the microflares around
  the spot, and suggest that the global magnetic structures around the
  spot strongly affect what kinds of polarity encounters are formed in
  the sunspot moat.

---------------------------------------------------------
Title: Orientation of X-Ray Bright Points in the Quiet Sun
Authors: Ueda, K.; Kano, R.; Tsuneta, S.; Shibahashi, H.
2010SoPh..261...77U    Altcode:
  Thanks to the high-resolution images from the X-ray telescope (XRT)
  aboard the Hinode satellite, X-ray bright points (XBPs) in the quiet
  region of the Sun are resolved and can be seen to have complex loop-like
  structures. We measure the orientation of such loop structures for 488
  XBPs picked up in 26 snapshot X-ray images near the disk center. The
  distribution of the orientation is slightly but clearly biased to
  the east - west direction: the random distribution is rejected with a
  significance level of 1% by the χ<SUP>2</SUP>-test. The distribution
  is similar to the orientation distribution for the bipolar magnetic
  fields. The XBP orientation is, however, much more random than that
  of the bipolar magnetic fields with similar size. 24% of the XBPs are
  due to emerging bipoles, while the remaining 76% are due to chance
  encounters of opposite polarities.

---------------------------------------------------------
Title: Analysis of the X-ray variability of an active region observed
    with Hinode/XRT for investigation of coronal heating
Authors: Terzo, Sergio; Tsuneta, Saku; Kano, Ryouhei; Miceli, Marco;
   Reale, Fabio
2010cosp...38.2898T    Altcode: 2010cosp.meet.2898T
  Impulsive mechanisms of solar and stellar coronal heating are under
  investigation. The analysis of the time variability of coronal emission
  is one of the useful tools. We analyze the small-scale variability of a
  solar active region in a high cadence Hinode/XRT observation. We compare
  measured fluctuation intensity distributions with the distribution
  expected for Poisson noise and look for possible signatures of
  nanoflaring activity, which might be extrapolated to stellar coronae.

---------------------------------------------------------
Title: A New View of the Sun with Hinode Mission
Authors: Sakao, Taro; Tsuneta, Saku; Shimojo, Masumi; Narukage,
   Noriyuki; Kano, Ryouhei; Obara, Takahiro; Watari, Shinichi; Hinode Team
2009TrSpT...7Tr215S    Altcode:
  We present highlights of observations of the Sun with Japanese Hinode
  mission launched by JAXA in September 2006. The scientific objective
  of Hinode mission is to observe, in an unprecedented detail, a wide
  variety of plasma activities in the Sun's corona together with magnetic
  activities on the photosphere and in the chromosphere, utilizing a suite
  of three state-of-the-art telescopes; Solar Optical Telescope (SOT),
  X-Ray Telescope (XRT), and EUV Imaging Spectrometer (EIS). Since the
  beginning of the observations late in October 2006, Hinode has been
  providing ample information on activities of magnetized plasmas in the
  solar atmosphere some of which are totally new to us. In this article,
  we present an overview of the Hinode mission as well as some highlights
  of the observations.

---------------------------------------------------------
Title: Plasma Outflows in the Corona as Observed With Hinode XRT
Authors: Sakao, T.; Kano, R.; Narukage, N.; Deluca, E. E.; Grigis, P.
2008AGUFMSH41B1624S    Altcode:
  We present imaging observations of plasma outflows in the solar corona
  made with X-Ray Telescope (XRT) aboard Hinode satellite. The XRT employs
  a back-illuminated CCD as the focal-plane imaging device which enables
  us, together with an optimized set of analysis filters, to investigate,
  for the first time, dynamic behavior of relatively cool (1-2 MK, say)
  plasmas in the corona. The XRT revealed a clear pattern of continuous
  outflow of plasmas from the edge of an active region NOAA AR 10942 right
  adjacent to a coronal hole. Plasmas of temperature ~1 MK flowed out
  with a sub-sonic velocity of typically ~140 km/s along magnetic field
  lines that are most likely open towards the interplanetary space. These
  outflowing plasmas may constitute a fraction of the (slow) solar
  wind. In addition to this discovery, the XRT has so far identified
  rich patterns of continuous outflows including those from coronal
  hole boundaries and along fan-like field lines rooted inside coronal
  holes. XRT observations of such plasma outflows in the corona are
  presented and their possible implications to the solar wind discussed.

---------------------------------------------------------
Title: The Thermal Structures of Solar Corona Revealed with Hinode/XRT
Authors: Narukage, N.; Sakao, T.; Kano, R.
2008AGUFMSH52A..03N    Altcode:
  The solar corona has a wide temperature range from less than 1MK
  (1,000,000K) to more than 10MK. The X-ray telescope (XRT) on board
  the Hinode satellite has 9 X-ray analysis filters with different
  temperature responses making it possible to detect both cool and
  hot coronal plasmas. Using the data observed with this telescope,
  we successfully derived the coronal temperature and emission measure
  around the whole sun, i.e., for not only active regions but also quiet
  regions and coronal holes. We also found that coronal structures are
  nicely classified using the temperature and emission measure. And the
  coronal structures were found to depend on the length of structure
  and the heating flux. Furthermore, we calculated the coronal potential
  magnetic field using the photospheric magnetic field. To compare the
  heating flux estimated with coronal temperature and the calculated
  coronal magnetic field might be the great clue to solving the big
  coronal heating question: why does the hot 1MK corona stably exist
  above the cool 6,000K solar surface? In this talk, we will show some
  results of our latest studies about the coronal thermal structures.

---------------------------------------------------------
Title: Hinode/XRT Diagnostics of Loop Thermal Structure
Authors: Reale, F.; Parenti, S.; Reeves, K. K.; Weber, M.; Bobra,
   M. G.; Barbera, M.; Kano, R.; Narukage, N.; Shimojo, M.; Sakao, T.;
   Peres, G.; Golub, L.
2008ASPC..397...50R    Altcode:
  We investigate possible diagnostics of the thermal structure of coronal
  loops from Hinode/XRT observations made with several filters. We
  consider the observation of an active region with five filters. We
  study various possible combinations of filter data to optimize for
  sensitivity to thermal structure and for signal enhancement.

---------------------------------------------------------
Title: Vertical Temperature Structures of the Solar Corona Derived
    with the Hinode X-Ray Telescope
Authors: Kano, Ryouhei; Sakao, Taro; Narukage, Noriyuki; Tsuneta,
   Saku; Kotoku, Jun'ichi; Bando, Takamasa; Deluca, Edward; Lundquist,
   Loraine; Golub, Leon; Hara, Hirohisa; Matsuzaki, Keiichi; Shimojo,
   Masumi; Shibasaki, Kiyoto; Shimizu, Toshifumi; Nakatani, Ichiro
2008PASJ...60..827K    Altcode:
  We obtained temperature structures in faint coronal features
  above and near the solar limb with the X-Ray Telescope aboard the
  Hinode satellite by accurately correcting the scattered X-rays
  from surrounding bright regions with occulted images during
  the solar eclipses. Our analysis yields a polar coronal hole
  temperature of about 1.0MK and an emission measure in the range of
  10<SUP>25.5</SUP>-10<SUP>26.0</SUP>cm<SUP>-5</SUP>. In addition,
  our methods allow us to measure the temperature and emission
  measure of two distinct quiet-Sun structures: radial (plume-like)
  structures near the boundary of the coronal-hole and diffuse quiet
  Sun regions at mid-latitudes. The radial structures appear to have
  increasing temperature with height during the first 100Mm, and
  constant temperatures above 100Mm. For the diffuse quiet-Sun region
  the temperatures are the highest just above the limb, and appear
  to decrease with height. These differences may be due to different
  magnetic configurations.

---------------------------------------------------------
Title: The Hinode X-Ray Telescope (XRT): Camera Design, Performance
    and Operations
Authors: Kano, R.; Sakao, T.; Hara, H.; Tsuneta, S.; Matsuzaki, K.;
   Kumagai, K.; Shimojo, M.; Minesugi, K.; Shibasaki, K.; DeLuca, E. E.;
   Golub, L.; Bookbinder, J.; Caldwell, D.; Cheimets, P.; Cirtain, J.;
   Dennis, E.; Kent, T.; Weber, M.
2008SoPh..249..263K    Altcode:
  The X-ray Telescope (XRT) aboard the Hinode satellite is a grazing
  incidence X-ray imager equipped with a 2048×2048 CCD. The XRT has
  1 arcsec pixels with a wide field of view of 34×34 arcmin. It is
  sensitive to plasmas with a wide temperature range from &lt; 1 to 30
  MK, allowing us to obtain TRACE-like low-temperature images as well as
  Yohkoh/SXT-like high-temperature images. The spacecraft Mission Data
  Processor (MDP) controls the XRT through sequence tables with versatile
  autonomous functions such as exposure control, region-of-interest
  tracking, flare detection, and flare location identification. Data are
  compressed either with DPCM or JPEG, depending on the purpose. This
  results in higher cadence and/or wider field of view for a given
  telemetry bandwidth. With a focus adjust mechanism, a higher resolution
  of Gaussian focus may be available on-axis. This paper follows the
  first instrument paper for the XRT (Golub et al., Solar Phys.243, 63,
  2007) and discusses the design and measured performance of the X-ray
  CCD camera for the XRT and its control system with the MDP.

---------------------------------------------------------
Title: The Analysis of Hinode/XRT Observations
Authors: Deluca, E. E.; Weber, M.; Savcheva, A.; Saar, S.; Testa,
   P.; Cirtain, J. W.; Sakao, T.; Noriyuki, N.; Kano, R.; Shimizu, T.
2008AGUSMSP51B..02D    Altcode:
  This poster will present the current state of Hinode/XRT analysis
  software. We will give an overview of the XRT Analysis Guide. We will
  include a detailed discussion of the following topics: <P />Co-alignment
  with SOT and EIS Spot removal for dynamics studies Filter calibration
  for thermal studies Dark calibrations <P />Sample data sets will be
  discussed and links to the data products will be provided.

---------------------------------------------------------
Title: Molecular Contamination Assessments on
    &lt;i&gt;Hinode&lt;/i&gt; X-Ray Telescope
Authors: Urayama, Fumitaka; Bando, Takamasa; Kano, Ryouhei; Hara,
   Hirohisa; Narukage, Noriyuki; Sakao, Taro
2008JSASS..56..536U    Altcode:
  The &lt;i&gt;Hinode&lt;/i&gt; (Solar-B) was launched by M-V rocket on 22
  September 2006 UT. The telemetry data of the &lt;i&gt;Hinode&lt;/i&gt;
  X-ray Telescope (XRT) showed that the X-ray count rate detected with
  the XRT had decreased rapidly since the operational heaters on the
  XRT telescope tube were turned on. This is attributed to the fact that
  molecular contaminants accumulated onto the CCD with the temperature
  of -60ºC resulting in the degradation of the XRT sensitivity. We baked
  the CCD at the temperature of 35ºC in order to remove the contaminants
  from the CCD surface. However many contaminant spots appeared on the
  surface. We found that major contaminant source existed in the telescope
  tube, and identified the contaminants as diethylhexyl phthalate (DEHP)
  or DEHP-like organics. The mechanisms to yield the contaminant spots
  were discussed.

---------------------------------------------------------
Title: Multiplicity of Solar X-Ray Corona in Time and Space
Authors: Kano, R.; XRT Team
2008PFR.....2S1010K    Altcode:
  The Soft X-ray Telescope (XRT) aboard the Hinode satellite is a grazing
  incidence X-ray telescope equipped with 2 k × 2 k CCD. XRT has 1
  arcsec resolution with wide field-of-view of 34 × 34 arcmin. It is
  sensitive to &lt; 1 MK to 30 MK, allowing us to obtain TRACE-like
  low temperature images as well. Co-alignment with SOT and EIS is
  realized through the XRT visible light telescope and with temperature
  overlap with EIS. Spacecraft mission data processor (MDP) controls XRT
  through the sequence tables with versatile autonomous functions such
  as exposure control, region-of-interest tracking, flare detection and
  flare location identification. Data is compressed either with DPCM or
  JPEG, depending on the purpose. This results in higher cadence and/or
  wider field-of-view for given telemetry bandwidth. With focus adjust
  mechanism, higher resolution of Gaussian focus may be available on-axis.

---------------------------------------------------------
Title: Relation between coronal temperature and magnetic field
Authors: Narukage, Noriyuki; Kano, Ryouhei; Shiota, Daiko; Sakao, Taro
2008cosp...37.2184N    Altcode: 2008cosp.meet.2184N
  The solar corona has a wide temperature range from less than 1MK to
  more than 10MK. The X-ray telescope (XRT) on board Hinode satellite
  has 9 X-ray analysis filters to observe the almost of whole coronal
  plasma. Using the data observed with this telescope, we successfully
  derived the coronal temperature around the whole sun. We found that
  coronal structures are nicely classified using the temperature and
  emission measure. The coronal structures were found to depend on the
  length of structure and the heating flux. Furthermore, we calculated
  the coronal potential magnetic field in high spatial resolution using
  the photospheric magnetic field observed with SOHO/MDI. To compare the
  heating flux estimated with coronal temperature and the calculated
  coronal magnetic field might be the great clue to solving the big
  coronal heating question.

---------------------------------------------------------
Title: Cross calibration of soft X-ray telescopes between Hinode/XRT
    and GOES13/SXI
Authors: Narukage, N.; Sakao, T.; Kano, R.; Shimojo, M.; Cirtain,
   J.; Deluca, E.; Nitta, N.; Lemen, J.
2007AGUFMSH53A1050N    Altcode:
  The X-Ray Telescope (XRT) aboard Hinode satellite is a grazing
  incidence telescope to observe all the coronal features with a wide
  temperature range from less than 1MK to more than 10MK. And the XRT
  has 9 X-ray analysis filters which are optimized to observed the
  almost whole coronal plasma and to derived the coronal temperature
  distribution. Meanwhile, the GOES13 satellite carries a Solar X-ray
  Imager (SXI) to monitor the solar X-rays. The SXI is also a grazing
  incidence telescope and has 7 X-ray filters. The XRT and SXI are
  similar telescopes to observe the dynamic solar corona. On 24 Nov 2006,
  the XRT and SXI-team performed the simultaneous observation for the
  cross calibration between XRT and SXI. In this study, we analyzed
  this data set and checked the actual characteristics of each X-ray
  analysis filter.

---------------------------------------------------------
Title: Mangetic field properties at the footpoints of solar
    microflares (active-region transient brightenings)
Authors: Shimizu, T.; Kano, R.; Katsukawa, Y.; Kubo, M.; Deluca, E.;
   Ichimoto, K.; Lites, B.; Nagata, S.; Sakao, T.; Shine, R.; Suematsu,
   Y.; Tarbell, T.; Title, A.; Tsuneta, S.
2007AGUFMSH52C..06S    Altcode:
  Solar active regions produce numerous numbers of small-scale explosive
  energy releases, i.e., microflares, which are captured by imaging
  observations in soft X-rays as transient brightenings of small-scale
  coronal loops. Thanks to advanced performance of X-Ray Telescope (XRT)
  onboard the Hinode satellite, we can investigate finer structure
  of the brightening X-ray sources in more details than we did with
  Yohkoh data. One of important questions on microflares is what causes
  microflares. The simultaneous visible-light observations by the Solar
  Optical Telescope (SOT) allow us to explore magnetic activities
  and magnetic field configuration at the photospheric footpoints
  of brightening loops, giving key observations to investigate the
  question. For our investigations of corona-photosphere magnetic
  coupling, we have established co-alignment between SOT and XRT
  with accuracy better than 1 arcsec (Shimizu et al. 2007, PASJ in
  press). It turns out that Ca II H observations are very useful
  to identify the exact positions of footpoints of X-ray transient
  brightening loops. Small "Kernels" are sometimes observed in Ca II H
  and they may be signature of highly accelerated non-thermal particles
  impinging on chromosphere. As already shown in Shimizu et al.(2002),
  frequent transient brightenings are observed at the locations where
  emerging activities are on going. However, another type of brightening
  triggering mechanism should exist to explain some observed multiple-loop
  brightenings. In the multiple-loop brightenings, multiple loops are
  magnetically in parallel with each other and no apparent magnetic
  activities, such as emerging and canceling, are observed at and near
  the footpoints. This paper will present SOT observations of some
  microflares observed with XRT.

---------------------------------------------------------
Title: Slipping Magnetic Reconnection in Coronal Loops
Authors: Aulanier, Guillaume; Golub, Leon; DeLuca, Edward E.; Cirtain,
   Jonathan W.; Kano, Ryouhei; Lundquist, Loraine L.; Narukage, Noriyuki;
   Sakao, Taro; Weber, Mark A.
2007Sci...318.1588A    Altcode:
  Magnetic reconnection of solar coronal loops is the main process that
  causes solar flares and possibly coronal heating. In the standard
  model, magnetic field lines break and reconnect instantaneously at
  places where the field mapping is discontinuous. However, another mode
  may operate where the magnetic field mapping is continuous but shows
  steep gradients: The field lines may slip across each other. Soft
  x-ray observations of fast bidirectional motions of coronal loops,
  observed by the Hinode spacecraft, support the existence of this
  slipping magnetic reconnection regime in the Sun’s corona. This
  basic process should be considered when interpreting reconnection,
  both on the Sun and in laboratory-based plasma experiments.

---------------------------------------------------------
Title: Evidence for Alfvén Waves in Solar X-ray Jets
Authors: Cirtain, J. W.; Golub, L.; Lundquist, L.; van Ballegooijen,
   A.; Savcheva, A.; Shimojo, M.; DeLuca, E.; Tsuneta, S.; Sakao, T.;
   Reeves, K.; Weber, M.; Kano, R.; Narukage, N.; Shibasaki, K.
2007Sci...318.1580C    Altcode:
  Coronal magnetic fields are dynamic, and field lines may misalign,
  reassemble, and release energy by means of magnetic reconnection. Giant
  releases may generate solar flares and coronal mass ejections and,
  on a smaller scale, produce x-ray jets. Hinode observations of polar
  coronal holes reveal that x-ray jets have two distinct velocities:
  one near the Alfvén speed (~800 kilometers per second) and another
  near the sound speed (200 kilometers per second). Many more jets were
  seen than have been reported previously; we detected an average of
  10 events per hour up to these speeds, whereas previous observations
  documented only a handful per day with lower average speeds of 200
  kilometers per second. The x-ray jets are about 2 × 10<SUP>3</SUP> to
  2 × 10<SUP>4</SUP> kilometers wide and 1 × 10<SUP>5</SUP> kilometers
  long and last from 100 to 2500 seconds. The large number of events,
  coupled with the high velocities of the apparent outflows, indicates
  that the jets may contribute to the high-speed solar wind.

---------------------------------------------------------
Title: Continuous Plasma Outflows from the Edge of a Solar Active
    Region as a Possible Source of Solar Wind
Authors: Sakao, Taro; Kano, Ryouhei; Narukage, Noriyuki; Kotoku,
   Jun'ichi; Bando, Takamasa; DeLuca, Edward E.; Lundquist, Loraine L.;
   Tsuneta, Saku; Harra, Louise K.; Katsukawa, Yukio; Kubo, Masahito;
   Hara, Hirohisa; Matsuzaki, Keiichi; Shimojo, Masumi; Bookbinder, Jay
   A.; Golub, Leon; Korreck, Kelly E.; Su, Yingna; Shibasaki, Kiyoto;
   Shimizu, Toshifumi; Nakatani, Ichiro
2007Sci...318.1585S    Altcode:
  The Sun continuously expels a huge amount of ionized material into
  interplanetary space as the solar wind. Despite its influence on the
  heliospheric environment, the origin of the solar wind has yet to
  be well identified. In this paper, we report Hinode X-ray Telescope
  observations of a solar active region. At the edge of the active region,
  located adjacent to a coronal hole, a pattern of continuous outflow of
  soft-x-ray emitting plasmas was identified emanating along apparently
  open magnetic field lines and into the upper corona. Estimates of
  temperature and density for the outflowing plasmas suggest a mass
  loss rate that amounts to ~1/4 of the total mass loss rate of the
  solar wind. These outflows may be indicative of one of the solar wind
  sources at the Sun.

---------------------------------------------------------
Title: Fine Thermal Structure of a Coronal Active Region
Authors: Reale, Fabio; Parenti, Susanna; Reeves, Kathy K.; Weber,
   Mark; Bobra, Monica G.; Barbera, Marco; Kano, Ryouhei; Narukage,
   Noriyuki; Shimojo, Masumi; Sakao, Taro; Peres, Giovanni; Golub, Leon
2007Sci...318.1582R    Altcode:
  The determination of the fine thermal structure of the solar corona is
  fundamental to constraining the coronal heating mechanisms. The Hinode
  X-ray Telescope collected images of the solar corona in different
  passbands, thus providing temperature diagnostics through energy
  ratios. By combining different filters to optimize the signal-to-noise
  ratio, we observed a coronal active region in five filters, revealing
  a highly thermally structured corona: very fine structures in the
  core of the region and on a larger scale further away. We observed
  continuous thermal distribution along the coronal loops, as well as
  entangled structures, and variations of thermal structuring along the
  line of sight.

---------------------------------------------------------
Title: Magnetic Feature and Morphological Study of X-Ray Bright
    Points with Hinode
Authors: Kotoku, Jun'ichi; Kano, Ryouhei; Tsuneta, Saku; Katsukawa,
   Yukio; Shimizu, Toshifumi; Sakao, Taro; Shibazaki, Kiyoto; Deluca,
   Edward E.; Korreck, Kelly E.; Golub, Leon; Bobra, Monica
2007PASJ...59S.735K    Altcode:
  We observed X-ray bright points (XBPs) in a quiet region of the Sun
  with the X-Ray Telescope (XRT) aboard the Hinode satellite on 2006
  December 19. XRT's high-resolution X-ray images revealed many XBPs with
  complicated structure and evolving dramatically with time. Almost all
  of the dynamic eruptions in the quiet region were composed of XBPs,
  and they had either loop or multiloop shapes, as is observed in larger
  flares. Brightening XBPs had strong magnetic fields with opposite
  polarities near their footpoints. While we have found a possible
  example of associated magnetic cancellation, other XBPs brighten and
  fade without any associated movement of the photospheric magnetic field.

---------------------------------------------------------
Title: A Study of Polar Jet Parameters Based on Hinode XRT
    Observations
Authors: Savcheva, Antonia; Cirtain, Jonathan; Deluca, Edward E.;
   Lundquist, Loraine L.; Golub, Leon; Weber, Mark; Shimojo, Masumi;
   Shibasaki, Kiyoto; Sakao, Taro; Narukage, Noriyuki; Tsuneta, Saku;
   Kano, Ryouhei
2007PASJ...59S.771S    Altcode:
  Hinode/SOHO campaign 7197 is the most extensive study of polar jet
  formation and evolution from within both the north and south polar
  coronal holes so far. For the first time, this study showed that the
  appearance of X-ray jets in the solar coronal holes occurs at very high
  frequency - about 60 jets d<SUP>-1</SUP> on average. Using observations
  collected by the X-Ray Telescope on Hinode, a number of physical
  parameters from a large sample of jets were statistically studied. We
  measured the apparent outward velocity, the height, the width and
  the lifetime of the jets. In our sample, all of these parameters show
  peaked distributions with maxima at 160kms<SUP>-1</SUP> for the outward
  velocity, 5 × 10<SUP>4</SUP> km for the height, 8 × 10<SUP>3</SUP>
  km for the width, and about 10min for the lifetime of the jets. We
  also present the first statistical study of jet transverse motions,
  which obtained transverse velocities of 0-35kms<SUP>-1</SUP>. These
  values were obtained on the basis of a larger (in terms of frequency)
  and better sampled set of events than what was previously statistically
  studied (Shimojo et al. 1996, PASJ, 48, 123). The results were made
  possible by the unique characteristics of XRT. We describe the methods
  used to determine the characteristics and set some future goals. We
  also show that despite some possible selection effects, jets preferably
  occur inside the polar coronal holes.

---------------------------------------------------------
Title: Evolution of the Sheared Magnetic Fields of Two X-Class Flares
    Observed by Hinode/XRT
Authors: Su, Yingna; Golub, Leon; van Ballegooijen, Adriaan; Deluca,
   Edward E.; Reeves, Kathy K.; Sakao, Taro; Kano, Ryouhei; Narukage,
   Noriyuki; Shibasaki Kiyoto
2007PASJ...59S.785S    Altcode:
  We present multi-wavelength observations of the evolution of the sheared
  magnetic fields in NOAA Active Region 10930, where two X-class flares
  occurred on 2006 December 13 and December 14, respectively. Observations
  made with the X-ray Telescope (XRT) and the Solar Optical Telescope
  (SOT) aboard Hinode suggest that the gradual formation of the sheared
  magnetic fields in this active region is caused by the rotation and
  west-to-east motion of an emerging sunspot. In the pre-flare phase
  of the two flares, XRT shows several highly sheared X-ray loops in
  the core field region, corresponding to a filament seen in the TRACE
  EUV observations. XRT observations also show that part of the sheared
  core field erupted, and another part of the sheared core field stayed
  behind during the flares, which may explain why a large part of the
  filament is still seen by TRACE after the flare. About 2-3 hours after
  the peak of each flare, the core field becomes visible in XRT again,
  and shows a highly sheared inner and less-sheared outer structure. We
  also find that the post-flare core field is clearly less sheared than
  the pre-flare core field, which is consistent with the idea that the
  energy released during the flares is stored in the highly sheared
  fields prior to the flare.

---------------------------------------------------------
Title: An On-Orbit Determination of the On-Axis Point Spread Function
    of the Hinode X-Ray Telescope
Authors: Weber, Mark; Deluca, Edward E.; Golub, Leon; Cirtain,
   Jonathan; Kano, Ryouhei; Sakao, Taro; Shibasaki, Kiyoto; Narukage,
   Noriyuki
2007PASJ...59S.853W    Altcode:
  The Hinode X-ray Telescope provides unprecedented observations of
  the solar corona in X-rays, due in part to its fine resolution. The
  X-ray point spread function (PSF) was measured before launch at the
  NASA X-ray Calibration Facility to have a FWHM of 0.8”. This paper
  describes the work to verify the PSF measurements using on-orbit
  observations of planetary transits and solar eclipses. Analysis of a
  Mercury transit gives a PSF FWHM = 1.0" ± 0.12".

---------------------------------------------------------
Title: The X-Ray Telescope (XRT) for the Hinode Mission
Authors: Golub, L.; DeLuca, E.; Austin, G.; Bookbinder, J.; Caldwell,
   D.; Cheimets, P.; Cirtain, J.; Cosmo, M.; Reid, P.; Sette, A.; Weber,
   M.; Sakao, T.; Kano, R.; Shibasaki, K.; Hara, H.; Tsuneta, S.; Kumagai,
   K.; Tamura, T.; Shimojo, M.; McCracken, J.; Carpenter, J.; Haight,
   H.; Siler, R.; Wright, E.; Tucker, J.; Rutledge, H.; Barbera, M.;
   Peres, G.; Varisco, S.
2007SoPh..243...63G    Altcode:
  The X-ray Telescope (XRT) of the Hinode mission provides an
  unprecedented combination of spatial and temporal resolution in solar
  coronal studies. The high sensitivity and broad dynamic range of XRT,
  coupled with the spacecraft's onboard memory capacity and the planned
  downlink capability will permit a broad range of coronal studies over
  an extended period of time, for targets ranging from quiet Sun to
  X-flares. This paper discusses in detail the design, calibration, and
  measured performance of the XRT instrument up to the focal plane. The
  CCD camera and data handling are discussed separately in a companion
  paper.

---------------------------------------------------------
Title: The Dynamics Of Fine Structures In Solar X-ray Jets
Authors: Shimojo, Masumi; Narukage, N.; Kano, R.; Sakao, T.; Tsuneta,
   T.; Cirtain, J. W.; Lundquist, L. L.; Deluca, E. E.; Golub, L.
2007AAS...210.9422S    Altcode: 2007BAAS...39Q.221S
  The X-ray telescope(XRT) aboard HINODE satellite has the great
  spatial/time resolution in X-ray range. And, the observations using
  XRT have revealed the fine structures of solar corona. From the
  observations, we found the fine thread structures in the X-ray jets
  and the structures move dynamically like wave. We also found that some
  X-ray jets start just after small loop expansion in the footpoint
  brightening. The observation results suggest that the reconnection
  process X-ray jets is very similar to that in large flares.

---------------------------------------------------------
Title: Hinode Data Calibration For Precise Image Co-alignment:
    XRT vs. SOT
Authors: Shimizu, Toshifumi; DeLuca, E. E.; Lundquist, L.; Sakao,
   T.; Kubo, M.; Narukage, N.; Kano, R.; Katsukawa, Y.; Ichimoto, K.;
   Suematsu, Y.; Tsuneta, S.; Tarbell, T.; Shine, D.; Hinode Team
2007AAS...210.9417S    Altcode: 2007BAAS...39Q.220S
  From late October in 2006, Hinode solar optical telescope (SOT) has
  started to produce series of 0.2-0.3 arcsec visible-light images,
  revealing dynamical behaviors of solar magnetic fields on the
  solar surface. Simultaneously, Hinode X-ray telescope (XRT) has been
  providing 1 arcsec resolution X-ray images of the solar corona, giving
  the location of heating and dynamics occuring in the corona. Precise
  image co-alignment of SOT data on XRT data with sub-arcsec accuracy is
  required to provide new information regarding connecting the corona to
  the photosphere. This presentation will give an introduction of Hinode
  between-telescopes' image co-alignment to SPD participants. For active
  region observations with sunspots, sunspots can be used as fiducial to
  co-align the data from the two telescopes each other. Satellite jitter
  in order of 1 arcsec or less is included in the series of XRT data,
  whereas image stabilization system (correlation tracker) removes the
  satellite jitter from the series of SOT images. Telescope pointings show
  orbital variation in order of a few arcsec, which can be well predicted
  from Hinode orbit information. Modeling co-alignment is under study
  and it is the only precise method for quiet Sun and limb observations.

---------------------------------------------------------
Title: Coronal Temperature Diagnostics With Hinode X-ray Telescope
Authors: Narukage, Noriyuki; Sakao, T.; Kano, R.; Shimojo, M.; Tsuneta,
   S.; Kosugi, T.; Deluca, E. E.; Golub, L.; Weber, M.; Cirtain, J.;
   Japan-US X-Ray Telescope Team
2007AAS...210.6304N    Altcode: 2007BAAS...39..172N
  An X-ray telescope (XRT) on board HINODE satellite observes the Sun
  in X-rays with high special resolution (1arcsec 730km on solar the
  disk). This telescope has 9 X-ray filters with different temperature
  responses. Using these filters, the XRT can detect the coronal
  plasma with a wide temperature range from less than 1MK to more
  than 10MK. Moreover, based on observations with more than 2 filters,
  we can estimate the coronal temperature. In this paper, we use the
  filter ratio method for coronal temperature diagnostics. Using this
  method, we can easily estimate the averaged temperature of the coronal
  plasma along the line-of-sight. This method has been used frequently
  in the past, but the high quality XRT data give us temperature maps
  with unprecedented accuracy and resolution. The XRT usually takes
  the full Sun images with 2 kinds of filters 4 times a day. Using this
  data and filter ratio method, we can obtain full Sun temperature maps
  with high special resolution. In our analysis, we can derive reliable
  temperatures not only in active regions but also in quiet regions and
  coronal holes. This map can be created with the data set of one synoptic
  observation. This means that we can obtain 4 maps a day. The result is
  a full Sun temperature movie that gives us an unprecedented view of the
  time evolution of solar temperature. In this meeting, we will show the
  full Sun temperature movie and our coronal temperature analysis results.

---------------------------------------------------------
Title: Continuous Upflow of Plasmas at the Edge of an Active Region
    as Revealed by the X-ray Telescope (XRT) aboard Hinode
Authors: Sakao, Taro; Kano, R.; Narukage, N.; Kotoku, J.; Bando, T.;
   DeLuca, E. E.; Lundquist, L. L.; Golub, L.; Kubo, M.; Katsukawa, Y.;
   Tsuneta, S.; Hara, H.; Matsuzaki, K.; Shimojo, M.; Shibasaki, K.;
   Shimizu, T.; Nakatani, I.
2007AAS...210.7205S    Altcode: 2007BAAS...39Q.179S
  We present X-ray imaging observations with Hinode X-Ray Telescope (XRT)
  of an active region NOAA AR 10942 made in the period of 20-22 February
  2007. A prominent feature that drew our particular attention is that
  there revealed continuous upflow of soft-X-ray-emitting plasmas along
  apparently-open field lines towards the outer corona emanating from the
  edge of the active region. <P />The field lines are originated from
  an ensamble of small spots of following polarity, and are located at
  a border between the active region and an adjacent equatorial coronal
  hole(s) located to the east. The upflow was observed to be continuous
  throughout the three days of observation intervals with projected
  velocity of 140 km/s, accompanied with undulating motion of the field
  lines. <P />We assert that these upflowing plasmas would be a possible
  source of slow solar wind material, which supports a foresighted
  notion which grew out of interplanetary scintillation observations
  that slow solar wind most likely has its origin in the vicinity of
  active regions with large flux expansion (Kojima et al. 1999). <P />A
  preliminaty analysis indicates that the temperature of the upflowing
  material near the base of the field lines is 1.3 MK with number density
  of 2 × 10<SUP>9 </SUP>/cm<SUP>3</SUP>. Assuming that all the material
  is to escape to the interplanetary space, this leads to a mass loss
  rate of 2 × 10<SUP>11</SUP> g/s which amounts to a good fraction of
  the total mass loss rate for solar wind. It is noteworthy that, even
  apart from this unique upflow, we see continuous (up)flows of plasmas
  anywhere around (surrounding) the active region. <P />Details of the
  upflow will be presented and their possible implication to slow solar
  wind discussed.

---------------------------------------------------------
Title: Structure and Coronal Activity around Filament Channels
    Observed with Hinode XRT And TRACE
Authors: Lundquist, Loraine L.; van Ballegooijen, A. A.; Reeves,
   K. K.; Sakao, T.; DeLuca, E. E.; Narukage, N.; Kano, R.
2007AAS...210.9427L    Altcode: 2007BAAS...39..221L
  The combination of multi-wavelength, high resolution, high cadence
  data from the Hinode X-Ray Telescope (XRT) and the Transition Region
  And Coronal Explorer (TRACE) give an unprecedented view of solar
  active region dynamics and coronal topology. We focus on examples of
  filament structures observed by TRACE and XRT in December 2006 and
  February 2007. Co-alignment of observations in these two instruments
  yields a striking picture of the coronal structures, with loops lying
  both along and above the filament. Overlying loops exhibit remarkable
  dynamics while the filament lies dormant, and numerous x-point and
  triple-leg structures undergo repeated brightenings. We also employ
  magnetic field data from SOT and from SOLIS to compare a non-linear
  force-free model of the coronal magnetic field with the observed loops.

---------------------------------------------------------
Title: Temperature Structures Above Coronal Hole and Quiet Sun
Authors: Kano, Ryouhei; Sakao, T.; Narukage, N.; Kotoku, J.; Bando,
   T.; DeLuca, E. E.; Lundquist, L.; Golub, L.; Tsuneta, S.; Hara, H.;
   Shibasaki, K.; Shimojo, M.
2007AAS...210.9436K    Altcode: 2007BAAS...39..223K
  The X-ray Telescope (XRT) on board Hinode satelite has the capability
  to derive the temperature structure in the solar corona. We present
  the hieght dependence of the temperature above the limb. Because X-ray
  intensity above the limb is so faint, it is important to estimate the
  scattered light from disk corona. The eclipses happened on February 17
  and March 19 in 2007 at Hinode orbit. On February 17, we took X-ray
  images above the south polar coronal hole, while Moon passed it. On
  March 19, we took the data for quiet Sun in the same way. <P />We
  can estimated the scattered light from the eclipse data, and derived
  the scatter-free X-ray images above the solar limb. In this meeting,
  we will present the temperatures above coronal hole and quiet Sun,
  based on the eclipse data.

---------------------------------------------------------
Title: Tolerance test of a sample filter for use in space
Authors: Hayashi, Masao; Tanaka, Mikito; Komiyama, Yutaka; Okamura,
   Sadanori; Tsuneta, Saku; Noguchi, Motokazu; Nakagiri, Masao; Kano,
   Ryouhei; Kimura, Toshihiko
2006PNAOJ...9...21H    Altcode:
  We report the result of a tolerance test of a sample filter for the
  planned Very Wide Field Imager on board the Hubble Origin Probe. We
  investigated whether the properties of the filter and its components,
  i.e., color glass, synthetic quartz, short-wavelength-pass coating
  and long-wavelength-pass coating, changed after they were put in a
  vacuum, after they were subjected to a thermal cycle, and after they
  were exposed to γ ray. Results are shown mostly in graphical form. No
  significant change of the properties was observed for the filter and
  any of the components before and after the tests, except for the color
  glass which was exposed to strong γ ray.

---------------------------------------------------------
Title: Contamination evaluation and thermal vacuum bakeout for
    SOLAR-B visible-light and X-ray telescope
Authors: Tamura, Tomonori; Hara, Hirohisa; Tsuneta, Saku; Ichimoto,
   Kiyoshi; Kumagai, Kazuyoshi; Nakagiri, Masao; Shimizu, Toshifumi;
   Sakao, Taro; Kano, Ryouhei
2005RNAOJ...8...21T    Altcode:
  In the development of space telescopes, we are concerned about molecular
  outgassing materials from telescope components. In particular, for
  solar telescopes in space, the deposition of the outgassing materials
  may lead to the increase of solar absorptance at a mirror surface
  and it causes the thermal distortion due to the resultant temperature
  increase. The mirror reflectivity at vacuum ultraviolet wavelengths
  is very sensitive to molecular contamination. We have extensively
  evaluated reflectance at 121.6nm (Lyman-alpha) of the contamination
  witness mirrors exposed to the telescope testing environments in the
  SOLAR-B visible-light telescope program. Thermal vacuum bakeout of
  flight components is very effective process to reduce the outgassing
  rate. We have severe contamination control program during the assembly
  and testing of the SOLAR-B telescope up to launch of the satellite.

---------------------------------------------------------
Title: Science of the X-ray Sun: The X-ray telescope on Solar-B
Authors: DeLuca, E. E.; Weber, M. A.; Sette, A. L.; Golub, L.;
   Shibasaki, K.; Sakao, T.; Kano, R.
2005AdSpR..36.1489D    Altcode:
  The X-Ray Telescope (XRT) on Solar-B is designed to provide high
  resolution, high cadence observations of the X-ray corona through
  a wide range of filters. The XRT science team has identified four
  general problems in coronal physics as the primary science goals for our
  instrument. Each of these goals will require collaborative observations
  from the other Solar-B instruments: EUV Imaging Spectrograph (EIS)
  and Solar Optical Telescope Focal Plane Package (SOT). We will discuss
  the science goals and observations needed to address those goals.

---------------------------------------------------------
Title: SolarB X-Ray Telescope (XRT)
Authors: Kano, R.; Hara, H.; Shimojo, M.; Tsuneta, S.; Sakao, T.;
   Matsuzaki, K.; Kosugi, T.; Golub, L.; Deluca, E. E.; Bookbinder,
   J. A.; Cheimets, P.; Owens, J. K.; Hill, L. D.
2004ASPC..325...15K    Altcode:
  The Soft X-ray Telescope (XRT) aboard SolarB is a grazing incidence
  X-ray telescope equipped with 2k × 2k CCD. XRT has 1 arcsec resolution
  with wide field-of-view of 34 × 34 arcmin. It is sensitive to
  &lt;1 MK to 30 MK, allowing us to obtain TRACE-like low temperature
  images as well. Co-alignment with SOT and EIS is realized through
  the XRT visible light telescope and with temperature overlap with
  EIS. Spacecraft mission data processor (MDP) controls XRT through
  the sequence tables with versatile autonomous functions such as
  exposure control, region-of-interest tracking, flare detection and
  flare location identification. Data are compressed either with DPCM or
  JPEG, depending on the purpose. This results in higher cadence and/or
  wider field-of-view for given telemetry bandwidth. With focus adjust
  mechanism, higher resolution of Gaussian focus may be available on-axis.

---------------------------------------------------------
Title: Focal plane CCD camera for the X-Ray Telescope (XRT) aboard
    SOLAR-B
Authors: Sakao, Taro; Kano, Ryouhei; Hara, Hirohisa; Matsuzaki,
   Keiichi; Shimojo, Masumi; Tsuneta, Saku; Kosugi, Takeo; Shibasaki,
   Kiyoto; Kumagai, Kazuyoshi; Sawa, Masaki; Tamura, Tomonori; Iwamura,
   Satoru; Nakano, Mitsuhiko; Du, Zhangong; Hiyoshi, Kenji; Horii,
   Michihiro; Golub, Leon; Bookbinder, Jay A.; Cheimets, Peter C.; Hill,
   Lawrence D.; Owens, Jerry K.
2004SPIE.5487.1189S    Altcode:
  We present scientific as well as engineering overview of the X-Ray
  Telescope (XRT) aboard the Japanese Solar-B mission to be launched in
  2006, with emphasis on the focal plane CCD camera that employs a 2k
  x 2k back-thinned CCD. Characterization activities for the flight CCD
  camera made at the National Astronomical Observatory of Japan (NAOJ)
  are discussed in detail with some of the results presented.

---------------------------------------------------------
Title: Design and Performance of Tip-Tilt Mirror System for Solar
    Telescope
Authors: Kodeki, Kazuhide; Fukushima, Kazuhiko; Hara, Hirohisa; Inoue,
   Masao; Kano, Ryouhei; Kashiwase, Toshio; Nagata, Shin'ichi; Sakao,
   Taro; Shimizu, Toshifumi; Tsuneta, Saku; Yoshida, Tsuyoshi
2004JSpRo..41..868K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Development of the Solar-B X-ray telescope focal plane camera
Authors: Kano, Ryouhei; Hara, Hirohisa; Kumagai, Kazuyoshi; Sawa,
   Masaki; Tsuneta, Saku; Sakao, Taro; Matsuzaki, Keiichi
2004naoj.book....5K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Evolution of the High Temperature Corona
Authors: Kano, R.
2004cosp...35.4441K    Altcode: 2004cosp.meet.4441K
  Yohkoh meticulously observed the solar corona for more than 10 years
  from 1991 to the accidental termination in December 2001. Yohkoh
  shows that any transients, such as flares and micro-flares, are due
  to magnetic reconnection in the form of cusp or loop-loop interactions
  without exception, while the heating mechanism for the more stationary
  corona, the energy content of which is much more dominant than that
  of the transients, remains totally unknown. Hot SXT loops have the
  highest temperature and emission measure (inverted corona) near
  the loop top, while cool TRACE loops appear to have more uniform
  temperature. These hot and cool loops reflect differences in the heat
  input rate across the loops as well along the loops. The question is
  whether these loops are heated by nano-flares, and (if the answer is
  yes) how they create the multi-temperature corona as observed. Reaching
  the detection limit in the hunting of smaller and smaller events, we
  stress the importance of X-ray intensity fluctuations, which contain
  information on pico-flares. Another mystery on longer time scale is
  that the overall intensity of the quiet-Sun X-ray corona appears to
  change with solar cycle: basal heating is modulated by the magnetic
  solar cycle, while the number of X-ray bright points is surprisingly
  constant over the solar cycle against previous observations.

---------------------------------------------------------
Title: Spatial and Temporal Properties of Hot and Cool Coronal Loops
Authors: Nagata, Shin'ichi; Hara, Hirohisa; Kano, Ryouhei; Kobayashi,
   Ken; Sakao, Taro; Shimizu, Toshifumi; Tsuneta, Saku; Yoshida, Tsuyoshi;
   Gurman, Joseph B.
2003ApJ...590.1095N    Altcode:
  A suite of images from the XUV Doppler Telescope (XDT), the Yohkoh Soft
  X-ray Telescope (SXT), and the Extreme-Ultraviolet Imaging Telescope
  (EIT) on the Solar and Heliospheric Observatory (SOHO) allow us to
  see the whole (T&gt;1 MK) temperature evolution of coronal loops. The
  detailed morphological comparison of an active region shows that hot
  loops seen in SXT (T&gt;3 MK) and cool loops seen in the the EIT 195
  Å band (T~1.5 MK) are located in almost alternating manner. The
  anticoincidence of the hot and the cool loops is conserved for a
  duration much longer than the estimated cooling timescale. However, both
  hot and cool loops have counterparts in the intermediate-temperature
  images. The cross-correlation coefficients are higher for neighboring
  temperature pairs and lower for pairs with larger temperature
  differences. These results suggest that loops are not isothermal but
  rather have a differential emission measure distribution of modest but
  finite width that peaks at different temperatures for different loops.

---------------------------------------------------------
Title: The Temperature Analysis of Yohkoh/SXT Data using the CHIANTI
    Spectral Database
Authors: Shimojo, M.; Hara, H.; Kano, R.
2002mwoc.conf..419S    Altcode:
  Since the CHIANTI database for astrophysical emission line spectroscopy
  was extended to X-ray wavelengths below 50Å recently (Dere et
  al. 2000), a temperature response of YOHKOH/SXT has been able to
  calculate using the database. The functions of temperature responses of
  SXT are very important for plasma diagnostic since we usually derive
  the electron temperature of coronal plasma using the observed signal
  counts and the ratio of the temperature responses. In this paper,
  we present the properties of the SXT temperature responses which are
  calculated from the CHIANTI database and also compare them with the
  SXT temperature responses which are calculated using Mewe spectral
  databases (Mewe, et al., 1985, 1986). We calculated the filter ratios
  using CHIANTI database and compared them with the filter ratios which
  are calculated from Mewe database. At the result, it is found that
  the difference between temperatures which are derived using CHIANTI
  and Mewe database is about 2 MK around 5 MK, if we use Al and Al12
  filters for the plasma diagnostic. The result is the same as Schmelz
  et al.(1999). In the paper, we also discuss the effect of the CHIANTI
  spectral databases for previous works which used the filter ratios
  based on Mewe database.

---------------------------------------------------------
Title: High-resolution grazing incidence telescope for the Solar-B
    observatory
Authors: Golub, Leon; DeLuca, Edward E.; Bookbinder, Jay A.; Cheimets,
   Peter; Shibasaki, Kiyoto; Sakao, Taro; Kano, Ryouhei
2000SPIE.4139..313G    Altcode:
  The X-ray observations from the Yohkoh SXT provided the greatest
  step forward in our understanding of the solar corona in nearly two
  decades. We believe that the scientific objectives of the Solar-B
  mission can best be achieved with an X-ray telescope (XRT) similar to
  the SXT, but with significant improvements in spatial resolution and
  in temperature response that take into account the knowledge gained
  from Yohkoh. We present the scientific justification for this view,
  discuss the instrumental requirements that flow from the scientific
  objectives, and describe the instrumentation that will meet these
  requirements. XRT is a grazing-incidence (GI) modified Wolter I X-ray
  telescope, of 35 cm inner diameter and 2.7 m focal length. The 2048 X
  2048 back-illuminated CCD has 13.5 (mu) pixels, corresponding to 1.0
  arcsec and giving full Sun field of view. This will be the highest
  resolution GI X-ray telescope ever flown for Solar coronal studies,
  and it has been designed specifically to observe both the high and
  low temperature coronal plasma.

---------------------------------------------------------
Title: The X-ray telescope on Solar B.
Authors: Deluca, E. E.; Golub, L.; Bookbinder, J.; Cheimets, P.;
   Shibasaki, K.; Sakao, T.; Kano, R.
2000BAAS...32..827D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The X-Ray Telescope on Solar B
Authors: DeLuca, E. E.; Golub, L.; Bookbinder, J.; Cheimets, P.;
   Shibasaki, K.; Sakao, T.; Kano, R.
2000SPD....31Q0293D    Altcode:
  The X-ray observations from the Yohkoh SXT provided the greatest
  step forward in our understanding of the solar corona in nearly two
  decades. We believe that the scientific objectives of the Solar-B
  mission can best be achieved with an X-ray telescope (XRT) similar to
  the SXT, but with significant improvements in spatial resolution and in
  temperature response that take into account the knowledge gained from
  Yohkoh. We present the scientific justification for this view, discuss
  the instrumental requirements that flow from the scientific objectives,
  and describe the instrumentation to meet these requirements. XRT is
  a grazing-incidence (GI) modified Wolter I X-ray telescope, of 35cm
  inner diameter and 2.7m focal length. The 2048x2048 back-illuminated
  CCD has 13.5&amp;mu pixels, corresponding to 1.0 arcsec and giving
  full Sun field of view. This will be the highest resolution GI X-ray
  telescope ever flown for Solar coronal studies, and it has been designed
  specifically to observe both the high and low temperature coronal
  plasma. A small optical telescope provide visibles light images for
  coalignment with the Solar-B optical and EUV instruments. The US XRT
  team is support by a NASA Contract from MSFC.

---------------------------------------------------------
Title: Initial Results from the XUV Doppler Telescope
Authors: Kano, R.; Hara, H.; Kobayashi, K.; Kumagai, K.; Nagata, S.;
   Sakao, T.; Shimizu, T.; Tsuneta, S.; Yoshida, T.
2000AdSpR..25.1739K    Altcode:
  We developed a unique telescope to obtain simultaneous XUV images and
  the velocity maps by measuring the line-of-sight Doppler shifts of the
  Fe XIV 211A&amp;ring line (T = 1.8 MK): the Solar XUV Doppler Telescope
  (hereafter XDT). The telescope was launched by the Institute of Space
  and Astronautical Science with the 22nd S520 rocket on January 31,
  1998, and took 14 XUV whole sun images during 5 minutes. Simultaneous
  observations of XDT with Yohkoh (SXT), SOHO (EIT, CDS, LASCO and MDI)
  were successfully carried out. The images taken with EIT, XDT and SXT
  are able to cover the wide temperature ranging from 1 to 10 MK, and
  clearly show the multi-temperature nature of the solar corona. Indeed,
  we notice that both the cool (1-2 MK) loops observed with EIT and
  XDT, and the hot (&gt;3 MK) loops observed with SXT exist in the same
  active regions but in a spatially exclusive way. The XDT red-blue ratio
  between longer- and shorter-wavelength bands of Fe XIV 211A&amp;ring
  line indicates a possible down-flow of 1.8 MK plasma near the footpoints
  of multiple cool loops

---------------------------------------------------------
Title: Narrow-Bandpass Multilayer Mirrors for an Extreme-Ultraviolet
    Doppler Telescope
Authors: Hara, Hirohisa; Nagata, Shin'ichi; Kano, Ryouhei; Kumagai,
   Kazuyoshi; Sakao, Taro; Shimizu, Toshifumi; Tsuneta, Saku; Yoshida,
   Tsuyoshi; Ishiyama, Wakana; Oshino, Tetsuya; Murakami, Katsuhiko
1999ApOpt..38.6617H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Erratum: Temperature Distributions and Energy Scaling Law of
    Solar Coronal Loops Obtained with Yohkoh
Authors: Kano, Ryouhei; Tsuneta, Saku
1999PASJ...51..569K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The XUV Doppler Telescope (XDT)
Authors: Sakao, T.; Tsuneta, S.; Hara, H.; Shimizu, T.; Kano, R.;
   Kumagai, K.; Yoshida, T.; Nagata, S.; Kobayashi, K.
1999SoPh..187..303S    Altcode:
  We present an overview and instrumental details of the solar XUV Doppler
  Telescope (XDT) launched in January 1998 with the S520CN-22 sounding
  rocket of the Institute of Space and Astronautical Science. The XDT
  observes nearly single-temperature solar corona at 1.8 MK with angular
  resolution of ≈ 5” pixel size, together with the ability to detect
  the coronal velocity field with a full-Sun field of view. By use of
  normal incidence optics whose primary and secondary mirrors are coated
  with multilayer materials in two sectors, the XDT takes images of the
  Sun in a set of shorter and longer wavelength bands around the Fe xiv
  211.3 Å emission line. Summation of a pair of images in the two bands
  provides an image of the 1.8 MK-corona while the difference between
  the two provides velocity images of the Fe xiv-emitting plasma. A brief
  description on the observation sequence together with the flight result
  is also given.

---------------------------------------------------------
Title: Development and flight performance of tip-tilt mirror system
    for a sounding rocket observation of the Sun.
Authors: Shimizu, T.; Yoshida, T.; Tsuneta, S.; Sakao, T.; Kano,
   R.; Hara, H.; Nagata, S.; Kodeki, K.; Inoue, M.; Fukushima, K.;
   Kashiwase, T.
1999RNAOJ...4...43S    Altcode: 1999RNOAJ...4...43S
  A tip-tilt mirror (TTM) system was developed for the XUV Doppler
  telescope (XDT) on board an ISAS sounding rocket. The spatial resolution
  of the telescope is about 5″ whereas the pointing stability is
  only ±0.3° with the rocket pointing control system. To achieve
  better than 5″stability on the focal plane of the telescope, the
  TTM system controls the tilt of the secondary mirror with fixed-coil
  magnetic actuators. The control signal to stabilize focal-plane images
  is supplied by the position-sensitive detector (PSD) of a pin-hole
  telescope equipped inside XDT. Closed-loop controls are made with
  the on-board software on the DSP processor. The sounding rocket was
  successfully launched on 31 January 1998 from the Kagoshima Space
  Center of ISAS. TTM worked perfectly during the flight, and achieved
  better than 5″stability on the focal plane during CCD exposures.

---------------------------------------------------------
Title: Development of the tip-tilt mirror system for the solar
    XUV telescope
Authors: Kodeki, Kazuhide; Fukushima, Kazuhiko; Kashiwase, Toshio;
   Inoue, Masao; Shimizu, Toshifumi; Yoshida, Tsuyoshi; Sakao, Taro;
   Hara, Hirohisa; Nagata, Shin'ichi; Kano, Ryouhei; Tsuneta, Saku
1998SPIE.3356..922K    Altcode:
  This paper describes the design and prelaunch performance of the
  tip-tilt mirror (TTM) system developed for the XUV Cassegrain telescope
  aboard the ISAS sounding rocket experiment. The spatial resolution
  of the telescope is about 5 arcsec, whereas the rocket pointing is
  only controlled to be within +/- 0.5 degree around the target without
  stability control. The TTM is utilized to stabilize the XUV image
  on the focal planes by tilting the secondary mirror with two-axes
  fixed-coil type actuators. The two position- sensitive detectors in
  the telescope optics and in the TTM mechanical structure from the
  normal and local closed-loop modes. The TTM has four grain modes with
  automatic transition among the modes. The low gain mode is used in
  the initial acquisition, and in case the TTM loses the tracking. The
  high gain mode is used in the normal tracking mode. This arrangement
  provides us with the wide initial acquisition angle with single TTM
  system as well as the high pointing accuracy once the tracking is
  established. The TTM has a launch-lock mechanism against the launch
  vibration of 16G. The closed-loop control with command and telemetry
  interface is done by the flight software against the launch vibration
  of 16G. The closed-loop control with command and telemetry interface
  is done by the flight software on the DSP processor. The use of the
  fast processor brings in the significant reduction in the weight and
  size of the control- electronics, more flexible control system, and
  shorter design and testing period.

---------------------------------------------------------
Title: XUV Doppler Telescope Aboard Sounding Rocket
Authors: Yoshida, T.; Kano, R.; Nagata, S.; Hara, H.; Sakao, T.;
   Shimizu, T.; Tsuneta, S.
1998ASSL..229..383Y    Altcode: 1998opaf.conf..383Y
  No abstract at ADS