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Author name code: mclaughlin
ADS astronomy entries on 2022-09-14
author:"McLaughlin, James A." 

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Title: Observations of Instability-driven Nanojets in Coronal Loops
Authors: Sukarmadji, A. Ramada C.; Antolin, Patrick; McLaughlin,
   James A.
2022ApJ...934..190S    Altcode: 2022arXiv220210960S
  The recent discovery of nanojets by Antolin et al. represents
  magnetic reconnection in a braided field, thus clearly identifying
  reconnection-driven nanoflares. Due to their small scale (500 km
  in width, 1500 km in length) and short timescales (<15 s), it is
  unclear how pervasive nanojets are in the solar corona. In this paper,
  we present Interface Region Imaging Spectrograph and Solar Dynamics
  Observatory observations of nanojets found in multiple coronal
  structures, namely, in a coronal loop powered by a blowout jet,
  and in two other coronal loops with coronal rain. In agreement with
  previous findings, we observe that nanojets are accompanied by small
  nanoflare-like intensity bursts in the (E)UV, have velocities of 150-250
  km s<SUP>-1</SUP> and occur transversely to the field line of origin,
  which is sometimes observed to split. However, we find a variety of
  nanojet directions in the plane transverse to the loop axis. These
  nanojets are found to have kinetic and thermal energies within the
  nanoflare range, and often occur in clusters. In the blowout jet case
  study, the Kelvin-Helmholtz instability (KHI) is directly identified
  as the reconnection driver. For the other two loops, we find that
  both, KHI and Rayleigh-Taylor instability (RTI) are likely to be the
  drivers. However, we find that KHI and RTI are each more likely in one
  of the other two cases. These observations of nanojets in a variety
  of structures and environments support nanojets being a general result
  of reconnection that are driven here by dynamic instabilities.

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Title: The Independence of Oscillatory Reconnection Periodicity from
    the Initial Pulse
Authors: Karampelas, Konstantinos; McLaughlin, James A.; Botha,
   Gert J. J.; Régnier, Stéphane
2022ApJ...933..142K    Altcode: 2022arXiv220701980K
  Oscillatory reconnection can manifest through the interaction between
  the ubiquitous MHD waves and omnipresent null points in the solar
  atmosphere and is characterized by an inherent periodicity. In the
  current study, we focus on the relationship between the period
  of oscillatory reconnection and the strength of the wave pulse
  initially perturbing the null point, in a hot coronal plasma. We
  use the PLUTO code to solve the fully compressive, resistive MHD
  equations for a 2D magnetic X-point. Using wave pulses with a wide
  range of amplitudes, we perform a parameter study to obtain values
  for the period, considering the presence and absence of anisotropic
  thermal conduction separately. In both cases, we find that the
  resulting period is independent of the strength of the initial
  perturbation. The addition of anisotropic thermal conduction only
  leads to an increase in the mean value for the period, in agreement
  with our previous study. We also consider a different type of initial
  driver and we obtain an oscillation period matching the independent
  trend previously mentioned. Thus, we report for the first time on
  the independence between the type and strength of the initializing
  wave pulse and the resulting period of oscillatory reconnection in a
  hot coronal plasma. This makes oscillatory reconnection a promising
  mechanism to be used within the context of coronal seismology.

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Title: Oscillatory Reconnection of a 2D X-point in a hot coronal
    plasma
Authors: Karampelas, Konstantinos; Botha, Gert J. J.; Regnier,
   Stephane; Mclaughlin, James A.
2022cosp...44.2559K    Altcode:
  Oscillatory reconnection (a relaxation mechanism with periodic changes
  in connectivity) has been proposed as a potential physical mechanism
  underpinning several periodic phenomena in the solar atmosphere
  including, but not limited to, quasi-periodic pulsations (QPPs)
  and flows. In the past, this mechanism had been extensively studied
  numerically for 2D and 3D simulations of null points in cold plasma. In
  our latest studies, we have expanded our understanding of oscillatory
  reconnection, by considering for the first time hot, coronal plasma. We
  will be presenting our latest results, from numerically solving the
  fully-compressive, resistive MHD equations for a 2D magnetic X-point
  under coronal conditions using the PLUTO code. We report on the
  resulting oscillatory reconnection including its periodicity and decay
  rate, by tracking the evolution of the current density profile at the
  null point. We also consider, for the first time, the effect of adding
  anisotropic thermal conduction to the mechanism, and how it simplifies
  the spectrum of the oscillation profile and increases its decay rate,
  while still allowing the mechanism to manifest. Finally, we reveal how
  the equilibrium magnetic field strength, density distribution and the
  amplitude of the initial perturbation relate to the decay rate, and
  period of oscillatory reconnection, opening the tantalising possibility
  of utilizing oscillatory reconnection as a seismological tool.

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Title: Using Oscillatory Reconnection of a 2D X-point as a tool for
    coronal seismology.
Authors: Karampelas, Konstantinos; Botha, Gert J. J.; Regnier,
   Stephane; Mclaughlin, James A.
2022cosp...44.2487K    Altcode:
  The mechanism of oscillatory reconnection of a null point has been
  one of the proposed mechanisms behind phenomena like quasi-periodic
  pulsations (QPPs). The manifestation of this mechanism through the
  interaction of the ubiquitous waves with null points in the solar
  atmosphere opens the possibility of utilizing oscillatory reconnection
  as a tool for coronal seismology. In the past, the first steps had
  been taken, by connecting the length of the initial current sheet
  with the period of oscillatory reconnection, and by identifying a
  linear regime where the period is affected by resistivity. Our recent
  numerical studies have expanded upon these findings, by considering
  plasma at coronal conditions, with the addition of anisotropic
  thermal conduction. We have performed a series of parameter studies
  with the use of the PLUTO code, which reveal a relation between the
  equilibrium magnetic field strength and density distribution with
  the period and decay rate of oscillatory reconnection. In addition,
  we see an independence of the oscillation period from the type and
  strength of the external wave pulse, which perturbs the null from its
  initial equilibrium state. This allows us to formulate an empirical
  formula connecting these four quantities, opening the way in using
  oscillatory reconnection for coronal seismology.

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Title: First Dark Matter Search Results from the LUX-ZEPLIN (LZ)
    Experiment
Authors: Aalbers, J.; Akerib, D. S.; Akerlof, C. W.; Al Musalhi,
   A. K.; Alder, F.; Alqahtani, A.; Alsum, S. K.; Amarasinghe, C. S.;
   Ames, A.; Anderson, T. J.; Angelides, N.; Araújo, H. M.; Armstrong,
   J. E.; Arthurs, M.; Azadi, S.; Bailey, A. J.; Baker, A.; Balajthy, J.;
   Balashov, S.; Bang, J.; Bargemann, J. W.; Barry, M. J.; Barthel, J.;
   Bauer, D.; Baxter, A.; Beattie, K.; Belle, J.; Beltrame, P.; Bensinger,
   J.; Benson, T.; Bernard, E. P.; Bhatti, A.; Biekert, A.; Biesiadzinski,
   T. P.; Birch, H. J.; Birrittella, B.; Blockinger, G. M.; Boast, K. E.;
   Boxer, B.; Bramante, R.; Brew, C. A. J.; Brás, P.; Buckley, J. H.;
   Bugaev, V. V.; Burdin, S.; Busenitz, J. K.; Buuck, M.; Cabrita, R.;
   Carels, C.; Carlsmith, D. L.; Carlson, B.; Carmona-Benitez, M. C.;
   Cascella, M.; Chan, C.; Chawla, A.; Chen, H.; Cherwinka, J. J.; Chott,
   N. I.; Cole, A.; Coleman, J.; Converse, M. V.; Cottle, A.; Cox, G.;
   Craddock, W. W.; Creaner, O.; Curran, D.; Currie, A.; Cutter, J. E.;
   Dahl, C. E.; David, A.; Davis, J.; Davison, T. J. R.; Delgaudio, J.;
   Dey, S.; de Viveiros, L.; Dobi, A.; Dobson, J. E. Y.; Druszkiewicz,
   E.; Dushkin, A.; Edberg, T. K.; Edwards, W. R.; Elnimr, M. M.; Emmet,
   W. T.; Eriksen, S. R.; Faham, C. H.; Fan, A.; Fayer, S.; Fearon,
   N. M.; Fiorucci, S.; Flaecher, H.; Ford, P.; Francis, V. B.; Fraser,
   E. D.; Fruth, T.; Gaitskell, R. J.; Gantos, N. J.; Garcia, D.; Geffre,
   A.; Gehman, V. M.; Genovesi, J.; Ghag, C.; Gibbons, R.; Gibson, E.;
   Gilchriese, M. G. D.; Gokhale, S.; Gomber, B.; Green, J.; Greenall,
   A.; Greenwood, S.; van der Grinten, M. G. D.; Gwilliam, C. B.; Hall,
   C. R.; Hans, S.; Hanzel, K.; Harrison, A.; Hartigan-O'Connor, E.;
   Haselschwardt, S. J.; Hertel, S. A.; Heuermann, G.; Hjemfelt, C.; Hoff,
   M. D.; Holtom, E.; Y-K. Hor, J.; Horn, M.; Huang, D. Q.; Hunt, D.;
   Ignarra, C. M.; Jacobsen, R. G.; Jahangir, O.; James, R. S.; Jeffery,
   S. N.; Ji, W.; Johnson, J.; Kaboth, A. C.; Kamaha, A. C.; Kamdin, K.;
   Kasey, V.; Kazkaz, K.; Keefner, J.; Khaitan, D.; Khaleeq, M.; Khazov,
   A.; Khurana, I.; Kim, Y. D.; Kocher, C. D.; Kodroff, D.; Korley, L.;
   Korolkova, E. V.; Kras, J.; Kraus, H.; Kravitz, S.; Krebs, H. J.;
   Kreczko, L.; Krikler, B.; Kudryavtsev, V. A.; Kyre, S.; Landerud, B.;
   Leason, E. A.; Lee, C.; Lee, J.; Leonard, D. S.; Leonard, R.; Lesko,
   K. T.; Levy, C.; Li, J.; Liao, F. -T.; Liao, J.; Lin, J.; Lindote, A.;
   Linehan, R.; Lippincott, W. H.; Liu, R.; Liu, X.; Liu, Y.; Loniewski,
   C.; Lopes, M. I.; Lopez Asamar, E.; López Paredes, B.; Lorenzon, W.;
   Lucero, D.; Luitz, S.; Lyle, J. M.; Majewski, P. A.; Makkinje, J.;
   Malling, D. C.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou,
   N.; Marzioni, M. F.; Maupin, C.; McCarthy, M. E.; McConnell, C. T.;
   McKinsey, D. N.; McLaughlin, J.; Meng, Y.; Migneault, J.; Miller,
   E. H.; Mizrachi, E.; Mock, J. A.; Monte, A.; Monzani, M. E.; Morad,
   J. A.; Morales Mendoza, J. D.; Morrison, E.; Mount, B. J.; Murdy,
   M.; Murphy, A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.; Nehrkorn,
   C.; Nelson, H. N.; Neves, F.; Nguyen, A.; Nikoleyczik, J. A.; Nilima,
   A.; O'Dell, J.; O'Neill, F. G.; O'Sullivan, K.; Olcina, I.; Olevitch,
   M. A.; Oliver-Mallory, K. C.; Orpwood, J.; Pagenkopf, D.; Pal, S.;
   Palladino, K. J.; Palmer, J.; Pangilinan, M.; Parveen, N.; Patton,
   S. J.; Pease, E. K.; Penning, B.; Pereira, C.; Pereira, G.; Perry,
   E.; Pershing, T.; Peterson, I. B.; Piepke, A.; Podczerwinski, J.;
   Porzio, D.; Powell, S.; Preece, R. M.; Pushkin, K.; Qie, Y.; Ratcliff,
   B. N.; Reichenbacher, J.; Reichhart, L.; Rhyne, C. A.; Richards, A.;
   Riffard, Q.; Rischbieter, G. R. C.; Rodrigues, J. P.; Rodriguez, A.;
   Rose, H. J.; Rosero, R.; Rossiter, P.; Rushton, T.; Rutherford, G.;
   Rynders, D.; Saba, J. S.; Santone, D.; Sazzad, A. B. M. R.; Schnee,
   R. W.; Scovell, P. R.; Seymour, D.; Shaw, S.; Shutt, T.; Silk, J. J.;
   Silva, C.; Sinev, G.; Skarpaas, K.; Skulski, W.; Smith, R.; Solmaz,
   M.; Solovov, V. N.; Sorensen, P.; Soria, J.; Stancu, I.; Stark, M. R.;
   Stevens, A.; Stiegler, T. M.; Stifter, K.; Studley, R.; Suerfu, B.;
   Sumner, T. J.; Sutcliffe, P.; Swanson, N.; Szydagis, M.; Tan, M.;
   Taylor, D. J.; Taylor, R.; Taylor, W. C.; Temples, D. J.; Tennyson,
   B. P.; Terman, P. A.; Thomas, K. J.; Tiedt, D. R.; Timalsina, M.; To,
   W. H.; Tomás, A.; Tong, Z.; Tovey, D. R.; Tranter, J.; Trask, M.;
   Tripathi, M.; Tronstad, D. R.; Tull, C. E.; Turner, W.; Tvrznikova,
   L.; Utku, U.; Va'vra, J.; Vacheret, A.; Vaitkus, A. C.; Verbus, J. R.;
   Voirin, E.; Waldron, W. L.; Wang, A.; Wang, B.; Wang, J. J.; Wang,
   W.; Wang, Y.; Watson, J. R.; Webb, R. C.; White, A.; White, D. T.;
   White, J. T.; White, R. G.; Whitis, T. J.; Williams, M.; Wisniewski,
   W. J.; Witherell, M. S.; Wolfs, F. L. H.; Wolfs, J. D.; Woodford, S.;
   Woodward, D.; Worm, S. D.; Wright, C. J.; Xia, Q.; Xiang, X.; Xiao,
   Q.; Xu, J.; Yeh, M.; Yin, J.; Young, I.; Zarzhitsky, P.; Zuckerman,
   A.; Zweig, E. A.
2022arXiv220703764A    Altcode:
  The LUX-ZEPLIN (LZ) experiment is a dark matter detector centered on
  a dual-phase xenon time projection chamber operating at the Sanford
  Underground Research Facility in Lead, South Dakota, USA. This Letter
  reports results from LZ's first search for Weakly Interacting Massive
  Particles (WIMPs) with an exposure of 60 live days using a fiducial
  mass of 5.5 t. A profile-likelihood ratio analysis shows the data to
  be consistent with a background-only hypothesis, setting new limits
  on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and
  spin-dependent WIMP-proton cross-sections for WIMP masses above 9
  GeV/c$^2$. The most stringent limit is set at 30 GeV/c$^2$, excluding
  cross sections above 5.9$\times 10^{-48}$ cm$^2$ at the 90\% confidence
  level.

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Title: Cosmogenic production of <SUP>37</SUP>Ar in the context of
    the LUX-ZEPLIN experiment
Authors: Aalbers, J.; Akerib, D. S.; Al Musalhi, A. K.; Alder, F.;
   Alsum, S. K.; Amarasinghe, C. S.; Ames, A.; Anderson, T. J.; Angelides,
   N.; Araújo, H. M.; Armstrong, J. E.; Arthurs, M.; Bai, X.; Baker,
   A.; Balajthy, J.; Balashov, S.; Bang, J.; Bargemann, J. W.; Bauer,
   D.; Baxter, A.; Beattie, K.; Bernard, E. P.; Bhatti, A.; Biekert, A.;
   Biesiadzinski, T. P.; Birch, H. J.; Blockinger, G. M.; Bodnia, E.;
   Boxer, B.; Brew, C. A. J.; Brás, P.; Burdin, S.; Busenitz, J. K.;
   Buuck, M.; Cabrita, R.; Carmona-Benitez, M. C.; Cascella, M.; Chan,
   C.; Chawla, A.; Chen, H.; Chott, N. I.; Cole, A.; Converse, M. V.;
   Cottle, A.; Cox, G.; Creaner, O.; Cutter, J. E.; Dahl, C. E.; David,
   A.; de Viveiros, L.; Dobson, J. E. Y.; Druszkiewicz, E.; Eriksen,
   S. R.; Fan, A.; Fayer, S.; Fearon, N. M.; Fiorucci, S.; Flaecher,
   H.; Fraser, E. D.; Fruth, T.; Gaitskell, R. J.; Genovesi, J.; Ghag,
   C.; Gibson, E.; Gilchriese, M. G. D.; Gokhale, S.; van der Grinten,
   M. G. D.; Gwilliam, C. B.; Hall, C. R.; Haselschwardt, S. J.; Hertel,
   S. A.; Horn, M.; Huang, D. Q.; Hunt, D.; Ignarra, C. M.; Jahangir,
   O.; James, R. S.; Ji, W.; Johnson, J.; Kaboth, A. C.; Kamaha, A. C.;
   Kamdin, K.; Khaitan, D.; Khazov, A.; Khurana, I.; Kodroff, D.; Korley,
   L.; Korolkova, E. V.; Kraus, H.; Kravitz, S.; Kreczko, L.; Kudryavtsev,
   V. A.; Leason, E. A.; Leonard, D. S.; Lesko, K. T.; Levy, C.; Lee,
   J.; Lin, J.; Lindote, A.; Linehan, R.; Lippincott, W. H.; Liu, X.;
   Lopes, M. I.; Lopez Asamar, E.; Lopez-Paredes, B.; Lorenzon, W.;
   Luitz, S.; Majewski, P. A.; Manalaysay, A.; Manenti, L.; Mannino,
   R. L.; Marangou, N.; McCarthy, M. E.; McKinsey, D. N.; McLaughlin,
   J.; Miller, E. H.; Mizrachi, E.; Monte, A.; Monzani, M. E.; Morad,
   J. A.; Morales Mendoza, J. D.; Morrison, E.; Mount, B. J.; Murphy,
   A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.; Nelson, H. N.; Neves, F.;
   Nikoleyczik, J. A.; Nilima, A.; Olcina, I.; Oliver-Mallory, K.; Pal,
   S.; Palladino, K. J.; Palmer, J.; Parveen, N.; Patton, S. J.; Pease,
   E. K.; Penning, B.; Pereira, G.; Perry, E.; Pershing, J.; Piepke, A.;
   Porzio, D.; Qie, Y.; Reichenbacher, J.; Rhyne, C. A.; Richards, A.;
   Riffard, Q.; Rischbieter, G. R. C.; Rosero, R.; Rossiter, P.; Rushton,
   T.; Santone, D.; Sazzad, A. B. M. R.; Schnee, R. W.; Scovell, P. R.;
   Shaw, S.; Shutt, T. A.; Silk, J. J.; Silva, C.; Sinev, G.; Smith,
   R.; Solmaz, M.; Solovov, V. N.; Sorensen, P.; Soria, J.; Stancu, I.;
   Stevens, A.; Stifter, K.; Suerfu, B.; Sumner, T. J.; Swanson, N.;
   Szydagis, M.; Taylor, W. C.; Taylor, R.; Temples, D. J.; Terman,
   P. A.; Tiedt, D. R.; Timalsina, M.; To, W. H.; Tong, Z.; Tovey,
   D. R.; Trask, M.; Tripathi, M.; Tronstad, D. R.; Turner, W.; Utku,
   U.; Vaitkus, A.; Wang, B.; Wang, Y.; Wang, J. J.; Wang, W.; Watson,
   J. R.; Webb, R. C.; White, R. G.; Whitis, T. J.; Williams, M.; Wolfs,
   F. L. H.; Woodford, S.; Woodward, D.; Wright, C. J.; Xia, Q.; Xiang,
   X.; Xu, J.; Yeh, M.; Lux-Zeplin Collaboration
2022PhRvD.105h2004A    Altcode: 2022arXiv220102858A
  We estimate the amount of <SUP>37</SUP>Ar produced in natural xenon
  via cosmic-ray-induced spallation, an inevitable consequence of the
  transportation and storage of xenon on the Earth's surface. We then
  calculate the resulting <SUP>37</SUP>Ar concentration in a 10-tonne
  payload (similar to that of the LUX-ZEPLIN experiment) assuming a
  representative schedule of xenon purification, storage, and delivery
  to the underground facility. Using the spallation model by Silberberg
  and Tsao, the sea-level production rate of <SUP>37</SUP>Ar in natural
  xenon is estimated to be 0.024 atoms /kg /day . Assuming the xenon is
  successively purified to remove radioactive contaminants in 1-tonne
  batches at a rate of 1 tonne /month , the average <SUP>37</SUP>Ar
  activity after 10 tons are purified and transported underground is
  0.058 −0.090 μ Bq /kg , depending on the degree of argon removal
  during above-ground purification. Such cosmogenic <SUP>37</SUP>Ar
  will appear as a noticeable background in the early science data,
  while decaying with a 35-day half-life. This newly noticed production
  mechanism of <SUP>37</SUP>Ar should be considered when planning for
  future liquid-xenon-based experiments.

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Title: Novel Data Analysis Techniques in Coronal Seismology
Authors: Anfinogentov, Sergey A.; Antolin, Patrick; Inglis, Andrew
   R.; Kolotkov, Dmitrii; Kupriyanova, Elena G.; McLaughlin, James A.;
   Nisticò, Giuseppe; Pascoe, David J.; Krishna Prasad, S.; Yuan, Ding
2022SSRv..218....9A    Altcode: 2021arXiv211213577A
  We review novel data analysis techniques developed or adapted for
  the field of coronal seismology. We focus on methods from the last
  ten years that were developed for extreme ultraviolet (EUV) imaging
  observations of the solar corona, as well as for light curves from
  radio and X-ray. The review covers methods for the analysis of
  transverse and longitudinal waves; spectral analysis of oscillatory
  signals in time series; automated detection and processing of large
  data sets; empirical mode decomposition; motion magnification;
  and reliable detection, including the most common pitfalls causing
  artefacts and false detections. We also consider techniques for the
  detailed investigation of MHD waves and seismological inference of
  physical parameters of the coronal plasma, including restoration of
  the three-dimensional geometry of oscillating coronal loops, forward
  modelling and Bayesian parameter inference.

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Title: A Next-Generation Liquid Xenon Observatory for Dark Matter
    and Neutrino Physics
Authors: Aalbers, J.; Abe, K.; Aerne, V.; Agostini, F.; Maouloud,
   S. Ahmed; Akerib, D. S.; Akimov, D. Yu.; Akshat, J.; Al Musalhi, A. K.;
   Alder, F.; Alsum, S. K.; Althueser, L.; Amarasinghe, C. S.; Amaro,
   F. D.; Ames, A.; Anderson, T. J.; Andrieu, B.; Angelides, N.; Angelino,
   E.; Angevaare, J.; Antochi, V. C.; Antón Martin, D.; Antunovic, B.;
   Aprile, E.; Araújo, H. M.; Armstrong, J. E.; Arneodo, F.; Arthurs,
   M.; Asadi, P.; Baek, S.; Bai, X.; Bajpai, D.; Baker, A.; Balajthy, J.;
   Balashov, S.; Balzer, M.; Bandyopadhyay, A.; Bang, J.; Barberio, E.;
   Bargemann, J. W.; Baudis, L.; Bauer, D.; Baur, D.; Baxter, A.; Baxter,
   A. L.; Bazyk, M.; Beattie, K.; Behrens, J.; Bell, N. F.; Bellagamba,
   L.; Beltrame, P.; Benabderrahmane, M.; Bernard, E. P.; Bertone,
   G. F.; Bhattacharjee, P.; Bhatti, A.; Biekert, A.; Biesiadzinski,
   T. P.; Binau, A. R.; Biondi, R.; Biondi, Y.; Birch, H. J.; Bishara,
   F.; Bismark, A.; Blanco, C.; Blockinger, G. M.; Bodnia, E.; Boehm,
   C.; Bolozdynya, A. I.; Bolton, P. D.; Bottaro, S.; Bourgeois, C.;
   Boxer, B.; Brás, P.; Breskin, A.; Breur, P. A.; Brew, C. A. J.;
   Brod, J.; Brookes, E.; Brown, A.; Brown, E.; Bruenner, S.; Bruno,
   G.; Budnik, R.; Bui, T. K.; Burdin, S.; Buse, S.; Busenitz, J. K.;
   Buttazzo, D.; Buuck, M.; Buzulutskov, A.; Cabrita, R.; Cai, C.; Cai,
   D.; Capelli, C.; Cardoso, J. M. R.; Carmona-Benitez, M. C.; Cascella,
   M.; Catena, R.; Chakraborty, S.; Chan, C.; Chang, S.; Chauvin, A.;
   Chawla, A.; Chen, H.; Chepel, V.; Chott, N. I.; Cichon, D.; Cimental
   Chavez, A.; Cimmino, B.; Clark, M.; Co, R. T.; Colijn, A. P.; Conrad,
   J.; Converse, M. V.; Costa, M.; Cottle, A.; Cox, G.; Creaner, O.;
   Cuenca Garcia, J. J.; Cussonneau, J. P.; Cutter, J. E.; Dahl, C. E.;
   D'Andrea, V.; David, A.; Decowski, M. P.; Dent, J. B.; Deppisch,
   F. F.; de Viveiros, L.; Di Gangi, P.; Di Giovanni, A.; Di Pede, S.;
   Dierle, J.; Diglio, S.; Dobson, J. E. Y.; Doerenkamp, M.; Douillet,
   D.; Drexlin, G.; Druszkiewicz, E.; Dunsky, D.; Eitel, K.; Elykov, A.;
   Emken, T.; Engel, R.; Eriksen, S. R.; Fairbairn, M.; Fan, A.; Fan,
   J. J.; Farrell, S. J.; Fayer, S.; Fearon, N. M.; Ferella, A.; Ferrari,
   C.; Fieguth, A.; Fieguth, A.; Fiorucci, S.; Fischer, H.; Flaecher,
   H.; Flierman, M.; Florek, T.; Foot, R.; Fox, P. J.; Franceschini,
   R.; Fraser, E. D.; Frenk, C. S.; Frohlich, S.; Fruth, T.; Fulgione,
   W.; Fuselli, C.; Gaemers, P.; Gaior, R.; Gaitskell, R. J.; Galloway,
   M.; Gao, F.; Garcia Garcia, I.; Genovesi, J.; Ghag, C.; Ghosh, S.;
   Gibson, E.; Gil, W.; Giovagnoli, D.; Girard, F.; Glade-Beucke, R.;
   Glück, F.; Gokhale, S.; de Gouvêa, A.; Gráf, L.; Grandi, L.; Grigat,
   J.; Grinstein, B.; van der Grinten, M. G. D.; Grössle, R.; Guan, H.;
   Guida, M.; Gumbsheimer, R.; Gwilliam, C. B.; Hall, C. R.; Hall, L. J.;
   Hammann, R.; Han, K.; Hannen, V.; Hansmann-Menzemer, S.; Harata,
   R.; Hardin, S. P.; Hardy, E.; Hardy, C. A.; Harigaya, K.; Harnik,
   R.; Haselschwardt, S. J.; Hernandez, M.; Hertel, S. A.; Higuera,
   A.; Hils, C.; Hochrein, S.; Hoetzsch, L.; Hoferichter, M.; Hood, N.;
   Hooper, D.; Horn, M.; Howlett, J.; Huang, D. Q.; Huang, Y.; Hunt, D.;
   Iacovacci, M.; Iaquaniello, G.; Ide, R.; Ignarra, C. M.; Iloglu, G.;
   Itow, Y.; Jacquet, E.; Jahangir, O.; Jakob, J.; James, R. S.; Jansen,
   A.; Ji, W.; Ji, X.; Joerg, F.; Johnson, J.; Joy, A.; Kaboth, A. C.;
   Kamaha, A. C.; Kanezaki, K.; Kar, K.; Kara, M.; Kato, N.; Kavrigin,
   P.; Kazama, S.; Keaveney, A. W.; Kellerer, J.; Khaitan, D.; Khazov,
   A.; Khundzakishvili, G.; Khurana, I.; Kilminster, B.; Kleifges, M.;
   Ko, P.; Kobayashi, M.; Kobayashi, M.; Kodroff, D.; Koltmann, G.;
   Kopec, A.; Kopmann, A.; Kopp, J.; Korley, L.; Kornoukhov, V. N.;
   Korolkova, E. V.; Kraus, H.; Krauss, L. M.; Kravitz, S.; Kreczko,
   L.; Kudryavtsev, V. A.; Kuger, F.; Kumar, J.; López Paredes, B.;
   LaCascio, L.; Laine, Q.; Landsman, H.; Lang, R. F.; Leason, E. A.;
   Lee, J.; Leonard, D. S.; Lesko, K. T.; Levinson, L.; Levy, C.; Li,
   I.; Li, S. C.; Li, T.; Liang, S.; Liebenthal, C. S.; Lin, J.; Lin,
   Q.; Lindemann, S.; Lindner, M.; Lindote, A.; Linehan, R.; Lippincott,
   W. H.; Liu, X.; Liu, K.; Liu, J.; Loizeau, J.; Lombardi, F.; Long,
   J.; Lopes, M. I.; Lopez Asamar, E.; Lorenzon, W.; Lu, C.; Luitz, S.;
   Ma, Y.; Machado, P. A. N.; Macolino, C.; Maeda, T.; Mahlstedt, J.;
   Majewski, P. A.; Manalaysay, A.; Mancuso, A.; Manenti, L.; Manfredini,
   A.; Mannino, R. L.; Marangou, N.; March-Russell, J.; Marignetti, F.;
   Marrodán Undagoitia, T.; Martens, K.; Martin, R.; Martinez-Soler,
   I.; Masbou, J.; Masson, D.; Masson, E.; Mastroianni, S.; Mastronardi,
   M.; Matias-Lopes, J. A.; McCarthy, M. E.; McFadden, N.; McGinness,
   E.; McKinsey, D. N.; McLaughlin, J.; McMichael, K.; Meinhardt, P.;
   Menéndez, J.; Meng, Y.; Messina, M.; Midha, R.; Milisavljevic, D.;
   Miller, E. H.; Milosevic, B.; Milutinovic, S.; Mitra, S. A.; Miuchi,
   K.; Mizrachi, E.; Mizukoshi, K.; Molinario, A.; Monte, A.; Monteiro,
   C. M. B.; Monzani, M. E.; Moore, J. S.; Morå, K.; Morad, J. A.;
   Morales Mendoza, J. D.; Moriyama, S.; Morrison, E.; Morteau, E.;
   Mosbacher, Y.; Mount, B. J.; Mueller, J.; Murphy, A. St. J.; Murra,
   M.; Naim, D.; Nakamura, S.; Nash, E.; Navaieelavasani, N.; Naylor,
   A.; Nedlik, C.; Nelson, H. N.; Neves, F.; Newstead, J. L.; Ni, K.;
   Nikoleyczik, J. A.; Niro, V.; Oberlack, U. G.; Obradovic, M.; Odgers,
   K.; O'Hare, C. A. J.; Oikonomou, P.; Olcina, I.; Oliver-Mallory, K.;
   Oranday, A.; Orpwood, J.; Ostrovskiy, I.; Ozaki, K.; Paetsch, B.; Pal,
   S.; Palacio, J.; Palladino, K. J.; Palmer, J.; Panci, P.; Pandurovic,
   M.; Parlati, A.; Parveen, N.; Patton, S. J.; Pěč, V.; Pellegrini,
   Q.; Penning, B.; Pereira, G.; Peres, R.; Perez-Gonzalez, Y.; Perry, E.;
   Pershing, T.; Petrossian-Byrne, R.; Pienaar, J.; Piepke, A.; Pieramico,
   G.; Pierre, M.; Piotter, M.; Pizella, V.; Plante, G.; Pollmann, T.;
   Porzio, D.; Qi, J.; Qie, Y.; Qin, J.; Raj, N.; Rajado Silva, M.;
   Ramanathan, K.; Ramírez García, D.; Ravanis, J.; Redard-Jacot, L.;
   Redigolo, D.; Reichard, S.; Reichenbacher, J.; Rhyne, C. A.; Richards,
   A.; Riffard, Q.; Rischbieter, G. R. C.; Rocchetti, A.; Rosenfeld,
   S. L.; Rosero, R.; Rupp, N.; Rushton, T.; Saha, S.; Sanchez, L.;
   Sanchez-Lucas, P.; Santone, D.; dos Santos, J. M. F.; Sarnoff,
   I.; Sartorelli, G.; Sazzad, A. B. M. R.; Scheibelhut, M.; Schnee,
   R. W.; Schrank, M.; Schreiner, J.; Schulte, P.; Schulte, D.; Schulze
   Eissing, H.; Schumann, M.; Schwemberger, T.; Schwenk, A.; Schwetz,
   T.; Scotto Lavina, L.; Scovell, P. R.; Sekiya, H.; Selvi, M.; Semenov,
   E.; Semeria, F.; Shagin, P.; Shaw, S.; Shi, S.; Shockley, E.; Shutt,
   T. A.; Si-Ahmed, R.; Silk, J. J.; Silva, C.; Silva, M. C.; Simgen, H.;
   Šimkovic, F.; Sinev, G.; Singh, R.; Skulski, W.; Smirnov, J.; Smith,
   R.; Solmaz, M.; Solovov, V. N.; Sorensen, P.; Soria, J.; Sparmann,
   T. J.; Stancu, I.; Steidl, M.; Stevens, A.; Stifter, K.; Strigari,
   L. E.; Subotic, D.; Suerfu, B.; Suliga, A. M.; Sumner, T. J.; Szabo,
   P.; Szydagis, M.; Takeda, A.; Takeuchi, Y.; Tan, P. -L.; Taricco, C.;
   Taylor, W. C.; Temples, D. J.; Terliuk, A.; Terman, P. A.; Thers,
   D.; Thieme, K.; Thümmler, Th.; Tiedt, D. R.; Timalsina, M.; To,
   W. H.; Toennies, F.; Tong, Z.; Toschi, F.; Tovey, D. R.; Tranter, J.;
   Trask, M.; Trinchero, G. C.; Tripathi, M.; Tronstad, D. R.; Trotta,
   R.; Tsai, Y. D.; Tunnell, C. D.; Turner, W. G.; Ueno, R.; Urquijo,
   P.; Utku, U.; Vaitkus, A.; Valerius, K.; Vassilev, E.; Vecchi, S.;
   Velan, V.; Vetter, S.; Vincent, A. C.; Vittorio, L.; Volta, G.;
   von Krosigk, B.; von Piechowski, M.; Vorkapic, D.; Wagner, C. E. M.;
   Wang, A. M.; Wang, B.; Wang, Y.; Wang, W.; Wang, J. J.; Wang, L. -T.;
   Wang, M.; Wang, Y.; Watson, J. R.; Wei, Y.; Weinheimer, C.; Weisman,
   E.; Weiss, M.; Wenz, D.; West, S. M.; Whitis, T. J.; Williams, M.;
   Wilson, M. J.; Winkler, D.; Wittweg, C.; Wolf, J.; Wolf, T.; Wolfs,
   F. L. H.; Woodford, S.; Woodward, D.; Wright, C. J.; Wu, V. H. S.;
   Wu, P.; Wüstling, S.; Wurm, M.; Xia, Q.; Xiang, X.; Xing, Y.; Xu,
   J.; Xu, Z.; Xu, D.; Yamashita, M.; Yamazaki, R.; Yan, H.; Yang, L.;
   Yang, Y.; Ye, J.; Yeh, M.; Young, I.; Yu, H. B.; Yu, T. T.; Yuan, L.;
   Zavattini, G.; Zerbo, S.; Zhang, Y.; Zhong, M.; Zhou, N.; Zhou, X.;
   Zhu, T.; Zhu, Y.; Zhuang, Y.; Zopounidis, J. P.; Zuber, K.; Zupan, J.
2022arXiv220302309A    Altcode:
  The nature of dark matter and properties of neutrinos are among the
  most pressing issues in contemporary particle physics. The dual-phase
  xenon time-projection chamber is the leading technology to cover the
  available parameter space for Weakly Interacting Massive Particles
  (WIMPs), while featuring extensive sensitivity to many alternative dark
  matter candidates. These detectors can also study neutrinos through
  neutrinoless double-beta decay and through a variety of astrophysical
  sources. A next-generation xenon-based detector will therefore be a true
  multi-purpose observatory to significantly advance particle physics,
  nuclear physics, astrophysics, solar physics, and cosmology. This
  review article presents the science cases for such a detector.

---------------------------------------------------------
Title: Oscillatory Reconnection of a 2D X-point in a Hot Coronal
    Plasma
Authors: Karampelas, Konstantinos; McLaughlin, James A.; Botha,
   Gert J. J.; Régnier, Stéphane
2022ApJ...925..195K    Altcode: 2021arXiv211205712K
  Oscillatory reconnection (a relaxation mechanism with periodic changes
  in connectivity) has been proposed as a potential physical mechanism
  underpinning several periodic phenomena in the solar atmosphere,
  including, but not limited to, quasi-periodic pulsations (QPPs). Despite
  its importance, however, the mechanism has never been studied within
  a hot, coronal plasma. We investigate oscillatory reconnection in a
  one million Kelvin plasma by solving the fully-compressive, resistive
  MHD equations for a 2D magnetic X-point under coronal conditions using
  the PLUTO code. We report on the resulting oscillatory reconnection
  including its periodicity and decay rate. We observe a more complicated
  oscillating profile for the current density compared to that found for
  a cold plasma, due to mode-conversion at the equipartition layer. We
  also consider, for the first time, the effect of adding anisotropic
  thermal conduction to the oscillatory reconnection mechanism, and
  we find this simplifies the spectrum of the oscillation profile
  and increases the decay rate. Crucially, the addition of thermal
  conduction does not prevent the oscillatory reconnection mechanism
  from manifesting. Finally, we reveal a relationship between the
  equilibrium magnetic field strength, decay rate, and period of
  oscillatory reconnection, which opens the tantalising possibility of
  utilizing oscillatory reconnection as a seismological tool.

---------------------------------------------------------
Title: Is phase mixing important in the quiet Sun?
Authors: Morton, Richard; McLaughlin, James; Tiwari, Ajay; Van
   Doorsselaere, Tom
2021AGUFMSH12B..09M    Altcode:
  The focus of many investigations on coronal wave heating has been to
  scrutinise the role of transverse (i.e. kink) modes; examining their
  damping by resonant absorption and the transfer of energy to Alfvén
  modes. Subsequently, the Alfvén modes are then subject to phase
  mixing and this leads to plasma heating. More recently, a non-linear
  mechanism for energy transfer has also been proposed, the so called
  uni-turbulence. Due to the ease with which they have been observed,
  the rapidly damped standing kink modes in active regions have spawned
  numerous studies investigating the role of resonant absorption in
  the observed damping. However, their counterparts in the quiet Sun,
  the propagating kink waves, have received little attention. Here I
  will discuss the results from a large-scale study of kink wave damping
  in the quiet Sun. We find convincing evidence that the damping of the
  kink waves is significantly weaker than in active regions and suggests
  that resonant absorption/phase mixing/uni-turbulence are not important
  mechanisms for wave-based heating of the quiescent Sun. I will also
  discuss the physical reason we suspect is behind this result and what
  it tells us about the fine-scale structure of the quiescent corona.

---------------------------------------------------------
Title: Weak Damping of Propagating MHD Kink Waves in the Quiescent
    Corona
Authors: Morton, Richard J.; Tiwari, Ajay K.; Van Doorsselaere, Tom;
   McLaughlin, James A.
2021ApJ...923..225M    Altcode: 2021arXiv210511924M
  Propagating transverse waves are thought to be a key transporter of
  Poynting flux throughout the Sun's atmosphere. Recent studies have shown
  that these transverse motions, interpreted as the magnetohydrodynamic
  kink mode, are prevalent throughout the corona. The associated energy
  estimates suggest the waves carry enough energy to meet the demands
  of coronal radiative losses in the quiescent Sun. However, it is still
  unclear how the waves deposit their energy into the coronal plasma. We
  present the results from a large-scale study of propagating kink waves
  in the quiescent corona using data from the Coronal Multi-channel
  Polarimeter (CoMP). The analysis reveals that the kink waves appear
  to be weakly damped, which would imply low rates of energy transfer
  from the large-scale transverse motions to smaller scales via either
  uniturbulence or resonant absorption. This raises questions about how
  the observed kink modes would deposit their energy into the coronal
  plasma. Moreover, these observations, combined with the results of Monte
  Carlo simulations, lead us to infer that the solar corona displays a
  spectrum of density ratios, with a smaller density ratio (relative to
  the ambient corona) in quiescent coronal loops and a higher density
  ratio in active-region coronal loops.

---------------------------------------------------------
Title: Projected sensitivities of the LUX-ZEPLIN experiment to new
    physics via low-energy electron recoils
Authors: Akerib, D. S.; Al Musalhi, A. K.; Alsum, S. K.; Amarasinghe,
   C. S.; Ames, A.; Anderson, T. J.; Angelides, N.; Araújo, H. M.;
   Armstrong, J. E.; Arthurs, M.; Bai, X.; Balajthy, J.; Balashov,
   S.; Bang, J.; Bargemann, J. W.; Bauer, D.; Baxter, A.; Beltrame, P.;
   Bernard, E. P.; Bernstein, A.; Bhatti, A.; Biekert, A.; Biesiadzinski,
   T. P.; Birch, H. J.; Blockinger, G. M.; Bodnia, E.; Boxer, B.; Brew,
   C. A. J.; Brás, P.; Burdin, S.; Busenitz, J. K.; Buuck, M.; Cabrita,
   R.; Carmona-Benitez, M. C.; Cascella, M.; Chan, C.; Chott, N. I.;
   Cole, A.; Converse, M. V.; Cottle, A.; Cox, G.; Creaner, O.; Cutter,
   J. E.; Dahl, C. E.; de Viveiros, L.; Dobson, J. E. Y.; Druszkiewicz,
   E.; Eriksen, S. R.; Fan, A.; Fayer, S.; Fearon, N. M.; Fiorucci, S.;
   Flaecher, H.; Fraser, E. D.; Fruth, T.; Gaitskell, R. J.; Genovesi,
   J.; Ghag, C.; Gibson, E.; Gokhale, S.; van der Grinten, M. G. D.;
   Gwilliam, C. B.; Hall, C. R.; Hardy, C. A.; Haselschwardt, S. J.;
   Hertel, S. A.; Horn, M.; Huang, D. Q.; Ignarra, C. M.; Jahangir,
   O.; James, R. S.; Ji, W.; Johnson, J.; Kaboth, A. C.; Kamaha, A. C.;
   Kamdin, K.; Kazkaz, K.; Khaitan, D.; Khazov, A.; Khurana, I.; Kodroff,
   D.; Korley, L.; Korolkova, E. V.; Kraus, H.; Kravitz, S.; Kreczko,
   L.; Krikler, B.; Kudryavtsev, V. A.; Leason, E. A.; Lee, J.; Leonard,
   D. S.; Lesko, K. T.; Levy, C.; Li, J.; Liao, J.; Lindote, A.; Linehan,
   R.; Lippincott, W. H.; Liu, X.; Lopes, M. I.; Lopez Asamar, E.; López
   Paredes, B.; Lorenzon, W.; Luitz, S.; Majewski, P. A.; Manalaysay,
   A.; Manenti, L.; Mannino, R. L.; Marangou, N.; McCarthy, M. E.;
   McKinsey, D. N.; McLaughlin, J.; Miller, E. H.; Mizrachi, E.; Monte,
   A.; Monzani, M. E.; Morad, J. A.; Morales Mendoza, J. D.; Morrison,
   E.; Mount, B. J.; Murphy, A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.;
   Nelson, H. N.; Neves, F.; Nikoleyczik, J. A.; Nilima, A.; Nguyen, A.;
   Olcina, I.; Oliver-Mallory, K. C.; Pal, S.; Palladino, K. J.; Palmer,
   J.; Patton, S.; Parveen, N.; Pease, E. K.; Penning, B.; Pereira, G.;
   Piepke, A.; Qie, Y.; Reichenbacher, J.; Rhyne, C. A.; Richards, A.;
   Riffard, Q.; Rischbieter, G. R. C.; Rosero, R.; Rossiter, P.; Santone,
   D.; Sazzad, A. B. M. R.; Schnee, R. W.; Scovell, P. R.; Shaw, S.;
   Shutt, T. A.; Silk, J. J.; Silva, C.; Smith, R.; Solmaz, M.; Solovov,
   V. N.; Sorensen, P.; Soria, J.; Stancu, I.; Stevens, A.; Stifter, K.;
   Suerfu, B.; Sumner, T. J.; Swanson, N.; Szydagis, M.; Taylor, W. C.;
   Taylor, R.; Temples, D. J.; Terman, P. A.; Tiedt, D. R.; Timalsina,
   M.; To, W. H.; Tovey, D. R.; Tripathi, M.; Tronstad, D. R.; Turner,
   W.; Utku, U.; Vaitkus, A.; Wang, B.; Wang, J. J.; Wang, W.; Watson,
   J. R.; Webb, R. C.; White, R. G.; Whitis, T. J.; Williams, M.; Wolfs,
   F. L. H.; Woodward, D.; Wright, C. J.; Xiang, X.; Xu, J.; Yeh, M.;
   Zarzhitsky, P.
2021PhRvD.104i2009A    Altcode: 2021arXiv210211740T
  LUX-ZEPLIN is a dark matter detector expected to obtain world-leading
  sensitivity to weakly-interacting massive particles interacting via
  nuclear recoils with a ∼7 -tonne xenon target mass. This paper
  presents sensitivity projections to several low-energy signals of the
  complementary electron recoil signal type: 1) an effective neutrino
  magnetic moment, and 2) an effective neutrino millicharge, both for
  p p -chain solar neutrinos, 3) an axion flux generated by the Sun, 4)
  axionlike particles forming the Galactic dark matter, 5) hidden photons,
  6) mirror dark matter, and 7) leptophilic dark matter. World-leading
  sensitivities are expected in each case, a result of the large 5.6 t
  1000 d exposure and low expected rate of electron-recoil backgrounds
  in the &lt;100 keV energy regime. A consistent signal generation,
  background model and profile-likelihood analysis framework is used
  throughout.

---------------------------------------------------------
Title: A Statistical Study of Propagating MHD Kink Waves in the
    Quiescent Corona
Authors: Tiwari, Ajay K.; Morton, Richard J.; McLaughlin, James A.
2021ApJ...919...74T    Altcode: 2021arXiv210512451T
  The Coronal Multi-channel Polarimeter (CoMP) has opened up exciting
  opportunities to probe transverse MHD waves in the Sun's corona. The
  archive of CoMP data is utilized to generate a catalog of quiescent
  coronal loops that can be used for studying propagating kink waves. The
  catalog contains 120 loops observed between 2012 and 2014. This catalog
  is further used to undertake a statistical study of propagating kink
  waves in the quiet regions of the solar corona, investigating phase
  speeds, loop lengths, footpoint power ratio (a measure of wave power
  entering the corona through each footpoint of a loop) and equilibrium
  parameter (which provides a measure of the change in wave amplitude)
  values. The statistical study enables us to establish the presence of a
  relationship between the rate of damping and the length of the coronal
  loop, with longer coronal loops displaying weaker wave damping. We
  suggest the reason for this behavior is related to a decreasing average
  density contrast between the loop and ambient plasma as loop length
  increases. The catalog presented here will provide the community with
  the foundation for the further study of propagating kink waves in the
  quiet solar corona.

---------------------------------------------------------
Title: Magnetohydrodynamic Waves in Open Coronal Structures
Authors: Banerjee, D.; Krishna Prasad, S.; Pant, V.; McLaughlin, J. A.;
   Antolin, P.; Magyar, N.; Ofman, L.; Tian, H.; Van Doorsselaere, T.;
   De Moortel, I.; Wang, T. J.
2021SSRv..217...76B    Altcode: 2020arXiv201208802B
  Modern observatories have revealed the ubiquitous presence of
  magnetohydrodynamic waves in the solar corona. The propagating waves
  (in contrast to the standing waves) are usually originated in the lower
  solar atmosphere which makes them particularly relevant to coronal
  heating. Furthermore, open coronal structures are believed to be the
  source regions of solar wind, therefore, the detection of MHD waves
  in these structures is also pertinent to the acceleration of solar
  wind. Besides, the advanced capabilities of the current generation
  telescopes have allowed us to extract important coronal properties
  through MHD seismology. The recent progress made in the detection,
  origin, and damping of both propagating slow magnetoacoustic waves and
  kink (Alfvénic) waves is presented in this review article especially
  in the context of open coronal structures. Where appropriate, we give
  an overview on associated theoretical modelling studies. A few of the
  important seismological applications of these waves are discussed. The
  possible role of Alfvénic waves in the acceleration of solar wind is
  also touched upon.

---------------------------------------------------------
Title: Quasi-Periodic Pulsations in Solar and Stellar Flares:
    A Review of Underpinning Physical Mechanisms and Their Predicted
    Observational Signatures
Authors: Zimovets, I. V.; McLaughlin, J. A.; Srivastava, A. K.;
   Kolotkov, D. Y.; Kuznetsov, A. A.; Kupriyanova, E. G.; Cho, I. -H.;
   Inglis, A. R.; Reale, F.; Pascoe, D. J.; Tian, H.; Yuan, D.; Li, D.;
   Zhang, Q. M.
2021SSRv..217...66Z    Altcode:
  The phenomenon of quasi-periodic pulsations (QPPs) in solar and stellar
  flares has been known for over 50 years and significant progress has
  been made in this research area. It has become clear that QPPs are
  not rare—they are found in many flares and, therefore, robust flare
  models should reproduce their properties in a natural way. At least
  fifteen mechanisms/models have been developed to explain QPPs in solar
  flares, which mainly assume the presence of magnetohydrodynamic (MHD)
  oscillations in coronal structures (magnetic loops and current sheets)
  or quasi-periodic regimes of magnetic reconnection. We review the most
  important and interesting results on flare QPPs, with an emphasis on
  the results of recent years, and we present the predicted and prominent
  observational signatures of each of the fifteen mechanisms. However,
  it is not yet possible to draw an unambiguous conclusion as to
  the correct underlying QPP mechanism because of the qualitative,
  rather than quantitative, nature of most of the models and also due
  to insufficient observational information on the physical properties
  of the flare region, in particular the spatial structure of the QPP
  source. We also review QPPs in stellar flares, where progress is
  largely based on solar-stellar analogies, suggesting similarities in
  the physical processes in flare regions on the Sun and magnetoactive
  stars. The presence of QPPs with similar properties in solar and
  stellar flares is, in itself, a strong additional argument in favor
  of the likelihood of solar-stellar analogies. Hence, advancing our
  understanding of QPPs in solar flares provides an important additional
  channel of information about stellar flares. However, further work in
  both theory/simulations and in observations is needed.

---------------------------------------------------------
Title: Separating 3<SUP>9</SUP>Ar from 4<SUP>0</SUP>Ar by cryogenic
    distillation with Aria for dark-matter searches
Authors: Agnes, P.; Albergo, S.; Albuquerque, I. F. M.; Alexander, T.;
   Alici, A.; Alton, A. K.; Amaudruz, P.; Arba, M.; Arpaia, P.; Arcelli,
   S.; Ave, M.; Avetissov, I. Ch.; Avetisov, R. I.; Azzolini, O.; Back,
   H. O.; Balmforth, Z.; Barbarian, V.; Barrado Olmedo, A.; Barrillon,
   P.; Basco, A.; Batignani, G.; Bondar, A.; Bonivento, W. M.; Borisova,
   E.; Bottino, B.; Boulay, M. G.; Buccino, G.; Bussino, S.; Busto,
   J.; Buzulutskov, A.; Cadeddu, M.; Cadoni, M.; Caminata, A.; Canesi,
   E. V.; Canci, N.; Cappello, G.; Caravati, M.; Cárdenas-Montes, M.;
   Cargioli, N.; Carlini, M.; Carnesecchi, F.; Castello, P.; Castellani,
   A.; Catalanotti, S.; Cataudella, V.; Cavalcante, P.; Cavuoti, S.;
   Cebrian, S.; Cela Ruiz, J. M.; Celano, B.; Chashin, S.; Chepurnov,
   A.; Cicalò, C.; Cifarelli, L.; Cintas, D.; Coccetti, F.; Cocco, V.;
   Colocci, M.; Conde Vilda, E.; Consiglio, L.; Copello, S.; Corning,
   J.; Covone, G.; Czudak, P.; D'Aniello, M.; D'Auria, S.; Da Rocha
   Rolo, M. D.; Dadoun, O.; Daniel, M.; Davini, S.; De Candia, A.; De
   Cecco, S.; De Falco, A.; De Filippis, G.; De Gruttola, D.; De Guido,
   G.; De Rosa, G.; Della Valle, M.; Dellacasa, G.; De Pasquale, S.;
   Derbin, A. V.; Devoto, A.; Di Noto, L.; Di Eusanio, F.; Dionisi, C.;
   Di Stefano, P.; Dolganov, G.; Dongiovanni, D.; Dordei, F.; Downing,
   M.; Erjavec, T.; Falciano, S.; Farenzena, S.; Fernandez Diaz, M.;
   Filip, C.; Fiorillo, G.; Franceschi, A.; Franco, D.; Frolov, E.;
   Funicello, N.; Gabriele, F.; Galbiati, C.; Garbini, M.; Garcia Abia,
   P.; Gendotti, A.; Ghiano, C.; Giampaolo, R. A.; Giganti, C.; Giorgi,
   M. A.; Giovanetti, G. K.; Gligan, M. L.; Goicoechea Casanueva, V.;
   Gola, A.; Goretti, A. M.; Graciani Diaz, R.; Grigoriev, G. Y.; Grobov,
   A.; Gromov, M.; Guan, M.; Guerzoni, M.; Guetti, M.; Gulino, M.; Guo,
   C.; Hackett, B. R.; Hallin, A.; Haranczyk, M.; Hill, S.; Horikawa,
   S.; Hubaut, F.; Hugues, T.; Hungerford, E. V.; Ianni, An.; Ippolito,
   V.; James, C. C.; Jillings, C.; Kachru, P.; Kemp, A. A.; Kendziora,
   C. L.; Keppel, G.; Khomyakov, A. V.; Kish, A.; Kochanek, I.; Kondo,
   K.; Korga, G.; Kubankin, A.; Kugathasan, R.; Kuss, M.; Kuźniak,
   M.; La Commara, M.; La Delfa, L.; La Grasta, D.; Lai, M.; Lami, N.;
   Langrock, S.; Leyton, M.; Li, X.; Lidey, L.; Lippi, F.; Lissia, M.;
   Longo, G.; Maccioni, N.; Machulin, I. N.; Mapelli, L.; Marasciulli, A.;
   Margotti, A.; Mari, S. M.; Maricic, J.; Marinelli, M.; Martínez, M.;
   Martinez Rojas, A. D.; Martini, A.; Mascia, M.; Masetto, M.; Masoni,
   A.; Mazzi, A.; McDonald, A. B.; Mclaughlin, J.; Messina, A.; Meyers,
   P. D.; Miletic, T.; Milincic, R.; Miola, R.; Moggi, A.; Moharana,
   A.; Moioli, S.; Monroe, J.; Morisi, S.; Morrocchi, M.; Mozhevitina,
   E. N.; Mróz, T.; Muratova, V. N.; Murenu, A.; Muscas, C.; Musenich,
   L.; Musico, P.; Nania, R.; Napolitano, T.; Navrer Agasson, A.; Nessi,
   M.; Nikulin, I.; Nowak, J.; Oleinik, A.; Oleynikov, V.; Pagani, L.;
   Pallavicini, M.; Palmas, S.; Pandola, L.; Pantic, E.; Paoloni, E.;
   Paternoster, G.; Pegoraro, P. A.; Pellegrini, L. A.; Pellegrino,
   C.; Pelczar, K.; Perotti, F.; Pesudo, V.; Picciau, E.; Pietropaolo,
   F.; Pinna, T.; Pocar, A.; Podda, P.; Poehlmann, D. M.; Pordes, S.;
   Poudel, S. S.; Pralavorio, P.; Price, D.; Raffaelli, F.; Ragusa, F.;
   Ramirez, A.; Razeti, M.; Razeto, A.; Renshaw, A. L.; Rescia, S.;
   Rescigno, M.; Resnati, F.; Retiere, F.; Rignanese, L. P.; Ripoli,
   C.; Rivetti, A.; Rode, J.; Romero, L.; Rossi, M.; Rubbia, A.; Rucaj,
   M.; Sabiu, G. M.; Salatino, P.; Samoylov, O.; Sánchez García, E.;
   Sandford, E.; Sanfilippo, S.; Sangiorgio, V. A.; Santacroce, V.;
   Santone, D.; Santorelli, R.; Santucci, A.; Savarese, C.; Scapparone,
   E.; Schlitzer, B.; Scioli, G.; Semenov, D. A.; Shaw, B.; Shchagin,
   A.; Sheshukov, A.; Simeone, M.; Skensved, P.; Skorokhvatov, M. D.;
   Smirnov, O.; Smith, B.; Sokolov, A.; Stefanizzi, R.; Steri, A.;
   Stracka, S.; Strickland, V.; Stringer, M.; Sulis, S.; Suvorov, Y.;
   Szelc, A. M.; Szucs-Balazs, J. Z.; Tartaglia, R.; Testera, G.; Thorpe,
   T. N.; Tonazzo, A.; Torres-Lara, S.; Tosti, S.; Tricomi, A.; Tuveri,
   M.; Unzhakov, E. V.; Usai, G.; Vallivilayil John, T.; Vescovi, S.;
   Viant, T.; Viel, S.; Vishneva, A.; Vogelaar, R. B.; Wada, M.; Wang,
   H.; Wang, Y.; Westerdale, S.; Wheadon, R. J.; Williams, L.; M. Wojcik,
   Ma.; Wojcik, Ma.; Xiao, X.; Yang, C.; Zani, A.; Zenobio, F.; Zichichi,
   A.; Zuzel, G.; Zykova, M. P.; DarkSide-20k Collaboration
2021EPJC...81..359A    Altcode: 2021arXiv210108686D
  Aria is a plant hosting a 350 m cryogenic isotopic distillation
  column, the tallest ever built, which is being installed in a mine
  shaft at Carbosulcis S.p.A., Nuraxi-Figus (SU), Italy. Aria is one
  of the pillars of the argon dark-matter search experimental program,
  lead by the Global Argon Dark Matter Collaboration. It was designed
  to reduce the isotopic abundance of 3<SUP>9</SUP>Ar in argon extracted
  from underground sources, called Underground Argon (UAr), which is used
  for dark-matter searches. Indeed, 3<SUP>9</SUP>Ar is a β -emitter
  of cosmogenic origin, whose activity poses background and pile-up
  concerns in the detectors. In this paper, we discuss the requirements,
  design, construction, tests, and projected performance of the plant
  for the isotopic cryogenic distillation of argon. We also present the
  successful results of the isotopic cryogenic distillation of nitrogen
  with a prototype plant.

---------------------------------------------------------
Title: Sensitivity of future liquid argon dark matter search
    experiments to core-collapse supernova neutrinos
Authors: DarkSide-20k Collaboration; Agnes, P.; Albergo, S.;
   Albuquerque, I. F. M.; Alexander, T.; Alici, A.; Alton, A. K.;
   Amaudruz, P.; Arcelli, S.; Ave, M.; Avetissov, I. Ch.; Avetisov, R. I.;
   Azzolini, O.; Back, H. O.; Balmforth, Z.; Barbarian, V.; Barrado
   Olmedo, A.; Barrillon, P.; Basco, A.; Batignani, G.; Bondar, A.;
   Bonivento, W. M.; Borisova, E.; Bottino, B.; Boulay, M. G.; Buccino,
   G.; Bussino, S.; Busto, J.; Buzulutskov, A.; Cadeddu, M.; Cadoni, M.;
   Caminata, A.; Canci, N.; Cappello, G.; Caravati, M.; Cárdenas-Montes,
   M.; Carlini, M.; Carnesecchi, F.; Castello, P.; Catalanotti, S.;
   Cataudella, V.; Cavalcante, P.; Cavuoti, S.; Cebrian, S.; Cela
   Ruiz, J. M.; Celano, B.; Chashin, S.; Chepurnov, A.; Chyhyrynets,
   E.; Cicalò, C.; Cifarelli, L.; Cintas, D.; Coccetti, F.; Cocco, V.;
   Colocci, M.; Conde Vilda, E.; Consiglio, L.; Copello, S.; Corning, J.;
   Covone, G.; Czudak, P.; D'Auria, S.; Da Rocha Rolo, M. D.; Dadoun,
   O.; Daniel, M.; Davini, S.; De Candia, A.; De Cecco, S.; De Falco,
   A.; De Filippis, G.; De Gruttola, D.; De Guido, G.; De Rosa, G.; Della
   Valle, M.; Dellacasa, G.; De Pasquale, S.; Derbin, A. V.; Devoto, A.;
   Di Noto, L.; Dionisi, C.; Di Stefano, P.; Dolganov, G.; Dordei, F.;
   Doria, L.; Downing, M.; Erjavec, T.; Fernandez Diaz, M.; Fiorillo,
   G.; Franceschi, A.; Franco, D.; Frolov, E.; Funicello, N.; Gabriele,
   F.; Galbiati, C.; Garbini, M.; Garcia Abia, P.; Gendotti, A.; Ghiano,
   C.; Giampaolo, R. A.; Giganti, C.; Giorgi, M. A.; Giovanetti, G. K.;
   Goicoechea Casanueva, V.; Gola, A.; Graciani Diaz, R.; Grigoriev,
   G. Y.; Grobov, A.; Gromov, M.; Guan, M.; Guerzoni, M.; Gulino, M.; Guo,
   C.; Hackett, B. R.; Hallin, A.; Haranczyk, M.; Hill, S.; Horikawa,
   S.; Hubaut, F.; Hugues, T.; Hungerford, E. V.; Ianni, An.; Ippolito,
   V.; James, C. C.; Jillings, C.; Kachru, P.; Kemp, A. A.; Kendziora,
   C. L.; Keppel, G.; Khomyakov, A. V.; Kim, S.; Kish, A.; Kochanek,
   I.; Kondo, K.; Korga, G.; Kubankin, A.; Kugathasan, R.; Kuss, M.;
   Kuźniak, M.; La Commara, M.; Lai, M.; Langrock, S.; Leyton, M.; Li,
   X.; Lidey, L.; Lissia, M.; Longo, G.; Machulin, I. N.; Mapelli, L.;
   Marasciulli, A.; Margotti, A.; Mari, S. M.; Maricic, J.; Martínez,
   M.; Martinez Rojas, A. D.; Martoff, C. J.; Masoni, A.; Mazzi, A.;
   McDonald, A. B.; Mclaughlin, J.; Messina, A.; Meyers, P. D.; Miletic,
   T.; Milincic, R.; Moggi, A.; Moharana, A.; Moioli, S.; Monroe, J.;
   Morisi, S.; Morrocchi, M.; Mozhevitina, E. N.; Mróz, T.; Muratova,
   V. N.; Muscas, C.; Musenich, L.; Musico, P.; Nania, R.; Napolitano,
   T.; Navrer Agasson, A.; Nessi, M.; Nikulin, I.; Nowak, J.; Oleinik,
   A.; Oleynikov, V.; Pagani, L.; Pallavicini, M.; Pandola, L.; Pantic,
   E.; Paoloni, E.; Paternoster, G.; Pegoraro, P. A.; Pelczar, K.;
   Pellegrini, L. A.; Pellegrino, C.; Perotti, F.; Pesudo, V.; Picciau,
   E.; Pietropaolo, F.; Pira, C.; Pocar, A.; Poehlmann, D. M.; Pordes,
   S.; Poudel, S. S.; Pralavorio, P.; Price, D.; Raffaelli, F.; Ragusa,
   F.; Ramirez, A.; Razeti, M.; Razeto, A.; Renshaw, A. L.; Rescia, S.;
   Rescigno, M.; Resnati, F.; Retiere, F.; Rignanese, L. P.; Ripoli, C.;
   Rivetti, A.; Rode, J.; Romero, L.; Rossi, M.; Rubbia, A.; Salatino,
   P.; Samoylov, O.; Sánchez García, E.; Sandford, E.; Sanfilippo, S.;
   Santone, D.; Santorelli, R.; Savarese, C.; Scapparone, E.; Schlitzer,
   B.; Scioli, G.; Semenov, D. A.; Shaw, B.; Shchagin, A.; Sheshukov, A.;
   Simeone, M.; Skensved, P.; Skorokhvatov, M. D.; Smirnov, O.; Smith,
   B.; Sokolov, A.; Steri, A.; Stracka, S.; Strickland, V.; Stringer,
   M.; Sulis, S.; Suvorov, Y.; Szelc, A. M.; Tartaglia, R.; Testera, G.;
   Thorpe, T. N.; Tonazzo, A.; Torres-Lara, S.; Tricomi, A.; Unzhakov,
   E. V.; Usai, G.; Vallivilayil John, T.; Viant, T.; Viel, S.; Vishneva,
   A.; Vogelaar, R. B.; Wada, M.; Wang, H.; Wang, Y.; Westerdale, S.;
   Wheadon, R. J.; Williams, L.; Wojcik, Ma. M.; Wojcik, Ma.; Xiao, X.;
   Yang, C.; Ye, Z.; Zani, A.; Zichichi, A.; Zuzel, G.; Zykova, M. P.
2021JCAP...03..043D    Altcode: 2021JCAP...03..043T; 2020arXiv201107819A
  Future liquid-argon DarkSide-20k and Argo detectors, designed for direct
  dark matter search, will be sensitive also to core-collapse supernova
  neutrinos, via coherent elastic neutrino-nucleus scattering. This
  interaction channel is flavor-insensitive with a high-cross section,
  enabling for a high-statistics neutrino detection with target masses
  of ∼50 t and ∼360 t for DarkSide-20k and Argo respectively. Thanks
  to the low-energy threshold of ∼0.5 keV<SUB>nr</SUB> achievable
  by exploiting the ionization channel, DarkSide-20k and Argo have the
  potential to discover supernova bursts throughout our galaxy and up to
  the Small Magellanic Cloud, respectively, assuming a 11-M<SUB>⊙</SUB>
  progenitor star. We report also on the sensitivity to the neutronization
  burst, whose electron neutrino flux is suppressed by oscillations
  when detected via charged current and elastic scattering. Finally,
  the accuracies in the reconstruction of the average and total neutrino
  energy in the different phases of the supernova burst, as well as its
  time profile, are also discussed, taking into account the expected
  background and the detector response.

---------------------------------------------------------
Title: Simulations of events for the LUX-ZEPLIN (LZ) dark matter
    experiment
Authors: Akerib, D. S.; Akerlof, C. W.; Alqahtani, A.; Alsum, S. K.;
   Anderson, T. J.; Angelides, N.; Araújo, H. M.; Armstrong, J. E.;
   Arthurs, M.; Bai, X.; Balajthy, J.; Balashov, S.; Bang, J.; Bauer, D.;
   Baxter, A.; Bensinger, J.; Bernard, E. P.; Bernstein, A.; Bhatti, A.;
   Biekert, A.; Biesiadzinski, T. P.; Birch, H. J.; Boast, K. E.; Boxer,
   B.; Brás, P.; Buckley, J. H.; Bugaev, V. V.; Burdin, S.; Busenitz,
   J. K.; Cabrita, R.; Carels, C.; Carlsmith, D. L.; Carmona-Benitez,
   M. C.; Cascella, M.; Chan, C.; Chott, N. I.; Cole, A.; Cottle,
   A.; Cutter, J. E.; Dahl, C. E.; Viveiros, L. de; Dobson, J. E. Y.;
   Druszkiewicz, E.; Edberg, T. K.; Eriksen, S. R.; Fan, A.; Fayer, S.;
   Fiorucci, S.; Flaecher, H.; Fraser, E. D.; Fruth, T.; Gaitskell,
   R. J.; Genovesi, J.; Ghag, C.; Gibson, E.; Gilchriese, M. G. D.;
   Gokhale, S.; van der Grinten, M. G. D.; Hall, C. R.; Harrison, A.;
   Haselschwardt, S. J.; Hertel, S. A.; Hor, J. Y. -K.; Horn, M.; Huang,
   D. Q.; Ignarra, C. M.; Jahangir, O.; Ji, W.; Johnson, J.; Kaboth,
   A. C.; Kamaha, A. C.; Kamdin, K.; Kazkaz, K.; Khaitan, D.; Khazov,
   A.; Khurana, I.; Kocher, C. D.; Korley, L.; Korolkova, E. V.; Kras,
   J.; Kraus, H.; Kravitz, S.; Kreczko, L.; Krikler, B.; Kudryavtsev,
   V. A.; Leason, E. A.; Lee, J.; Leonard, D. S.; Lesko, K. T.; Levy,
   C.; Li, J.; Liao, J.; Liao, F. -T.; Lin, J.; Lindote, A.; Linehan,
   R.; Lippincott, W. H.; Liu, R.; Liu, X.; Loniewski, C.; Lopes, M. I.;
   López Paredes, B.; Lorenzon, W.; Luitz, S.; Lyle, J. M.; Majewski,
   P. A.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou, N.;
   Marzioni, M. F.; McKinsey, D. N.; McLaughlin, J.; Meng, Y.; Miller,
   E. H.; Mizrachi, E.; Monte, A.; Monzani, M. E.; Morad, J. A.; Morrison,
   E.; Mount, B. J.; Murphy, A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.;
   Nehrkorn, C.; Nelson, H. N.; Neves, F.; Nikoleyczik, J. A.; Nilima, A.;
   Olcina, I.; Oliver-Mallory, K. C.; Pal, S.; Palladino, K. J.; Palmer,
   J.; Parveen, N.; Pease, E. K.; Penning, B.; Pereira, G.; Piepke, A.;
   Pushkin, K.; Reichenbacher, J.; Rhyne, C. A.; Richards, A.; Riffard,
   Q.; Rischbieter, G. R. C.; Rosero, R.; Rossiter, P.; Rutherford,
   G.; Santone, D.; Sazzad, A. B. M. R.; Schnee, R. W.; Schubnell, M.;
   Scovell, P. R.; Seymour, D.; Shaw, S.; Shutt, T. A.; Silk, J. J.;
   Silva, C.; Smith, R.; Solmaz, M.; Solovov, V. N.; Sorensen, P.;
   Stancu, I.; Stevens, A.; Stifter, K.; Sumner, T. J.; Swanson, N.;
   Szydagis, M.; Tan, M.; Taylor, W. C.; Taylor, R.; Temples, D. J.;
   Terman, P. A.; Tiedt, D. R.; Timalsina, M.; Tomás, A.; Tripathi,
   M.; Tronstad, D. R.; Turner, W.; Tvrznikova, L.; Utku, U.; Vacheret,
   A.; Vaitkus, A.; Wang, J. J.; Wang, W.; Watson, J. R.; Webb, R. C.;
   White, R. G.; Whitis, T. J.; Wolfs, F. L. H.; Woodward, D.; Xiang,
   X.; Xu, J.; Yeh, M.; Zarzhitsky, P.
2021APh...12502480A    Altcode:
  The LUX-ZEPLIN dark matter search aims to achieve a sensitivity
  to the WIMP-nucleon spin-independent cross-section down to (1-2)
  ×10<SUP>-12</SUP> pb at a WIMP mass of 40 GeV/c<SUP>2</SUP>. This
  paper describes the simulations framework that, along with radioactivity
  measurements, was used to support this projection, and also to provide
  mock data for validating reconstruction and analysis software. Of
  particular note are the event generators, which allow us to model
  the background radiation, and the detector response physics used in
  the production of raw signals, which can be converted into digitized
  waveforms similar to data from the operational detector. Inclusion of
  the detector response allows us to process simulated data using the
  same analysis routines as developed to process the experimental data.

---------------------------------------------------------
Title: Enhancing the sensitivity of the LUX-ZEPLIN (LZ) dark matter
    experiment to low energy signals
Authors: Akerib, D. S.; Al Musalhi, A. K.; Alsum, S. K.; Amarasinghe,
   C. S.; Ames, A.; Anderson, T. J.; Angelides, N.; Araújo, H. M.;
   Armstrong, J. E.; Arthurs, M.; Bai, X.; Balajthy, J.; Balashov,
   S.; Bang, J.; Bargemann, J. W.; Bauer, D.; Baxter, A.; Beltrame, P.;
   Bernard, E. P.; Bernstein, A.; Bhatti, A.; Biekert, A.; Biesiadzinski,
   T. P.; Birch, H. J.; Blockinger, G. M.; Boxer, B.; Brew, C. A. J.;
   Brás, P.; Burdin, S.; Busenitz, J. K.; Buuck, M.; Cabrita, R.;
   Carmona-Benitez, M. C.; Cascella, M.; Chan, C.; Chott, N. I.; Cole,
   A.; Converse, M. V.; Cottle, A.; Cox, G.; Cutter, J. E.; Dahl,
   C. E.; de Viveiros, L.; Dobson, J. E. Y.; Druszkiewicz, E.; Eriksen,
   S. R.; Fan, A.; Fayer, S.; Fearon, N. M.; Fiorucci, S.; Flaecher,
   H.; Fraser, E. D.; Fruth, T.; Gaitskell, R. J.; Genovesi, J.; Ghag,
   C.; Gibson, E.; Gokhale, S.; van der Grinten, M. G. D.; Gwilliam,
   C. B.; Hall, C. R.; Haselschwardt, S. J.; Hertel, S. A.; Horn,
   M.; Huang, D. Q.; Ignarra, C. M.; Jahangir, O.; James, R. S.; Ji,
   W.; Johnson, J.; Kaboth, A. C.; Kamaha, A. C.; Kamdin, K.; Kazkaz,
   K.; Khaitan, D.; Khazov, A.; Khurana, I.; Kodroff, D.; Korley, L.;
   Korolkova, E. V.; Kraus, H.; Kravitz, S.; Kreczko, L.; Krikler, B.;
   Kudryavtsev, V. A.; Leason, E. A.; Lesko, K. T.; Levy, C.; Li, J.;
   Liao, J.; Lin, J.; Lindote, A.; Linehan, R.; Lippincott, W. H.; Liu,
   X.; Lopes, M. I.; Lopez Asamar, E.; López Paredes, B.; Lorenzon, W.;
   Luitz, S.; Majewski, P. A.; Manalaysay, A.; Manenti, L.; Mannino,
   R. L.; Marangou, N.; McCarthy, M. E.; McKinsey, D. N.; McLaughlin,
   J.; Miller, E. H.; Mizrachi, E.; Monte, A.; Monzani, M. E.; Morad,
   J. A.; Morales Mendoza, J. D.; Morrison, E.; Mount, B. J.; Murphy,
   A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.; Nelson, H. N.; Neves,
   F.; Nikoleyczik, J. A.; Olcina, I.; Oliver-Mallory, K. C.; Pal, S.;
   Palladino, K. J.; Palmer, J.; Parveen, N.; Pease, E. K.; Penning, B.;
   Pereira, G.; Piepke, A.; Qie, Y.; Reichenbacher, J.; Rhyne, C. A.;
   Richards, A.; Riffard, Q.; Rischbieter, G. R. C.; Rosero, R.; Rossiter,
   P.; Santone, D.; Sazzad, A. B. M. R.; Schnee, R. W.; Scovell, P. R.;
   Shaw, S.; Shutt, T. A.; Silk, J. J.; Silva, C.; Smith, R.; Solmaz, M.;
   Solovov, V. N.; Sorensen, P.; Stancu, I.; Stevens, A.; Stifter, K.;
   Suerfu, B.; Sumner, T. J.; Swanson, N.; Szydagis, M.; Taylor, W. C.;
   Taylor, R.; Temples, D. J.; Terman, P. A.; Tiedt, D. R.; Timalsina,
   M.; To, W. H.; Tripathi, M.; Tronstad, D. R.; Turner, W.; Utku, U.;
   Vaitkus, A.; Wang, B.; Wang, J. J.; Wang, W.; Watson, J. R.; Webb,
   R. C.; White, R. G.; Whitis, T. J.; Williams, M.; Wolfs, F. L. H.;
   Woodward, D.; Wright, C. J.; Xiang, X.; Xu, J.; Yeh, M.; Zarzhitsky, P.
2021arXiv210108753A    Altcode:
  Two-phase xenon detectors, such as that at the core of the forthcoming
  LZ dark matter experiment, use photomultiplier tubes to sense the
  primary (S1) and secondary (S2) scintillation signals resulting
  from particle interactions in their liquid xenon target. This paper
  describes a simulation study exploring two techniques to lower the
  energy threshold of LZ to gain sensitivity to low-mass dark matter
  and astrophysical neutrinos, which will be applicable to other liquid
  xenon detectors. The energy threshold is determined by the number of
  detected S1 photons; typically, these must be recorded in three or
  more photomultiplier channels to avoid dark count coincidences that
  mimic real signals. To lower this threshold: a) we take advantage of
  the double photoelectron emission effect, whereby a single vacuum
  ultraviolet photon has a $\sim20\%$ probability of ejecting two
  photoelectrons from a photomultiplier tube photocathode; and b) we drop
  the requirement of an S1 signal altogether, and use only the ionization
  signal, which can be detected more efficiently. For both techniques
  we develop signal and background models for the nominal exposure, and
  explore accompanying systematic effects, including the dependence on the
  free electron lifetime in the liquid xenon. When incorporating double
  photoelectron signals, we predict a factor of $\sim 4$ sensitivity
  improvement to the dark matter-nucleon scattering cross-section at
  $2.5$ GeV/c$^2$, and a factor of $\sim1.6$ increase in the solar
  $^8$B neutrino detection rate. Dropping the S1 requirement may allow
  sensitivity gains of two orders of magnitude in both cases. Finally,
  we apply these techniques to even lower masses by taking into account
  the atomic Migdal effect; this could lower the dark matter particle
  mass threshold to $80$ MeV/c$^2$.

---------------------------------------------------------
Title: Using Transverse Waves to Probe the Plasma Conditions at the
    Base of the Solar Wind
Authors: Weberg, Micah J.; Morton, Richard J.; McLaughlin, James A.
2020ApJ...894...79W    Altcode:
  It has long been suggested that magnetohydrodynamic (MHD) waves may
  supply a significant proportion of the energy required to heat the
  corona and accelerate the solar wind. Depending on the properties of
  the local plasma, MHD wave modes may exhibit themselves as a variety of
  incompressible, transverse waves. The local magnetic field and particle
  density influence the properties of these waves (e.g., amplitude),
  thus direct measurements of transverse waves provide a mechanism to
  indirectly probe the local plasma conditions. We present the first
  statistical approach to magnetoseismology of a localized region of the
  solar corona, analyzing transverse waves above the south polar coronal
  hole on 2011 May 23. Automated methods are utilized to examine 4 hr of
  EUV imaging data to study how the waves evolve as a function of height
  (I.e., altitude) through the low corona. Between heights of 15 and 35
  Mm, we find that the measured wave periods are approximately constant,
  and that observed displacement and velocity amplitudes increase at
  rates that are consistent with undamped waves. This enables us to
  derive a relative density profile for the coronal hole environment
  in question, without the use of spectroscopic data. Furthermore,
  our results indicate that between 5 and 15 Mm above the limb, the
  relative density is larger than that expected from 1D hydrostatic
  models, and signals a more extended transition region with a gradual
  change in density. This has implications for self-consistent models
  of wave propagation from the photosphere to the corona and beyond.

---------------------------------------------------------
Title: Measurement of the gamma ray background in the Davis cavern
    at the Sanford Underground Research Facility
Authors: Akerib, D. S.; Akerlof, C. W.; Alsum, S. K.; Angelides, N.;
   Araújo, H. M.; Armstrong, J. E.; Arthurs, M.; Bai, X.; Balajthy, J.;
   Balashov, S.; Baxter, A.; Bernard, E. P.; Biekert, A.; Biesiadzinski,
   T. P.; Boast, K. E.; Boxer, B.; Brás, P.; Buckley, J. H.; Bugaev,
   V. V.; Burdin, S.; Busenitz, J. K.; Carels, C.; Carlsmith, D. L.;
   Carmona-Benitez, M. C.; Cascella, M.; Chan, C.; Cole, A.; Cottle,
   A.; Cutter, J. E.; Dahl, C. E.; de Viveiros, L.; Dobson, J. E. Y.;
   Druszkiewicz, E.; Edberg, T. K.; Fan, A.; Fiorucci, S.; Flaecher,
   H.; Fruth, T.; Gaitskell, R. J.; Genovesi, J.; Ghag, C.; Gilchriese,
   M. G. D.; Gokhale, S.; van der Grinten, M. G. D.; Hall, C. R.;
   Hans, S.; Harrison, J.; Haselschwardt, S. J.; Hertel, S. A.; Hor,
   J. Y. -K.; Horn, M.; Huang, D. Q.; Ignarra, C. M.; Jahangir, O.; Ji,
   W.; Johnson, J.; Kaboth, A. C.; Kamdin, K.; Khaitan, D.; Khazov, A.;
   Kim, W. T.; Kocher, C. D.; Korley, L.; Korolkova, E. V.; Kras, J.;
   Kraus, H.; Kravitz, S. W.; Kreczko, L.; Krikler, B.; Kudryavtsev,
   V. A.; Leason, E. A.; Lee, J.; Leonard, D. S.; Lesko, K. T.; Levy,
   C.; Li, J.; Liao, J.; Liao, F. -T.; Lin, J.; Lindote, A.; Linehan,
   R.; Lippincott, W. H.; Liu, R.; Liu, X.; Loniewski, C.; Lopes, M. I.;
   López Paredes, B.; Lorenzon, W.; Luitz, S.; Lyle, J. M.; Majewski,
   P. A.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou, N.;
   Marzioni, M. F.; McKinsey, D. N.; McLaughlin, J.; Meng, Y.; Miller,
   E. H.; Monzani, M. E.; Morad, J. A.; Morrison, E.; Mount, B. J.;
   Murphy, A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.; Nehrkorn,
   C.; Nelson, H. N.; Neves, F.; Nikoleyczik, J.; Nilima, A.; Olcina,
   I.; Oliver-Mallory, K. C.; Pal, S.; Palladino, K. J.; Pease, E. K.;
   Penning, B. P.; Pereira, G.; Piepke, A.; Pushkin, K.; Reichenbacher,
   J.; Rhyne, C. A.; Riffard, Q.; Rischbieter, G. R. C.; Rodrigues,
   J. P.; Rosero, R.; Rossiter, P.; Rutherford, G.; Sazzad, A. B. M. R.;
   Schnee, R. W.; Schubnell, M.; Scovell, P. R.; Seymour, D.; Shaw, S.;
   Shutt, T. A.; Silk, J. J.; Silva, C.; Solmaz, M.; Solovov, V. N.;
   Sorensen, P.; Stancu, I.; Stevens, A.; Stiegler, T. M.; Stifter, K.;
   Szydagis, M.; Taylor, W. C.; Taylor, R.; Temples, D.; Terman, P. A.;
   Tiedt, D. R.; Timalsina, M.; Tomás, A.; Tripathi, M.; Tvrznikova,
   L.; Utku, U.; Uvarov, S.; Vacheret, A.; Wang, J. J.; Watson, J. R.;
   Webb, R. C.; White, R. G.; Whitis, T. J.; Wolfs, F. L. H.; Woodward,
   D.; Yin, J.; Lux-Zeplin (Lz) Collaboration
2020APh...11602391A    Altcode: 2019arXiv190402112A
  Deep underground environments are ideal for low background searches due
  to the attenuation of cosmic rays by passage through the earth. However,
  they are affected by backgrounds from γ-rays emitted by <SUP>40</SUP>K
  and the <SUP>238</SUP>U and <SUP>232</SUP>Th decay chains in the
  surrounding rock. The LUX-ZEPLIN (LZ) experiment will search for dark
  matter particle interactions with a liquid xenon TPC located within the
  Davis campus at the Sanford Underground Research Facility, Lead, South
  Dakota, at the 4850-foot level. In order to characterise the cavern
  background, in-situ γ-ray measurements were taken with a sodium iodide
  detector in various locations and with lead shielding. The integral
  count rates (0-3300 keV) varied from 596 Hz to 1355 Hz for unshielded
  measurements, corresponding to a total flux from the cavern walls of
  1.9 ± 0.4 γ cm-<SUP>2</SUP>s-<SUP>1</SUP>. The resulting activity
  in the walls of the cavern can be characterised as 220 ± 60 Bq/kg of
  <SUP>40</SUP>K, 29 ± 15 Bq/kg of <SUP>238</SUP>U, and 13 ± 3 Bq/kg
  of <SUP>232</SUP>Th.

---------------------------------------------------------
Title: Exploring Flaring Behaviour on Low Mass Stars, Solar-type
    Stars and the Sun
Authors: Doyle, L.; Ramsay, G.; Doyle, J. G.; Wyper, P. F.; Scullion,
   E.; Wu, K.; McLaughlin, J. A.
2020IAUS..354..384D    Altcode:
  We report on our project to study the activity in both the Sun and low
  mass stars. Utilising high cadence, Hα observations of a filament
  eruption made using the CRISP spectropolarimeter mounted on the
  Swedish Solar Telescope has allowed us to determine 3D velocity maps
  of the event. To gain insight into the physical mechanism which drives
  the event we have qualitatively compared our observation to a 3D MHD
  reconnection model. Solar-type and low mass stars can be highly active
  producing flares with energies exceeding erg. Using K2 and TESS data
  we find no correlation between the number of flares and the rotation
  phase which is surprising. Our solar flare model can be used to aid
  our understanding of the origin of flares in other stars. By scaling
  up our solar model to replicate observed stellar flare energies,
  we investigate the conditions needed for such high energy flares.

---------------------------------------------------------
Title: Pan-STARRS Search for Kilonovae: discovery of PS19hgw, an
    intrinsically faint transient in KUG 0152+311 (144 Mpc)
Authors: S; McLaughlin; Smartt, S. J.; Smith, K. W.; Chambers, K. C.;
   Huber, M.; Srivastav, S.; McBrien, O.; Young, D. R.; Gillanders, J.;
   O'Neill, D.; Clark, P.; Sim, S.; Boer, T. D.; Bulger, J.; Fairlamb,
   J.; Lin, C. C.; Lowe, T.; Magnier, E.; Schultz, A.; Wainscoat, R. J.;
   Willman, M.; Chen, T. W.; Wright, D. E.; Stubbs, C.; Rest, A.
2019TNSAN.154....1S    Altcode:
  We are carrying out the "Pan-STARRS Search for Kilonovae" which is a
  focused search for intrinsically faint transients, or rapidly evolving
  transients in galaxies which are closer than 200 Mpc in the ongoing
  Pan-STARRS Near Earth Object surveys (see Smartt et al. AstroNote
  2019-48 for details). Here we report the discovery of an intrinsically
  faint transient PS19hgw (AT2019wxt) in the host galaxy KUG 0152+311, at
  a redshift of z = 0.036, or d = 144 Mpc (from NED). It has an absolute
  magnitude at discovery of M_i = -16.6. We note that this is in the 80%
  contour of the skymap of the possible BNS gravitational wave source
  S191213g (the LALInference.fits.gz, The LIGO Scientific Collaboration
  and the Virgo Collaboration, GCN 26402), was discovered after the merger
  time, and is at a distance consistent with the parameter estimation
  of LVC for this event.

---------------------------------------------------------
Title: Observations and 3D Magnetohydrodynamic Modeling of a Confined
    Helical Jet Launched by a Filament Eruption
Authors: Doyle, Lauren; Wyper, Peter F.; Scullion, Eamon; McLaughlin,
   James A.; Ramsay, Gavin; Doyle, J. Gerard
2019ApJ...887..246D    Altcode: 2019arXiv191202133D
  We present a detailed analysis of a confined filament eruption
  and jet associated with a C1.5 class solar flare. Multi-wavelength
  observations from the Global Oscillations Network Group and Solar
  Dynamics Observatory reveal the filament forming over several days
  following the emergence and then partial cancellation of a minority
  polarity spot within a decaying bipolar active region. The emergence
  is also associated with the formation of a 3D null point separatrix
  that surrounds the minority polarity. The filament eruption occurs
  concurrently with brightenings adjacent to and below the filament,
  suggestive of breakout and flare reconnection, respectively. The
  erupting filament material becomes partially transferred into a
  strong outflow jet (∼60 km s<SUP>-1</SUP>) along coronal loops,
  becoming guided back toward the surface. Utilizing high-resolution
  Hα observations from the Swedish Solar Telescope/CRisp Imaging
  SpectroPolarimeter, we construct velocity maps of the outflows,
  demonstrating their highly structured but broadly helical nature. We
  contrast the observations with a 3D magnetohydrodynamic simulation
  of a breakout jet in a closed-field background and find close
  qualitative agreement. We conclude that the suggested model provides
  an intuitive mechanism for transferring twist/helicity in confined
  filament eruptions, thus validating the applicability of the breakout
  model not only to jets and coronal mass ejections but also to confined
  eruptions and flares.

---------------------------------------------------------
Title: A Blueprint of State-of-the-art Techniques for Detecting
    Quasi-periodic Pulsations in Solar and Stellar Flares
Authors: Broomhall, Anne-Marie; Davenport, James R. A.; Hayes, Laura
   A.; Inglis, Andrew R.; Kolotkov, Dmitrii Y.; McLaughlin, James A.;
   Mehta, Tishtrya; Nakariakov, Valery M.; Notsu, Yuta; Pascoe, David J.;
   Pugh, Chloe E.; Van Doorsselaere, Tom
2019ApJS..244...44B    Altcode: 2019arXiv191008458B
  Quasi-periodic pulsations (QPPs) appear to be a common feature observed
  in the light curves of both solar and stellar flares. However, their
  quasi-periodic nature, along with the fact that they can be small
  in amplitude and short-lived, makes QPPs difficult to unequivocally
  detect. In this paper, we test the strengths and limitations of
  state-of-the-art methods for detecting QPPs using a series of
  hare-and-hounds exercises. The hare simulated a set of flares,
  both with and without QPPs of a variety of forms, while the hounds
  attempted to detect QPPs in blind tests. We use the results of these
  exercises to create a blueprint for anyone who wishes to detect QPPs
  in real solar and stellar data. We present eight clear recommendations
  to be kept in mind for future QPP detections, with the plethora of
  solar and stellar flare data from new and future satellites. These
  recommendations address the key pitfalls in QPP detection, including
  detrending, trimming data, accounting for colored noise, detecting
  stationary-period QPPs, detecting QPPs with nonstationary periods,
  and ensuring that detections are robust and false detections are
  minimized. We find that QPPs can be detected reliably and robustly
  by a variety of methods, which are clearly identified and described,
  if the appropriate care and due diligence are taken.

---------------------------------------------------------
Title: The LUX-ZEPLIN (LZ) Experiment
Authors: The LZ Collaboration; Akerib, D. S.; Akerlof, C. W.; Akimov,
   D. Yu.; Alquahtani, A.; Alsum, S. K.; Anderson, T. J.; Angelides, N.;
   Araújo, H. M.; Arbuckle, A.; Armstrong, J. E.; Arthurs, M.; Auyeung,
   H.; Bai, X.; Bailey, A. J.; Balajthy, J.; Balashov, S.; Bang, J.;
   Barry, M. J.; Barthel, J.; Bauer, D.; Bauer, P.; Baxter, A.; Belle, J.;
   Beltrame, P.; Bensinger, J.; Benson, T.; Bernard, E. P.; Bernstein,
   A.; Bhatti, A.; Biekert, A.; Biesiadzinski, T. P.; Birrittella, B.;
   Boast, K. E.; Bolozdynya, A. I.; Boulton, E. M.; Boxer, B.; Bramante,
   R.; Branson, S.; Brás, P.; Breidenbach, M.; Buckley, J. H.; Bugaev,
   V. V.; Bunker, R.; Burdin, S.; Busenitz, J. K.; Campbell, J. S.;
   Carels, C.; Carlsmith, D. L.; Carlson, B.; Carmona-Benitez, M. C.;
   Cascella, M.; Chan, C.; Cherwinka, J. J.; Chiller, A. A.; Chiller,
   C.; Chott, N. I.; Cole, A.; Coleman, J.; Colling, D.; Conley, R. A.;
   Cottle, A.; Coughlen, R.; Craddock, W. W.; Curran, D.; Currie, A.;
   Cutter, J. E.; da Cunha, J. P.; Dahl, C. E.; Dardin, S.; Dasu, S.;
   Davis, J.; Davison, T. J. R.; de Viveiros, L.; Decheine, N.; Dobi,
   A.; Dobson, J. E. Y.; Druszkiewicz, E.; Dushkin, A.; Edberg, T. K.;
   Edwards, W. R.; Edwards, B. N.; Edwards, J.; Elnimr, M. M.; Emmet,
   W. T.; Eriksen, S. R.; Faham, C. H.; Fan, A.; Fayer, S.; Fiorucci,
   S.; Flaecher, H.; Fogarty Florang, I. M.; Ford, P.; Francis, V. B.;
   Froborg, F.; Fruth, T.; Gaitskell, R. J.; Gantos, N. J.; Garcia, D.;
   Geffre, A.; Gehman, V. M.; Gelfand, R.; Genovesi, J.; Gerhard, R. M.;
   Ghag, C.; Gibson, E.; Gilchriese, M. G. D.; Gokhale, S.; Gomber,
   B.; Gonda, T. G.; Greenall, A.; Greenwood, S.; Gregerson, G.; van
   der Grinten, M. G. D.; Gwilliam, C. B.; Hall, C. R.; Hamilton, D.;
   Hans, S.; Hanzel, K.; Harrington, T.; Harrison, A.; Hasselkus, C.;
   Haselschwardt, S. J.; Hemer, D.; Hertel, S. A.; Heise, J.; Hillbrand,
   S.; Hitchcock, O.; Hjemfelt, C.; Hoff, M. D.; Holbrook, B.; Holtom,
   E.; Y-K. Hor, J.; Horn, M.; Huang, D. Q.; Hurteau, T. W.; Ignarra,
   C. M.; Irving, M. N.; Jacobsen, R. G.; Jahangir, O.; Jeffery, S. N.;
   Ji, W.; Johnson, M.; Johnson, J.; Johnson, P.; Jones, W. G.; Kaboth,
   A. C.; Kamaha, A.; Kamdin, K.; Kasey, V.; Kazkaz, K.; Keefner, J.;
   Khaitan, D.; Khaleeq, M.; Khazov, A.; Khromov, A. V.; Khurana, I.;
   Kim, Y. D.; Kim, W. T.; Kocher, C. D.; Konovalov, A. M.; Korley,
   L.; Korolkova, E. V.; Koyuncu, M.; Kras, J.; Kraus, H.; Kravitz,
   S. W.; Krebs, H. J.; Kreczko, L.; Krikler, B.; Kudryavtsev, V. A.;
   Kumpan, A. V.; Kyre, S.; Lambert, A. R.; Landerud, B.; Larsen, N. A.;
   Laundrie, A.; Leason, E. A.; Lee, H. S.; Lee, J.; Lee, C.; Lenardo,
   B. G.; Leonard, D. S.; Leonard, R.; Lesko, K. T.; Levy, C.; Li, J.;
   Liu, Y.; Liao, J.; Liao, F. -T.; Lin, J.; Lindote, A.; Linehan, R.;
   Lippincott, W. H.; Liu, R.; Liu, X.; Loniewski, C.; Lopes, M. I.;
   López Paredes, B.; Lorenzon, W.; Lucero, D.; Luitz, S.; Lyle,
   J. M.; Lynch, C.; Majewski, P. A.; Makkinje, J.; Malling, D. C.;
   Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou, N.; Markley,
   D. J.; MarrLaundrie, P.; Martin, T. J.; Marzioni, M. F.; Maupin,
   C.; McConnell, C. T.; McKinsey, D. N.; McLaughlin, J.; Mei, D. -M.;
   Meng, Y.; Miller, E. H.; Minaker, Z. J.; Mizrachi, E.; Mock, J.;
   Molash, D.; Monte, A.; Monzani, M. E.; Morad, J. A.; Morrison, E.;
   Mount, B. J.; Murphy, A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.;
   Nehrkorn, C.; Nelson, H. N.; Nesbit, J.; Neves, F.; Nikkel, J. A.;
   Nikoleyczik, J. A.; Nilima, A.; O'Dell, J.; Oh, H.; O'Neill, F. G.;
   O'Sullivan, K.; Olcina, I.; Olevitch, M. A.; Oliver-Mallory, K. C.;
   Oxborough, L.; Pagac, A.; Pagenkopf, D.; Pal, S.; Palladino, K. J.;
   Palmaccio, V. M.; Palmer, J.; Pangilinan, M.; Patton, S. J.; Pease,
   E. K.; Penning, B. P.; Pereira, G.; Pereira, C.; Peterson, I. B.;
   Piepke, A.; Pierson, S.; Powell, S.; Preece, R. M.; Pushkin, K.;
   Qie, Y.; Racine, M.; Ratcliff, B. N.; Reichenbacher, J.; Reichhart,
   L.; Rhyne, C. A.; Richards, A.; Riffard, Q.; Rischbieter, G. R. C.;
   Rodrigues, J. P.; Rose, H. J.; Rosero, R.; Rossiter, P.; Rucinski,
   R.; Rutherford, G.; Rynders, D.; Saba, J. S.; Sabarots, L.; Santone,
   D.; Sarychev, M.; Sazzad, A. B. M. R.; Schnee, R. W.; Schubnell, M.;
   Scovell, P. R.; Severson, M.; Seymour, D.; Shaw, S.; Shutt, G. W.;
   Shutt, T. A.; Silk, J. J.; Silva, C.; Skarpaas, K.; Skulski, W.; Smith,
   A. R.; Smith, R. J.; Smith, R. E.; So, J.; Solmaz, M.; Solovov, V. N.;
   Sorensen, P.; Sosnovtsev, V. V.; Stancu, I.; Stark, M. R.; Stephenson,
   S.; Stern, N.; Stevens, A.; Stiegler, T. M.; Stifter, K.; Studley, R.;
   Sumner, T. J.; Sundarnath, K.; Sutcliffe, P.; Swanson, N.; Szydagis,
   M.; Tan, M.; Taylor, W. C.; Taylor, R.; Taylor, D. J.; Temples, D.;
   Tennyson, B. P.; Terman, P. A.; Thomas, K. J.; Thomson, J. A.; Tiedt,
   D. R.; Timalsina, M.; To, W. H.; Tomás, A.; Tope, T. E.; Tripathi,
   M.; Tronstad, D. R.; Tull, C. E.; Turner, W.; Tvrznikova, L.; Utes,
   M.; Utku, U.; Uvarov, S.; Va'vra, J.; Vacheret, A.; Vaitkus, A.;
   Verbus, J. R.; Vietanen, T.; Voirin, E.; Vuosalo, C. O.; Walcott, S.;
   Waldron, W. L.; Walker, K.; Wang, J. J.; Wang, R.; Wang, L.; Wang, Y.;
   Watson, J. R.; Migneault, J.; Weatherly, S.; Webb, R. C.; Wei, W. -Z.;
   While, M.; White, R. G.; White, J. T.; White, D. T.; Whitis, T. J.;
   Wisniewski, W. J.; Wilson, K.; Witherell, M. S.; Wolfs, F. L. H.;
   Wolfs, J. D.; Woodward, D.; Worm, S. D.; Xiang, X.; Xiao, Q.; Xu,
   J.; Yeh, M.; Yin, J.; Young, I.; Zhang, C.
2019arXiv191009124T    Altcode:
  We describe the design and assembly of the LUX-ZEPLIN experiment,
  a direct detection search for cosmic WIMP dark matter particles. The
  centerpiece of the experiment is a large liquid xenon time projection
  chamber sensitive to low energy nuclear recoils. Rejection of
  backgrounds is enhanced by a Xe skin veto detector and by a liquid
  scintillator Outer Detector loaded with gadolinium for efficient
  neutron capture and tagging. LZ is located in the Davis Cavern at
  the 4850' level of the Sanford Underground Research Facility in Lead,
  South Dakota, USA. We describe the major subsystems of the experiment
  and its key design features and requirements.

---------------------------------------------------------
Title: Exploring the Properties of Transverse Waves at the Base of
    the Solar Wind
Authors: Weberg, Micah J.; Morton, Richard; McLaughlin, James; Laming,
   Martin; Ko, Yuan-Kuen
2019shin.confE.173W    Altcode:
  Transverse (or ‘Alfvénic’) waves are commonly invoked by
  theories and models to explain coronal heating and solar wind
  acceleration. However, direct measurements are sparse and most of
  what we know is derived from indirect proxies for wave activity. In
  this study, we present a large, statistical study of transverse waves
  directly observed in coronal plumes between May 2010 and May 2019
  by SDO / AIA. The data was processed using an automated version of
  the Northumbria University Wave Tracking Code (NUWT) and presents a
  detailed picture of wave properties at the base of the solar wind. We
  find that the bulk wave parameters within the time periods analysed
  are largely consistent over most of a solar cycle. However, there is
  some evidence for smaller-scale variations with height, latitude, and
  over time periods of a few years. We will also explore the possibility
  of frequency-dependant processes which may give limits on the height
  at which wave dissipation, and thereby solar wind acceleration,
  begins. Lastly, we will give estimates for the total energy flux
  contained in the waves and discuss how it compares to the energy
  required to accelerate the solar wind.

---------------------------------------------------------
Title: Damping of Propagating Kink Waves in the Solar Corona
Authors: Tiwari, Ajay K.; Morton, Richard J.; Régnier, Stéphane;
   McLaughlin, James A.
2019ApJ...876..106T    Altcode: 2019arXiv190408834T
  Alfvénic waves have gained renewed interest since the existence of
  ubiquitous propagating kink waves were discovered in the corona. It
  has long been suggested that Alfvénic waves play an important role
  in coronal heating and the acceleration of the solar wind. To this
  effect, it is imperative to understand the mechanisms that enable their
  energy to be transferred to the plasma. Mode conversion via resonant
  absorption is believed to be one of the main mechanisms for kink wave
  damping and it is considered to play a key role in the process of energy
  transfer. This study examines the damping of propagating kink waves in
  quiescent coronal loops using the Coronal Multi-channel Polarimeter. A
  coherence-based method is used to track the Doppler velocity signal
  of the waves, which enables us to investigate the spatial evolution of
  velocity perturbations. The power ratio of outward to inward propagating
  waves is used to estimate the associated damping lengths and quality
  factors. To enable accurate estimates of these quantities, we provide
  the first derivation of a likelihood function suitable for fitting
  models to the ratio of two power spectra obtained from discrete Fourier
  transforms. Maximum likelihood estimation is used to fit an exponential
  damping model to the observed variation in power ratio as a function
  of frequency. We confirm earlier indications that propagating kink
  waves are undergoing frequency-dependent damping. Additionally, we find
  that the rate of damping decreases, or equivalently the damping length
  increases, for longer coronal loops that reach higher in the corona.

---------------------------------------------------------
Title: 3D WKB solution for fast magnetoacoustic wave behaviour within
    a separatrix dome containing a coronal null point
Authors: McLaughlin, James A.; Thurgood, Jonathan O.; Botha, Gert
   J. J.; Wiggs, Joshua A.
2019MNRAS.484.1390M    Altcode: 2019MNRAS.tmp..133M
  The propagation of the fast magnetoacoustic wave is studied within a
  magnetic topology containing a 3D coronal null point whose fan field
  lines form a dome. The topology is constructed from a magnetic dipole
  embedded within a global uniform field. This study aims to improve the
  understanding of how magnetohydrodynamics (MHD) waves propagate through
  inhomogeneous media, specifically in a medium containing an isolated 3D
  magnetic null point. We consider the linearized MHD equations for an
  inhomogeneous, ideal, cold plasma. The equations are solved utilizing
  the WKB approximation and Charpit's Method. We find that for a planar
  fast wave generated below the null point, the resultant propagation is
  strongly dependent upon initial location and that there are two main
  behaviours: the majority of the wave escapes the null (experiencing
  different severities of refraction depending upon the interplay with the
  equilibrium Alfvén-speed profile) or, alternatively, part of the wave
  is captured by the coronal null point (for elements generated within
  a specific critical radius about the spine and on the z = 0 plane). We
  also generalize the magnetic topology and find that the height of the
  null determines the amount of wave that is captured. We conclude that
  for a wavefront generated below the null point, nulls at a greater
  height can trap proportionally less of the corresponding wave energy.

---------------------------------------------------------
Title: On the periodicity of linear and nonlinear oscillatory
    reconnection
Authors: Thurgood, J. O.; Pontin, D. I.; McLaughlin, J. A.
2019A&A...621A.106T    Altcode: 2018arXiv181108831T
  Context. An injection of energy towards a magnetic null point can
  drive reversals of current-sheet polarity leading to time-dependent,
  oscillatory reconnection (OR), which may explain periodic phenomena
  generated when reconnection occurs in the solar atmosphere. However, the
  details of what controls the period of these current-sheet oscillations
  in realistic systems is poorly understood, despite being of crucial
  importance in assessing whether a specific model of OR can account for
  observed periodic behaviour. <BR /> Aims: This paper aims to highlight
  that different types of reconnection reversal are supported about
  null points, and that these can be distinct from the oscillation
  in the closed-boundary, linear systems considered by a number of
  authors in the 1990s. In particular, we explore the features of a
  nonlinear oscillation local to the null point, and examine the effect
  of resistivity and perturbation energy on the period, contrasting it to
  the linear, closed-boundary case. <BR /> Methods: Numerical simulations
  of the single-fluid, resistive MHD equations are used to investigate the
  effects of plasma resistivity and perturbation energy upon the resulting
  OR. <BR /> Results: It is found that for small perturbations that behave
  linearly, the inverse Lundquist number dictates the period, provided
  the perturbation energy (i.e. the free energy) is small relative to
  the inverse Lundquist number defined on the boundary, regardless of
  the broadband structure of the initial perturbation. However, when the
  perturbation energy exceeds the threshold required for "nonlinear"
  null collapse to occur, a complex oscillation of the magnetic
  field is produced which is, at most, only weakly-dependent on the
  resistivity. The resultant periodicity is instead strongly influenced
  by the amount of free energy, with more energetic perturbations
  producing higher-frequency oscillations. <BR /> Conclusions: Crucially,
  with regards to typical solar-based and astrophysical-based input
  energies, we demonstrate that the majority far exceed the threshold
  for nonlinearity to develop. This substantially alters the properties
  and periodicity of both null collapse and subsequent OR. Therefore,
  nonlinear regimes of OR should be considered in solar and astrophysical
  contexts. <P />The movie associated to Fig. 3 is available at <A
  href="https://www.aanda.org/10.1051/0004-6361/201834369/olm">https://www.aanda.org</A>

---------------------------------------------------------
Title: A basal contribution from p-modes to the Alfvénic wave flux
    in the Sun's corona
Authors: Morton, R. J.; Weberg, M. J.; McLaughlin, J. A.
2019NatAs...3..223M    Altcode: 2019arXiv190203811M; 2019NatAs.tmp..196M
  Many cool stars possess complex magnetic fields<SUP>1</SUP> that are
  considered to undertake a central role in the structuring and energizing
  of their atmospheres<SUP>2</SUP>. Alfvénic waves are thought to
  make a critical contribution to energy transfer along these magnetic
  fields, with the potential to heat plasma and accelerate stellar
  winds<SUP>3-5</SUP>. Despite Alfvénic waves having been identified
  in the Sun's atmosphere, the nature of the basal wave energy flux
  is poorly understood. It is generally assumed that the associated
  Poynting flux is generated solely in the photosphere and propagates
  into the corona, typically through the continuous buffeting of magnetic
  fields by turbulent convective cells<SUP>4,6,7</SUP>. Here, we provide
  evidence that the Sun's internal acoustic modes also contribute to
  the basal flux of Alfvénic waves, delivering a spatially ubiquitous
  input to the coronal energy balance that is sustained over the solar
  cycle. Alfvénic waves are thus a fundamental feature of the Sun's
  corona. Acknowledging that internal acoustic modes have a key role
  in injecting additional Poynting flux into the upper atmospheres
  of Sun-like stars has potentially significant consequences for the
  modelling of stellar coronae and winds.

---------------------------------------------------------
Title: Predictions of DKIST/DL-NIRSP Observations for an Off-limb
    Kink-unstable Coronal Loop
Authors: Snow, B.; Botha, G. J. J.; Scullion, E.; McLaughlin, J. A.;
   Young, P. R.; Jaeggli, S. A.
2018ApJ...863..172S    Altcode: 2018arXiv180704972S
  Synthetic intensity maps are generated from a 3D kink-unstable flux
  rope simulation using several DKIST/DL-NIRSP spectral lines to make
  a prediction of the observational signatures of energy transport and
  release. The reconstructed large field-of-view intensity mosaics and
  single tile sit-and-stare high-cadence image sequences show detailed,
  fine-scale structure and exhibit signatures of wave propagation,
  redistribution of heat, flows, and fine-scale bursts. These fine-scale
  bursts are present in the synthetic Doppler velocity maps and can be
  interpreted as evidence for small-scale magnetic reconnection at the
  loop boundary. The spectral lines reveal the different thermodynamic
  structures of the loop, with the hotter lines showing the loop
  interior and braiding and the cooler lines showing the radial edges
  of the loop. The synthetic observations of DL-NIRSP are found to
  preserve the radial expansion, and hence the loop radius can be
  measured accurately. The electron number density can be estimated
  using the intensity ratio of the Fe XIII lines at 10747 and 10798
  Å. The estimated density from this ratio is correct to within ±10%
  during the later phases of the evolution; however, it is less accurate
  initially when line-of-sight density inhomogeneities contribute to the
  Fe XIII intensity, resulting in an overprediction of the density by
  ≈30%. The identified signatures are all above a conservative estimate
  for instrument noise and therefore will be detectable. In summary, we
  have used forward modeling to demonstrate that the coronal off-limb
  mode of DKIST/DL-NIRSP will be able to detect multiple independent
  signatures of a kink-unstable loop and observe small-scale transient
  features including loop braiding/twisting and small-scale reconnection
  events occurring at the radial edge of the loop.

---------------------------------------------------------
Title: Resistively-limited current sheet implosions in planar
    anti-parallel (1D) and null-point containing (2D) magnetic field
    geometries
Authors: Thurgood, Jonathan O.; Pontin, David I.; McLaughlin, James A.
2018PhPl...25g2105T    Altcode: 2018arXiv180608157T
  Implosive formation of current sheets is a fundamental plasma
  process. Previous studies focused on the early time evolution, while
  here our primary aim is to explore the longer-term evolution, which
  may be critical for determining the efficiency of energy release. To
  address this problem, we investigate two closely related problems,
  namely: (i) 1D, pinched anti-parallel magnetic fields and (ii) 2D, null
  point containing fields which are locally imbalanced ("null-collapse"
  or "X-point collapse"). Within the framework of resistive MHD, we
  simulate the full nonlinear evolution through three distinct phases:
  the initial implosion, its eventual halting mechanism, and subsequent
  evolution post-halting. In a parameter study, we find that the scaling
  with resistivity of current sheet properties at the halting time is in
  good agreement—in both geometries—with that inferred from a known 1D
  similarity solution. We find that the halting of the implosions occurs
  rapidly after reaching the diffusion scale by sudden Ohmic heating of
  the dense plasma within the current sheet, which provides a pressure
  gradient sufficient to oppose further collapse and decelerate the
  converging flow. This back-pressure grows to exceed that required for
  force balance and so the post-implosion evolution is characterised by
  the consequences of the current sheet "bouncing" outwards. These are:
  (i) the launching of propagating fast MHD waves (shocks) outwards and
  (ii) the width-wise expansion of the current sheet itself. The expansion
  is only observed to stall in the 2D case, where the pressurisation
  is relieved by outflow in the reconnection jets. In the 2D case, we
  quantify the maximum amount of current sheet expansion as it scales
  with resistivity and analyse the structure of the reconnection region,
  which forms post-expansion, replete with Petschek-type slow shocks
  and fast termination shocks.

---------------------------------------------------------
Title: Implosive Collapse about Magnetic Null Points: A Quantitative
    Comparison between 2D and 3D Nulls
Authors: Thurgood, Jonathan O.; Pontin, David I.; McLaughlin, James A.
2018ApJ...855...50T    Altcode: 2018arXiv180207076T
  Null collapse is an implosive process whereby MHD waves focus their
  energy in the vicinity of a null point, forming a current sheet and
  initiating magnetic reconnection. We consider, for the first time,
  the case of collapsing 3D magnetic null points in nonlinear, resistive
  MHD using numerical simulation, exploring key physical aspects of the
  system as well as performing a detailed parameter study. We find that
  within a particular plane containing the 3D null, the plasma and current
  density enhancements resulting from the collapse are quantitatively
  and qualitatively as per the 2D case in both the linear and nonlinear
  collapse regimes. However, the scaling with resistivity of the 3D
  reconnection rate—which is a global quantity—is found to be less
  favorable when the magnetic null point is more rotationally symmetric,
  due to the action of increased magnetic back-pressure. Furthermore,
  we find that, with increasing ambient plasma pressure, the collapse
  can be throttled, as is the case for 2D nulls. We discuss this
  pressure-limiting in the context of fast reconnection in the solar
  atmosphere and suggest mechanisms by which it may be overcome. We
  also discuss the implications of the results in the context of
  null collapse as a trigger mechanism of Oscillatory Reconnection,
  a time-dependent reconnection mechanism, and also within the wider
  subject of wave-null point interactions. We conclude that, in general,
  increasingly rotationally asymmetric nulls will be more favorable in
  terms of magnetic energy release via null collapse than their more
  symmetric counterparts.

---------------------------------------------------------
Title: Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares
Authors: McLaughlin, J. A.; Nakariakov, V. M.; Dominique, M.; Jelínek,
   P.; Takasao, S.
2018SSRv..214...45M    Altcode: 2018arXiv180204180M
  Solar flare emission is detected in all EM bands and variations in flux
  density of solar energetic particles. Often the EM radiation generated
  in solar and stellar flares shows a pronounced oscillatory pattern, with
  characteristic periods ranging from a fraction of a second to several
  minutes. These oscillations are referred to as quasi-periodic pulsations
  (QPPs), to emphasise that they often contain apparent amplitude and
  period modulation. We review the current understanding of quasi-periodic
  pulsations in solar and stellar flares. In particular, we focus on
  the possible physical mechanisms, with an emphasis on the underlying
  physics that generates the resultant range of periodicities. These
  physical mechanisms include MHD oscillations, self-oscillatory
  mechanisms, oscillatory reconnection/reconnection reversal, wave-driven
  reconnection, two loop coalescence, MHD flow over-stability, the
  equivalent LCR-contour mechanism, and thermal-dynamical cycles. We
  also provide a histogram of all QPP events published in the literature
  at this time. The occurrence of QPPs puts additional constraints on
  the interpretation and understanding of the fundamental processes
  operating in flares, e.g. magnetic energy liberation and particle
  acceleration. Therefore, a full understanding of QPPs is essential in
  order to work towards an integrated model of solar and stellar flares.

---------------------------------------------------------
Title: Onset of 2D magnetic reconnection in the solar photosphere,
    chromosphere, and corona
Authors: Snow, B.; Botha, G. J. J.; McLaughlin, J. A.; Hillier, A.
2018A&A...609A.100S    Altcode: 2017arXiv171100683S
  <BR /> Aims: We aim to investigate the onset of 2D time-dependent
  magnetic reconnection that is triggered using an external (non-local)
  velocity driver located away from, and perpendicular to, an
  equilibrium Harris current sheet. Previous studies have typically
  utilised an internal trigger to initiate reconnection, for example
  initial conditions centred on the current sheet. Here, an external
  driver allows for a more naturalistic trigger as well as the study
  of the earlier stages of the reconnection start-up process. <BR />
  Methods: Numerical simulations solving the compressible, resistive
  magnetohydrodynamic (MHD) equations were performed to investigate the
  reconnection onset within different atmospheric layers of the Sun,
  namely the corona, chromosphere and photosphere. <BR /> Results: A
  reconnecting state is reached for all atmospheric heights considered,
  with the dominant physics being highly dependent on atmospheric
  conditions. The coronal case achieves a sharp rise in electric field
  (indicative of reconnection) for a range of velocity drivers. For the
  chromosphere, we find a larger velocity amplitude is required to trigger
  reconnection (compared to the corona). For the photospheric environment,
  the electric field is highly dependent on the inflow speed; a sharp
  increase in electric field is obtained only as the velocity entering
  the reconnection region approaches the Alfvén speed. Additionally,
  the role of ambipolar diffusion is investigated for the chromospheric
  case and we find that the ambipolar diffusion alters the structure
  of the current density in the inflow region. <BR /> Conclusions: The
  rate at which flux enters the reconnection region is controlled by
  the inflow velocity. This determines all aspects of the reconnection
  start-up process, that is, the early onset of reconnection is dominated
  by the advection term in Ohm's law in all atmospheric layers. A lower
  plasma-β enhances reconnection and creates a large change in the
  electric field. A high plasma-β hinders the reconnection, yielding a
  sharp rise in the electric field only when the velocity flowing into
  the reconnection region approaches the local Alfvén speed.

---------------------------------------------------------
Title: An Automated Algorithm for Identifying and Tracking Transverse
    Waves in Solar Images
Authors: Weberg, Micah J.; Morton, Richard J.; McLaughlin, James A.
2018ApJ...852...57W    Altcode: 2018arXiv180704842W
  Recent instrumentation has demonstrated that the solar atmosphere
  supports omnipresent transverse waves, which could play a key role
  in energizing the solar corona. Large-scale studies are required
  in order to build up an understanding of the general properties
  of these transverse waves. To help facilitate this, we present an
  automated algorithm for identifying and tracking features in solar
  images and extracting the wave properties of any observed transverse
  oscillations. We test and calibrate our algorithm using a set of
  synthetic data, which includes noise and rotational effects. The
  results indicate an accuracy of 1%-2% for displacement amplitudes
  and 4%-10% for wave periods and velocity amplitudes. We also apply
  the algorithm to data from the Atmospheric Imaging Assembly on board
  the Solar Dynamics Observatory and find good agreement with previous
  studies. Of note, we find that 35%-41% of the observed plumes exhibit
  multiple wave signatures, which indicates either the superposition
  of waves or multiple independent wave packets observed at different
  times within a single structure. The automated methods described
  in this paper represent a significant improvement on the speed and
  quality of direct measurements of transverse waves within the solar
  atmosphere. This algorithm unlocks a wide range of statistical studies
  that were previously impractical.

---------------------------------------------------------
Title: Annual Properties of Transverse Waves in the Corona over most
    of Solar Cycle 24
Authors: Weberg, M. J.; Morton, R. J.; McLaughlin, J. A.
2017AGUFMSH42B..07W    Altcode:
  Waves are an omnipresent feature in heliophysical plasmas. In
  particular, transverse (or "Alfvénic") waves have been observed at a
  wide range of spatial and temporal scales within the corona and solar
  wind. These waves play a key role in transporting energy through the
  solar atmosphere and are also thought to contribute to the heating and
  acceleration of the solar wind. Previous studies of low-frequency (&lt;
  10 mHz) transverse waves in coronal loops and polar plumes have provided
  tantalizing glimpses at specific time periods, however few, if any,
  systematic studies have been performed spanning long time scales. In
  this study, we combine recent advancements in the automated detection
  and measurement of low-frequency transverse waves with over 7 years
  of SDO / AIA data to provide a detailed picture of coronal transverse
  waves in polar plumes and, for the first time, begin to examine their
  long-term behaviour. We measure waves at three different heights in
  each of eight, four-hour periods spanning May 2010 - May 2017. We
  find that the bulk wave parameters within these 24 regions are largely
  consistent over most of a solar cycle. However, there is some evidence
  for smaller-scale variations both with height and over time periods
  of a few years. We also discuss total energy flux estimations based
  on the full wave power spectra, which yields a more nuanced picture
  than previous values based on summary statistics. Overall, this work
  expands our view of wave processes in the corona and is relevant to
  both theoretical and modelling considerations of energy transport
  within the solar atmosphere. Crucially, these initial results suggest
  that the energy flux provided by the low-frequency transverse waves
  varies little over the solar cycle, potentially indicating that the
  waves provide a consistent source of energy to the corona and beyond.

---------------------------------------------------------
Title: Three-dimensional Oscillatory Reconnection
Authors: Thurgood, Jonathan; Pontin, David; McLaughlin, James
2017shin.confE..88T    Altcode:
  Here we detail the dynamic evolution of localised reconnection regions
  about three-dimensional (3D) magnetic null points by using numerical
  simulation. We demonstrate for the first time that reconnection
  triggered by the localised collapse of a 3D null point due to an
  external MHD wave involves a self-generated oscillation, whereby the
  current sheet and outflow jets undergo a reconnection reversal process
  during which back-pressure formation at the jet heads acts to prise
  open the collapsed field before overshooting the equilibrium into an
  opposite-polarity configuration. The discovery that reconnection at
  fully 3D nulls can proceed naturally in a time-dependent and periodic
  fashion is suggestive that oscillatory reconnection mechanisms may play
  a role in explaining periodicity in astrophysical phenomena associated
  with magnetic reconnection, such as the observed quasi-periodicity of
  solar and stellar flare emission. Furthermore, we find a consequence
  of oscillatory reconnection is the generation of a plethora of
  freely-propagating MHD waves which escape the vicinity of the
  reconnection region.

---------------------------------------------------------
Title: Three-dimensional Oscillatory Magnetic Reconnection
Authors: Thurgood, Jonathan O.; Pontin, David I.; McLaughlin, James A.
2017ApJ...844....2T    Altcode: 2017arXiv170609662T
  Here we detail the dynamic evolution of localized reconnection regions
  about 3D magnetic null points using numerical simulation. We demonstrate
  for the first time that reconnection triggered by the localized collapse
  of a 3D null point that is due to an external magnetohydrodynamic
  (MHD) wave involves a self-generated oscillation, whereby the current
  sheet and outflow jets undergo a reconnection reversal process
  during which back-pressure formation at the jet heads acts to prise
  open the collapsed field before overshooting the equilibrium into an
  opposite-polarity configuration. The discovery that reconnection at
  fully 3D nulls can proceed naturally in a time-dependent and periodic
  fashion suggests that oscillatory reconnection mechanisms may play a
  role in explaining periodicity in astrophysical phenomena associated
  with magnetic reconnection, such as the observed quasi-periodicity
  of solar and stellar flare emission. Furthermore, we find that
  a consequence of oscillatory reconnection is the generation of a
  plethora of freely propagating MHD waves that escape the vicinity of
  the reconnection region.

---------------------------------------------------------
Title: Project SunbYte: solar astronomy on a budget
Authors: Alvarez Gonzalez, F.; Badilita, A. -M.; Baker, A.; Cho,
   Y. -H.; Dhot, N.; Fedun, V.; Hare, C.; He, T.; Hobbs, M.; Javed,
   M.; Lovesey, H.; Lord, C.; Panoutsos, G.; Permyakov, A.; Pope, S.;
   Portnell, M.; Rhodes, L.; Sharma, R.; Taras, P.; Taylor, J.; Tilbrook,
   R.; Verth, G.; Wrigley, S. N.; Yaqoob, M.; Cook, R.; McLaughlin, J.;
   Morton, R.; Scullion, E.; Shelyag, S.; Hamilton, A.; Zharkov, S.;
   Jess, D.; Wrigley, M.
2017A&G....58d2.24A    Altcode:
  The Sheffield University Nova Balloon Lifted Solar Telescope (SunbYte)
  is a high-altitude balloon experiment devised and run largely by
  students at the University of Sheffield, and is scheduled for launch
  in October 2017. It was the only UK project in 2016 to be selected for
  the balloon side of the Swedish-German student programme REXUS/BEXUS
  (Rocket and Balloon Experiments for University Students; see box on
  p2.25). The success of the SunbYte team in the REXUS/BEXUS selection
  process is an unprecedented opportunity for the students to gain
  valuable experience working in the space engineering industry, using
  their theoretical knowledge and networking with students and technology
  companies from all over Europe.

---------------------------------------------------------
Title: Erosion and Basin Modification of Smaller Complex Craters in
    the Isidis Region, Mars
Authors: McLaughlin, J. A.; Davatzes, A. K.
2017LPI....48.1190M    Altcode:
  Trends of features found / In martian crater basins / Rim degradation.

---------------------------------------------------------
Title: Automating Direct Observations of Transverse Waves in the
    Solar Corona
Authors: Weberg, M. J.; Morton, R. J.; McLaughlin, J. A.
2016AGUFMSH21E2576W    Altcode:
  A multitude of MHD waves have been observed at a large range of scales
  in the solar atmosphere. According to theories and models, transverse
  (or "Alfvénic") waves are a viable mechanism for both heating and
  accelerating the solar wind and may also drive certain elemental
  fractionation processes in the chromosphere and corona. However,
  direct measurements of transverse waves in polar plumes (Thurgood
  et al. 2014) have raised some questions concerning the total energy
  carried by the waves and whether or not it is sufficient to be a
  primary driver of either solar wind heating or acceleration. In
  this work we build upon on the framework of Morton &amp; McLaughlin
  (2013) and Thurgood et al. (2014) and extend the capabilities of the
  Northumbria University Wave Tracking (NUWT) code. In particular, we
  present an automated method of detecting and quantifying transverse
  waves in polar coronal holes. With the application of Fourier analysis
  methods, we investigate the superposition of multiple waves propagating
  along individual structures and, additionally, examine multi-variate
  relationships that may exist between wave parameters. We report the
  distributions of wave parameters for hundreds of waves observed using
  data from the 171 Å channel of SDO / AIA at select times throughout
  the solar cycle. Finally, we discuss how the measured average wave
  energy compares to theoretical predictions. The methods described in
  this research can be easily applied to other instruments, both space-
  and ground-based, and the observations of wave parameters and energetics
  place important constraints on wave-driven models of the solar corona.

---------------------------------------------------------
Title: Exploring Coronal Dynamics: A Next Generation Solar Physics
    Mission white paper
Authors: Morton, R. J.; Scullion, E.; Bloomfield, D. S.; McLaughlin,
   J. A.; Regnier, S.; McIntosh, S. W.; Tomczyk, S.; Young, P.
2016arXiv161106149M    Altcode:
  Determining the mechanisms responsible for the heating of the
  coronal plasma and maintaining and accelerating the solar wind
  are long standing goals in solar physics. There is a clear need to
  constrain the energy, mass and momentum flux through the solar corona
  and advance our knowledge of the physical process contributing to
  these fluxes. Furthermore, the accurate forecasting of Space Weather
  conditions at the near-Earth environment and, more generally, the
  plasma conditions of the solar wind throughout the heliosphere, require
  detailed knowledge of these fluxes in the near-Sun corona. Here we
  present a short case for a space-based imaging-spectrometer coronagraph,
  which will have the ability to provide synoptic information on the
  coronal environment and provide strict constraints on the mass, energy,
  and momentum flux through the corona. The instrument would ideally
  achieve cadences of $\sim10$~s, spatial resolution of 1" and observe the
  corona out to 2~$R_{\sun}$. Such an instrument will enable significant
  progress in our understanding of MHD waves throughout complex plasmas,
  as well as potentially providing routine data products to aid Space
  Weather forecasting.

---------------------------------------------------------
Title: 3D WKB solution for fast magnetoacoustic wave behaviour around
    an X-line
Authors: McLaughlin, J. A.; Botha, G. J. J.; Régnier, S.; Spoors,
   D. L.
2016A&A...591A.103M    Altcode: 2016arXiv160702379M
  Context. We study the propagation of a fast magnetoacoustic wave in
  a 3D magnetic field created from two magnetic dipoles. The magnetic
  topology contains an X-line. <BR /> Aims: We aim to contribute to the
  overall understanding of MHD wave propagation within inhomogeneous
  media, specifically around X-lines. <BR /> Methods: We investigate the
  linearised, 3D MHD equations under the assumptions of ideal and cold
  plasma. We utilise the WKB approximation and Charpit's method during
  our investigation. <BR /> Results: It is found that the behaviour
  of the fast magnetoacoustic wave is entirely dictated by the local,
  inhomogeneous, equilibrium Alfvén speed profile. All parts of the
  wave experience refraction during propagation, where the magnitude of
  the refraction effect depends on the location of an individual wave
  element within the inhomogeneous magnetic field. The X-line, along
  which the Alfvén speed is identically zero, acts as a focus for the
  refraction effect. There are two main types of wave behaviour: part
  of the wave is either trapped by the X-line or escapes the system, and
  there exists a critical starting region around the X-line that divides
  these two types of behaviour. For the set-up investigated, it is found
  that 15.5% of the fast wave energy is trapped by the X-line. <BR />
  Conclusions: We conclude that linear, β = 0 fast magnetoacoustic waves
  can accumulate along X-lines and thus these will be specific locations
  of fast wave energy deposition and thus preferential heating. The work
  here highlights the importance of understanding the magnetic topology
  of a system. We also demonstrate how the 3D WKB technique described
  in this paper can be applied to other magnetic configurations.

---------------------------------------------------------
Title: Nuwt: Northumbria University Wave Tracking (Nuwt) Code
Authors: Morton, Richard J.; Mooroogen, Krishna; McLaughlin, James A.
2016zndo.....49563M    Altcode:
  This is the first release of the Northumbria University Wave Tracking
  (NUWT) code (in IDL). The code is primarily designed to analyse
  transverse waves along curvilinear features in solar imaging data,
  however, the underlying operations will work on any images. Tutorials
  and videos are included with the release.

---------------------------------------------------------
Title: Behaviour of Magnetoacoustic Waves in the Neighbourhood of
a Two-Dimensional Null Point: Initially Cylindrically Symmetric
    Perturbations
Authors: McLaughlin, J. A.
2016JApA...37....2M    Altcode: 2016arXiv160702363M
  The propagation of magnetoacoustic waves in the neighbourhood of a 2D
  null point is investigated for both β=0 and β ≠ 0 plasmas. Previous
  work has shown that the Alfvén speed, here v <SUB> A </SUB>∝ r, plays
  a vital role in such systems and so a natural choice is to switch to
  polar coordinates. For β=0 plasma, we derive an analytical solution
  for the behaviour of the fast magnetoacoustic wave in terms of the
  Klein-Gordon equation. We also solve the system with a semi-analytical
  WKB approximation which shows that the β=0 wave focuses on the null
  and contracts around it but, due to exponential decay, never reaches
  the null in a finite time. For the β ≠ 0 plasma, we solve the system
  numerically and find the behaviour to be similar to that of the β=0
  system at large radii, but completely different close to the null. We
  show that for an initially cylindrically-symmetric fast magnetoacoustic
  wave perturbation, there is a decrease in wave speed along the
  separatrices and so the perturbation starts to take on a quasi-diamond
  shape; with the corners located along the separatrices. This is due
  to the growth in pressure gradients that reach a maximum along the
  separatrices, which in turn reduces the acceleration of the fast wave
  along the separatrices leading to a deformation of the wave morphology.

---------------------------------------------------------
Title: First Direct Measurements of Transverse Waves in Solar Polar
    Plumes Using SDO/AIA
Authors: Thurgood, J. O.; Morton, R. J.; McLaughlin, J. A.
2014ApJ...790L...2T    Altcode: 2014arXiv1406.5348T
  There is intense interest in determining the precise contribution of
  Alfvénic waves propagating along solar structures to the problems
  of coronal heating and solar wind acceleration. Since the launch of
  SDO/AIA, it has been possible to resolve transverse oscillations in
  off-limb solar polar plumes and recently McIntosh et al. concluded
  that such waves are energetic enough to play a role in heating the
  corona and accelerating the fast solar wind. However, this result is
  based on comparisons to Monte Carlo simulations and confirmation via
  direct measurements is still outstanding. Thus, this Letter reports
  on the first direct measurements of transverse wave motions in solar
  polar plumes. Over a four hour period, we measure the transverse
  displacements, periods, and velocity amplitudes of 596 distinct
  oscillations observed in the 171 Å channel of SDO/AIA. We find a
  broad range of non-uniformly distributed parameter values which are
  well described by log-normal distributions with peaks at 234 km,
  121 s, and 8 km s<SUP>-1</SUP>, and mean and standard deviations of
  407 ± 297 km, 173 ± 118 s, and 14 ± 10 km s<SUP>-1</SUP>. Within
  standard deviations, our direct measurements are broadly consistent
  with previous results. However, accounting for the whole of our observed
  non-uniform parameter distribution we calculate an energy flux of 9-24
  W m<SUP>-2</SUP>, which is 4-10 times below the energy requirement for
  solar wind acceleration. Hence, our results indicate that transverse
  magnetohydrodynamic waves as resolved by SDO/AIA cannot be the dominant
  energy source for fast solar wind acceleration in the open-field corona.

---------------------------------------------------------
Title: High-resolution Observations of Active Region Moss and its
    Dynamics
Authors: Morton, R. J.; McLaughlin, J. A.
2014ApJ...789..105M    Altcode: 2014arXiv1405.5694M
  The High Resolution Coronal Imager has provided the sharpest view
  of the EUV corona to date. In this paper, we exploit its impressive
  resolving power to provide the first analysis of the fine-scale
  structure of moss in an active region. The data reveal that the moss
  is made up of a collection of fine threads that have widths with a
  mean and standard deviation of 440 ± 190 km (FWHM). The brightest
  moss emission is located at the visible head of the fine-scale
  structure and the fine structure appears to extend into the lower
  solar atmosphere. The emission decreases along the features, implying
  that the lower sections are most likely dominated by cooler transition
  region plasma. These threads appear to be the cool, lower legs of the
  hot loops. In addition, the increased resolution allows for the first
  direct observation of physical displacements of the moss fine structure
  in a direction transverse to its central axis. Some of these transverse
  displacements demonstrate periodic behavior, which we interpret as a
  signature of kink (Alfvénic) waves. Measurements of the properties
  of the transverse motions are made and the wave motions have means
  and standard deviations of 55 ± 37 km for the transverse displacement
  amplitude, 77 ± 33 s for the period, and 4.7 ± 2.5 km s<SUP>-1</SUP>
  for the velocity amplitude. The presence of waves in the transition
  region of hot loops could have important implications for the heating
  of active regions.

---------------------------------------------------------
Title: High-resolution observations of active region moss and its
    dynamics
Authors: Morton, Richard; McLaughlin, James
2014cosp...40E2181M    Altcode:
  The High resolution Coronal Imager (Hi-C) has provided the sharpest
  view of the EUV corona to date. I will present results that exploit
  its impressive resolving power to provide the first analysis of the
  fine-scale structure of moss in an active region. The data reveal
  that the moss is made up of a collection of fine threads that have
  widths ranging between 400-1000 km. These fine-scale structures are
  connected to the bright moss and appear to extend into the lower solar
  atmosphere. The emission decreases along the features implying the
  lower sections are most likely dominated by cooler transition region
  plasma. These threads appear to be the cool, lower legs of the hot
  loops. The increased resolution also allows for the first direct
  observation of physical displacements of the moss fine-structure in
  a direction transverse to its central axis. Some of these transverse
  displacements demonstrate periodic behaviour, which we interpret as
  a signature of kink (Alfvénic) waves. The presence of waves in the
  transition region of hot loops could have important implications for
  the heating of active regions.

---------------------------------------------------------
Title: On Ponderomotive Effects Induced by Alfvén Waves in
    Inhomogeneous 2.5D MHD Plasmas
Authors: Thurgood, J. O.; McLaughlin, J. A.
2013SoPh..288..205T    Altcode: 2013arXiv1302.4340T
  Where spatial gradients in the amplitude of an Alfvén wave are
  non-zero, a nonlinear magnetic-pressure gradient acts upon the medium
  (commonly referred to as the ponderomotive force). We investigate the
  nature of such a force in inhomogeneous 2.5D MHD plasmas by analysing
  source terms in the nonlinear wave equations for the general case of
  inhomogeneous B and ρ, and consider supporting nonlinear numerical
  simulations. Our equations indicate that there are two distinct classes
  of ponderomotive effect induced by Alfvén waves in general 2.5D MHD,
  each with both a longitudinal and transverse manifestation. i) Geometric
  effects: Gradients in the pulse geometry relative to the background
  magnetic field cause the wave to sustain cospatial disturbances, the
  longitudinal and transverse daughter disturbances - where we report on
  the transverse disturbance for the first time. ii) ∇(c<SUB>A</SUB>)
  effects: Where a pulse propagates through an inhomogeneous region
  (where the gradients in the Alfvén-speed profile c<SUB>A</SUB> are
  non-zero), the nonlinear magnetic-pressure gradient acts to accelerate
  the plasma. Transverse gradients (phase mixing regions) excite
  independently propagating fast magnetoacoustic waves (generalising
  the result of Nakariakov, Roberts, and Murawski (Solar Phys.175, 93,
  1997)) and longitudinal gradients (longitudinally dispersive regions)
  perturb along the field (thus creating static disturbances in β=0,
  and slow waves in β≠0). We additionally demonstrate that mode
  conversion due the nonlinear Lorentz force is a one-way process, and
  does not act as a mechanism to nonlinearly generate Alfvén waves due to
  propagating magnetoacoustic waves. We conclude that these ponderomotive
  effects are induced by an Alfvén wave propagating in any MHD medium,
  and have the potential to have significant consequences on the dynamics
  of energy transport and aspects of dissipation provided the system is
  sufficiently nonlinear and inhomogeneous.

---------------------------------------------------------
Title: 3D Alfvén wave behaviour about proper and improper magnetic
    null points
Authors: Thurgood, J. O.; McLaughlin, J. A.
2013A&A...558A.127T    Altcode: 2013arXiv1307.7001T
  Context. Magnetohydrodynamic (MHD) waves and magnetic null points
  are both prevalent in many astrophysical plasmas, including the
  solar atmosphere. Interaction between waves and null points has been
  implicated as a possible mechanism for localised heating events. <BR
  /> Aims: Here we investigate the transient behaviour of the Alfvén
  wave about fully 3D proper and improper magnetic null points. <BR />
  Methods: We introduce an Alfvén wave into the vicinity of both proper
  and improper null points by numerically solving the ideal, β = 0 MHD
  equations using the LARE3D code. A magnetic fieldline and flux-based
  coordinate system permits the isolation of resulting wave modes and
  the analysis of their interaction. <BR /> Results: We find that the
  Alfvén wave propagates throughout the region and accumulates near the
  fan-plane, causing current build up. For different values of null point
  eccentricity, the qualitative behaviour changes only by the imposition
  of anisotropic pulse dilation, owing to the differing rates at which
  fieldlines diverge from the spine. For all eccentricities, we find that
  the fast and Alfvén waves are linearly decoupled. During the driving
  phase, an independently propagating fast wave is nonlinearly generated
  owing to the ponderomotive force. Subsequently, no further excitation of
  fast waves occurs. <BR /> Conclusions: We find that the key aspects of
  the theory of Alfvén waves about 2D null points extends intuitively to
  the fully 3D case; i.e. the wave propagates along fieldlines and thus
  accumulates at predictable parts of the topology. We also highlight
  that unlike in the 2D case, in 3D Alfvén-wave pulses are always
  toroidal, and thus any aspects of 2D Alfvén-wave-null models that
  are pulse-geometry specific must be reconsidered in 3D.

---------------------------------------------------------
Title: Phase Mixing of Alfvén Waves Near a 2D Magnetic Null Point
Authors: McLaughlin, J. A.
2013JApA...34..223M    Altcode: 2014arXiv1407.1743M; 2013JApA..tmp...23M
  The propagation of linear Alfvén wave pulses in an inhomogeneous plasma
  near a 2D coronal null point is investigated. When a uniform plasma
  density is considered, it is seen that an initially planar Alfvén
  wavefront remains planar, despite the varying equilibrium Alfvén
  speed, and that all the wave collects at the separatrices. Thus,
  in the non-ideal case, these Alfvénic disturbances preferentially
  dissipate their energy at these locations. For a non-uniform equilibrium
  density, it is found that the Alfvén wavefront is significantly
  distorted away from the initially planar geometry, inviting the
  possibility of dissipation due to phase mixing. Despite this however,
  we conclude that for the Alfvén wave, current density accumulation
  and preferential heating still primarily occur at the separatrices,
  even when an extremely non-uniform density profile is considered.

---------------------------------------------------------
Title: Hi-C and AIA observations of transverse magnetohydrodynamic
    waves in active regions (Corrigendum)
Authors: Morton, R. J.; McLaughlin, J. A.
2013A&A...556C...1M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Non-symmetric magnetohydrostatic equilibria: a multigrid
    approach
Authors: MacTaggart, D.; Elsheikh, A.; McLaughlin, J. A.; Simitev,
   R. D.
2013A&A...556A..40M    Altcode: 2013arXiv1307.6720M
  <BR /> Aims: Linear magnetohydrostatic (MHS) models of solar magnetic
  fields balance plasma pressure gradients, gravity and Lorentz
  forces where the current density is composed of a linear force-free
  component and a cross-field component that depends on gravitational
  stratification. In this paper, we investigate an efficient numerical
  procedure for calculating such equilibria. <BR /> Methods: The MHS
  equations are reduced to two scalar elliptic equations - one on the
  lower boundary and the other within the interior of the computational
  domain. The normal component of the magnetic field is prescribed on the
  lower boundary and a multigrid method is applied on both this boundary
  and within the domain to find the poloidal scalar potential. Once
  solved to a desired accuracy, the magnetic field, plasma pressure and
  density are found using a finite difference method. <BR /> Results:
  We investigate the effects of the cross-field currents on the linear
  MHS equilibria. Force-free and non-force-free examples are given to
  demonstrate the numerical scheme and an analysis of speed-up due to
  parallelization on a graphics processing unit (GPU) is presented. It
  is shown that speed-ups of ×30 are readily achievable.

---------------------------------------------------------
Title: Nonlinear Alfvén wave dynamics at a 2D magnetic null point:
    ponderomotive force
Authors: Thurgood, J. O.; McLaughlin, J. A.
2013A&A...555A..86T    Altcode: 2013arXiv1305.7073T
  Context. In the linear, β = 0 MHD regime, the transient properties of
  magnetohydrodynamic (MHD) waves in the vicinity of 2D null points are
  well known. The waves are decoupled and accumulate at predictable parts
  of the magnetic topology: fast waves accumulate at the null point;
  whereas Alfvén waves cannot cross the separatricies. However, in
  nonlinear MHD mode conversion can occur at regions of inhomogeneous
  Alfvén speed, suggesting that the decoupled nature of waves may
  not extend to the nonlinear regime. <BR /> Aims: We investigate the
  behaviour of low-amplitude Alfvén waves about a 2D magnetic null point
  in nonlinear, β = 0 MHD. <BR /> Methods: We numerically simulate
  the introduction of low-amplitude Alfvén waves into the vicinity
  of a magnetic null point using the nonlinear LARE2D code. <BR />
  Results: Unlike in the linear regime, we find that the Alfvén wave
  sustains cospatial daughter disturbances, manifest in the transverse and
  longitudinal fluid velocity, owing to the action of nonlinear magnetic
  pressure gradients (viz. the ponderomotive force). These disturbances
  are dependent on the Alfvén wave and do not interact with the medium to
  excite magnetoacoustic waves, although the transverse daughter becomes
  focused at the null point. Additionally, an independently propagating
  fast magnetoacoustic wave is generated during the early stages, which
  transports some of the initial Alfvén wave energy towards the null
  point. Subsequently, despite undergoing dispersion and phase-mixing
  due to gradients in the Alfvén-speed profile (∇c<SUB>A</SUB> ≠
  0) there is no further nonlinear generation of fast waves. <BR />
  Conclusions: We find that Alfvén waves at 2D cold null points behave
  largely as in the linear regime, however they sustain transverse and
  longitudinal disturbances - effects absent in the linear regime -
  due to nonlinear magnetic pressure gradients.

---------------------------------------------------------
Title: Hi-C and AIA observations of transverse magnetohydrodynamic
    waves in active regions
Authors: Morton, R. J.; McLaughlin, J. A.
2013A&A...553L..10M    Altcode: 2013arXiv1305.0140M
  The recent launch of the High resolution Coronal imager (Hi-C)
  provided a unique opportunity of studying the EUV corona with
  unprecedented spatial resolution. We utilize these observations
  to investigate the properties of low-frequency (50-200 s) active
  region transverse waves, whose omnipresence had been suggested
  previously. The five-fold improvement in spatial resolution over
  SDO/AIA reveals coronal loops with widths 150-310 km and that these
  loops support transverse waves with displacement amplitudes &lt;50
  km. However, the results suggest that wave activity in the coronal
  loops is of low energy, with typical velocity amplitudes &lt;3 km
  s<SUP>-1</SUP>. An extended time-series of SDO data suggests that
  low-energy wave behaviour is typical of the coronal structures both
  before and after the Hi-C observations. <P />Appendix A and five
  movies associated to Figs. A.2-A.6 are available in electronic form
  at <A href="http://www.aanda.org">http://www.aanda.org</A>

---------------------------------------------------------
Title: Numerical Simulations of Magnetoacoustic-Gravity Waves in
    the Solar Atmosphere
Authors: Murawski, K.; Srivastava, A. K.; McLaughlin, J. A.; Oliver, R.
2013SoPh..283..383M    Altcode: 2012SoPh..tmp..328M; 2012arXiv1208.5837M
  We investigate the excitation of magnetoacoustic-gravity waves
  generated from localized pulses in the gas pressure as well as in the
  vertical component of velocity. These pulses are initially launched
  at the top of the solar photosphere, which is permeated by a weak
  magnetic field. We investigate three different configurations of the
  background magnetic field lines: horizontal, vertical, and oblique to
  the gravitational force. We numerically model magnetoacoustic-gravity
  waves by implementing a realistic (VAL-C) model of the solar
  temperature. We solve the two-dimensional ideal magnetohydrodynamic
  equations numerically with the use of the FLASH code to simulate the
  dynamics of the lower solar atmosphere. The initial pulses result in
  shocks at higher altitudes. Our numerical simulations reveal that a
  small-amplitude initial pulse can produce magnetoacoustic-gravity
  waves, which are later reflected from the transition region due
  to the large-temperature gradient. The cavities in the lower solar
  atmosphere are found to have the best conditions to act as a resonator
  for various oscillations, including their trapping and leakage into
  the higher atmosphere. Our numerical simulations successfully model
  the excitation of such wave modes, their reflection and trapping,
  as well as the associated plasma dynamics.

---------------------------------------------------------
Title: On the periodicity of oscillatory reconnection
Authors: McLaughlin, J. A.; Thurgood, J. O.; MacTaggart, D.
2012A&A...548A..98M    Altcode: 2012arXiv1212.1000M
  Context. Oscillatory reconnection is a time-dependent magnetic
  reconnection mechanism that naturally produces periodic outputs
  from aperiodic drivers. <BR /> Aims: This paper aims to quantify
  and measure the periodic nature of oscillatory reconnection for the
  first time. <BR /> Methods: We solve the compressible, resistive,
  nonlinear magnetohydrodynamics (MHD) equations using 2.5D numerical
  simulations. <BR /> Results: We identify two distinct periodic regimes:
  the impulsive and stationary phases. In the impulsive phase, we find
  the greater the amplitude of the initial velocity driver, the longer
  the resultant current sheet and the earlier its formation. In the
  stationary phase, we find that the oscillations are exponentially
  decaying and for driving amplitudes 6.3-126.2 km s<SUP>-1</SUP>, we
  measure stationary-phase periods in the range 56.3-78.9 s, i.e. these
  are high frequency (0.01-0.02 Hz) oscillations. In both phases, we
  find that the greater the amplitude of the initial velocity driver, the
  shorter the resultant period, but note that different physical processes
  and periods are associated with both phases. <BR /> Conclusions: We
  conclude that the oscillatory reconnection mechanism behaves akin to
  a damped harmonic oscillator.

---------------------------------------------------------
Title: Linear and nonlinear MHD mode coupling of the fast
    magnetoacoustic wave about a 3D magnetic null point
Authors: Thurgood, J. O.; McLaughlin, J. A.
2012A&A...545A...9T    Altcode: 2012arXiv1208.5885T
  Context. Coronal magnetic null points have been implicated as possible
  locations for localised heating events in 2D models. We investigate this
  possibility about fully 3D null points. <BR /> Aims: We investigate
  the nature of the fast magnetoacoustic wave about a fully 3D magnetic
  null point, with a specific interest in its propagation, and we look
  for evidence of MHD mode coupling and/or conversion to the Alfvén
  mode. <BR /> Methods: A special fieldline and flux-based coordinate
  system was constructed to permit the introduction of a pure fast
  magnetoacoustic wave in the vicinity of proper and improper 3D null
  points. We considered the ideal, β = 0, MHD equations, which are
  solved using the LARE3D numerical code. The constituent modes of
  the resulting wave were isolated and identified using the special
  coordinate system. Numerical results were supported by analytical
  work derived from perturbation theory and a linear implementation of
  the WKB method. <BR /> Results: An initially pure fast wave is found
  to be permanently decoupled from the Alfvén mode both linearly and
  nonlinearly for both proper and improper 3D null points. The pure fast
  mode also generates and sustains a nonlinear disturbance aligned along
  the equilibrium magnetic field. The resulting pure fast magnetoacoustic
  pulse has transient behaviour, which is found to be governed by the
  (equilibrium) Alfvén-speed profile, and a refraction effect focuses
  all the wave energy towards the null point. <BR /> Conclusions:
  Thus, the main results from previous 2D work do indeed carry over
  to the fully 3D magnetic null points and so we conclude that 3D null
  points are locations for preferential heating in the corona by 3D fast
  magnetoacoustic waves.

---------------------------------------------------------
Title: Generation of Quasi-periodic Waves and Flows in the Solar
    Atmosphere by Oscillatory Reconnection
Authors: McLaughlin, J. A.; Verth, G.; Fedun, V.; Erdélyi, R.
2012ApJ...749...30M    Altcode: 2012arXiv1203.6846M
  We investigate the long-term evolution of an initially buoyant magnetic
  flux tube emerging into a gravitationally stratified coronal hole
  environment and report on the resulting oscillations and outflows. We
  perform 2.5-dimensional nonlinear numerical simulations, generalizing
  the models of McLaughlin et al. and Murray et al. We find that the
  physical mechanism of oscillatory reconnection naturally generates
  quasi-periodic vertical outflows, with a transverse/swaying aspect. The
  vertical outflows consist of both a periodic aspect and evidence
  of a positively directed flow. The speed of the vertical outflow
  (20-60 km s<SUP>-1</SUP>) is comparable to those reported in the
  observational literature. We also perform a parametric study varying
  the magnetic strength of the buoyant flux tube and find a range of
  associated periodicities: 1.75-3.5 minutes. Thus, the mechanism of
  oscillatory reconnection may provide a physical explanation to some
  of the high-speed, quasi-periodic, transverse outflows/jets recently
  reported by a multitude of authors and instruments.

---------------------------------------------------------
Title: Determination of Sub-resolution Structure of a Jet by Solar
    Magnetoseismology
Authors: Morton, R. J.; Verth, G.; McLaughlin, J. A.; Erdélyi, R.
2012ApJ...744....5M    Altcode: 2011arXiv1109.4851M
  A thin dark thread is observed in a UV/EUV solar jet in the 171 Å,
  193 Å, and 211 Å, and partially in 304 Å. The dark thread appears
  to originate in the chromosphere but its temperature does not appear
  to lie within the passbands of the Atmospheric Imaging Assembly
  onboard the Solar Dynamics Observatory. We therefore implement solar
  magnetoseismology to estimate the plasma parameters of the dark
  thread. A propagating kink (transverse) wave is observed to travel
  along the dark thread. The wave is tracked over a range of ~7000 km
  by placing multiple slits along the axis of the dark thread. The phase
  speed and amplitude of the wave are estimated and magnetoseismological
  theory is employed to determine the plasma parameters. We are able
  to estimate the plasma temperature, density gradient, magnetic field
  gradient, and sub-resolution expansion of the dark thread. The dark
  thread is found to be cool, T &lt;~ 3 × 10<SUP>4</SUP>, with both
  strong density and magnetic field gradients. The expansion of the flux
  tube along its length is ~300-400 km.

---------------------------------------------------------
Title: Review Article: MHD Wave Propagation Near Coronal Null Points
    of Magnetic Fields
Authors: McLaughlin, J. A.; Hood, A. W.; de Moortel, I.
2011SSRv..158..205M    Altcode: 2010SSRv..tmp..174M; 2010arXiv1004.5568M; 2010SSRv..tmp..157M
  We present a comprehensive review of MHD wave behaviour in the
  neighbourhood of coronal null points: locations where the magnetic
  field, and hence the local Alfvén speed, is zero. The behaviour of
  all three MHD wave modes, i.e. the Alfvén wave and the fast and slow
  magnetoacoustic waves, has been investigated in the neighbourhood
  of 2D, 2.5D and (to a certain extent) 3D magnetic null points, for
  a variety of assumptions, configurations and geometries. In general,
  it is found that the fast magnetoacoustic wave behaviour is dictated
  by the Alfvén-speed profile. In a β=0 plasma, the fast wave is
  focused towards the null point by a refraction effect and all the
  wave energy, and thus current density, accumulates close to the null
  point. Thus, null points will be locations for preferential heating
  by fast waves. Independently, the Alfvén wave is found to propagate
  along magnetic fieldlines and is confined to the fieldlines it is
  generated on. As the wave approaches the null point, it spreads out due
  to the diverging fieldlines. Eventually, the Alfvén wave accumulates
  along the separatrices (in 2D) or along the spine or fan-plane (in
  3D). Hence, Alfvén wave energy will be preferentially dissipated at
  these locations. It is clear that the magnetic field plays a fundamental
  role in the propagation and properties of MHD waves in the neighbourhood
  of coronal null points. This topic is a fundamental plasma process and
  results so far have also lead to critical insights into reconnection,
  mode-coupling, quasi-periodic pulsations and phase-mixing.

---------------------------------------------------------
Title: Phase mixing of nonlinear visco-resistive Alfvén waves
Authors: McLaughlin, J. A.; de Moortel, I.; Hood, A. W.
2011A&A...527A.149M    Altcode: 2011arXiv1101.5945M
  <BR /> Aims: We investigate the behaviour of nonlinear, nonideal Alfvén
  wave propagation within an inhomogeneous magnetic environment. <BR />
  Methods: The governing MHD equations are solved in 1D and 2D using
  both analytical techniques and numerical simulations. <BR /> Results:
  We find clear evidence for the ponderomotive effect and visco-resistive
  heating. The ponderomotive effect generates a longitudinal component
  to the transverse Alfvén wave, with a frequency twice that of the
  driving frequency. Analytical work shows the addition of resistive
  heating. This leads to a substantial increase in the local temperature
  and thus gas pressure of the plasma, resulting in material being pushed
  along the magnetic field. In 2D, our system exhibits phase mixing and
  we observe an evolution in the location of the maximum heating, i.e. we
  find a drifting of the heating layer. <BR /> Conclusions: Considering
  Alfvén wave propagation in 2D with an inhomogeneous density gradient,
  we find that the equilibrium density profile is significantly modified
  by both the flow of density due to visco-resistive heating and the
  nonlinear response to the localised heating through phase mixing.

---------------------------------------------------------
Title: A finite-difference algorithm for full waveform teleseismic
    tomography
Authors: Roecker, S.; Baker, B.; McLaughlin, J.
2010GeoJI.181.1017R    Altcode:
  We adapt a 2-D spectral domain finite difference waveform tomography
  algorithm previously used in active source seismological imaging to
  the case of a plane wave propagating through a 2.5-D viscoelastic
  medium in order to recover P and S wave speed variations from body
  waves recorded at teleseismic distances. A transferable efficacy that
  permits recovery of arbitrarily heterogenous models on moderately
  sized computers provides the primary motivation for choosing this
  algorithm. Synthetic waveforms can be generated either by specifying
  an analytic solution for a background plane wave in a 1-D model and
  solving for the source distribution that would produce it, or by solving
  for a scattered field excited by a plane wave source and then adding
  the background wavefield to it. Because the former approach typically
  involves a concentration of sources at the free surface, the latter
  tends to be more stable numerically. We adapt a gradient approach to
  solve the inverse problem to maintain tractability; calculating the
  gradient does not require much more computational effort than does
  the forward problem. The waveform tomography algorithm can be applied
  in a straightforward way to perform receiver function migration and
  traveltime inversion.

---------------------------------------------------------
Title: Impulsively generated oscillations in a 3D coronal loop
Authors: Pascoe, D. J.; de Moortel, I.; McLaughlin, J. A.
2009A&A...505..319P    Altcode:
  Aims: The effect of changing the attack angle for the interaction of
  a fast MHD wave with a 3D coronal loop is studied, to investigate
  to what extent the properties of the excited transverse kink mode
  oscillations of the loop depend on this angle. <BR />Methods: 3D
  numerical simulations are performed of the interaction of a fast
  MHD wave, generated by a pressure pulse, with a 3D coronal loop. The
  loop itself is modelled as a density enhancement (with a finite plasma
  beta) within a magnetic arcade. The initial pressure pulse has a width
  comparable to the loop diameter and is situated outside of the loop,
  at the same height as the loop apex. This height is kept fixed but
  the (horizontal) angle between the pressure pulse and the loop is
  varied. <BR />Results: We find that the global, transverse kink mode is
  efficiently excited for a range of attack angles and qualitatively in
  agreement with theoretical expectations. The period and damping time are
  found to be independent of the attack angle. For larger values of the
  attack angle, the global (longitudinal) slow wave is excited, whereas
  for intermediate values the second harmonic kink mode is also present.

---------------------------------------------------------
Title: Nonlinear fast magnetoacoustic wave propagation in the
neighbourhood of a 2D magnetic X-point: oscillatory reconnection
Authors: McLaughlin, J. A.; De Moortel, I.; Hood, A. W.; Brady, C. S.
2009A&A...493..227M    Altcode: 2009arXiv0901.1781M
  Context: This paper extends the models of Craig &amp; McClymont
  (1991, ApJ, 371, L41) and McLaughlin &amp; Hood (2004, A&amp;A,
  420, 1129) to include finite β and nonlinear effects. <BR />Aims:
  We investigate the nature of nonlinear fast magnetoacoustic waves
  about a 2D magnetic X-point. <BR />Methods: We solve the compressible
  and resistive MHD equations using a Lagrangian remap, shock capturing
  code (Arber et al. 2001, J. Comp. Phys., 171, 151) and consider an
  initial condition in {v}×{B} \cdot {hat{z}} (a natural variable of
  the system). <BR />Results: We observe the formation of both fast and
  slow oblique magnetic shocks. The nonlinear wave deforms the X-point
  into a “cusp-like” point which in turn collapses to a current
  sheet. The system then evolves through a series of horizontal and
  vertical current sheets, with associated changes in connectivity,
  i.e. the system exhibits oscillatory reconnection. Our final state is
  non-potential (but in force balance) due to asymmetric heating from
  the shocks. Larger amplitudes in our initial condition correspond to
  larger values of the final current density left in the system. <BR
  />Conclusions: The inclusion of nonlinear terms introduces several
  new features to the system that were absent from the linear regime. <P
  />A movie is available in electronic form at http://www.aanda.org

---------------------------------------------------------
Title: Influence of a dense photosphere-like layer on vertical
    oscillations of a curved coronal slab
Authors: Gruszecki, M.; Murawski, K.; McLaughlin, J. A.
2008A&A...489..413G    Altcode:
  Aims: We consider a model of a two-dimensional curved solar coronal slab
  and explore the excitation and attenuation of fast magnetoacoustic
  vertical oscillations. We include a dense photosphere-like layer
  into the physical system. <BR />Methods: The time-dependent, ideal
  magnetohydrodynamic equations are solved numerically to determine
  the spatial and temporal signatures of the impulsively excited
  oscillations. <BR />Results: The numerical results reveal that
  the inclusion of the dense photosphere-like layer has a significant
  influence on the wave period (P) and attenuation time (τ ). The wave
  characteristics exhibit a stronger dependence on the mass density
  contrast between the loop and the photosphere than on the width of the
  transition layer, according to the parametric studies performed here. We
  find that P decreases and τ /P grows with the mass density contrast
  between the photosphere-like layer and solar corona, d_ph. At the limit
  of d_ph→ ∞ , P and τ /P attain their values which correspond to
  the case when the photosphere-like layer is removed from the system
  and its action is mimicked by implementation of line-tying boundary
  conditions at the bottom boundary. <BR />Conclusions: The inclusion
  of a dense photosphere-like layer results in more efficient excitation
  and attenuation of vertical waves oscillation, compared with the case
  of line-tying boundary conditions. The enhancement of the attenuation
  rate arises from energy leakage through the photosphere-like layer.

---------------------------------------------------------
Title: 3D MHD Coronal Oscillations about a Magnetic Null Point:
    Application of WKB Theory
Authors: McLaughlin, J. A.; Ferguson, J. S. L.; Hood, A. W.
2008SoPh..251..563M    Altcode: 2007arXiv0712.1731M; 2008SoPh..tmp....8M
  This paper is a demonstration of how the WKB approximation can
  be used to help solve the linearised 3D MHD equations. Using
  Charpit's method and a Runge - Kutta numerical scheme, we have
  demonstrated this technique for a potential 3D magnetic null point,
  B=[x,εy,−(ε+1)z]. Under our cold-plasma assumption, we have
  considered two types of wave propagation: fast magnetoacoustic and
  Alfvén waves. We find that the fast magnetoacoustic wave experiences
  refraction towards the magnetic null point and that the effect of this
  refraction depends upon the Alfvén speed profile. The wave and thus the
  wave energy accumulate at the null point. We have found that current
  buildup is exponential and the exponent is dependent upon ε. Thus,
  for the fast wave there is preferential heating at the null point. For
  the Alfvén wave, we find that the wave propagates along the field
  lines. For an Alfvén wave generated along the fan plane, the wave
  accumulates along the spine. For an Alfvén wave generated across the
  spine, the value of ε determines where the wave accumulation will
  occur: fan plane (ε=1), along the x-axis (0&lt;ε&lt;1) or along the
  y-axis (ε&gt;1). We have shown analytically that currents build up
  exponentially, leading to preferential heating in these areas. The work
  described here highlights the importance of understanding the magnetic
  topology of the coronal magnetic field for the location of wave heating.

---------------------------------------------------------
Title: Three-dimensional Magnetohydrodynamic Wave Behavior in Active
Regions: Individual Loop Density Structure
Authors: McLaughlin, J. A.; Ofman, L.
2008ApJ...682.1338M    Altcode:
  We present the numerical results from a three-dimensional (3D) nonlinear
  MHD simulation of wave activity in an idealized active region in
  which individual, realistic loop density structure is included. The
  active region is modeled by an initially force-free, dipole magnetic
  configuration with gravitationally stratified density and contains a
  loop with a higher density than its surroundings. This study represents
  an extension to the model of Ofman &amp; Thompson. As found in their
  work, we see that fast wave propagation is distorted by the Alfvén
  speed profile and that the wave propagation generates field line
  oscillations, which are rapidly damped. We find that the addition of
  a high-density loop significantly changes the behavior inside that
  loop, specifically in that the loop can support trapped waves. We
  also find that the impact of the fast wave impulsively excites both
  horizontal and vertical loop oscillations. From a parametric study
  of the oscillations, we find that the amplitude of the oscillations
  decreases with increasing density contrast, whereas the period and
  damping time increase. This is one of the key results presented here:
  that individual loop density structure can influence the damping rate,
  and specifically that the damping time increases with increasing density
  contrast. All these results were compared with an additional study
  performed on a straight coronal loop with similar parameters. Through
  comparison with the straight loop, we find that the damping mechanism
  in our curved loop is wave leakage due to curvature. The work performed
  here highlights the importance of including individual loop density
  structure in the modeling of active regions and illustrates the need
  for obtaining accurate density measurements for coronal seismology.

---------------------------------------------------------
Title: 3d Simulations Of Excitation And Damping Of Waves In A Dipole
    Active Region
Authors: Selwa, Malgorzata; Ofman, L.; McLaughlin, J.
2007AAS...210.9114S    Altcode: 2007BAAS...39R.206S
  We present numerical results of three dimensional MHD model of an
  idealized active region field. The active region is initialized
  as a force-free dipole magnetic configuration with gravitationally
  stratified density and contains a loop with a higher density than
  its surroundings. This study represents an extension to the model of
  McLaughlin &amp; Ofman (2007). We examine the impact of a different
  density profiles of the loop on excitation and damping of kink waves by
  introducing a velocity or pressure pulse which models the impact of a
  flare on surrounding fields. We study the resulting loop oscillations
  and compare our results with TRACE observations.

---------------------------------------------------------
Title: 3D MHD Model of Waves in an Active Region
Authors: Ofman, L.; McLaughlin, J.
2006AGUFMSH33B0416O    Altcode:
  Wave activity associated with flares and CME's have been observed with
  SOHO, TRACE, and other satellites. The propagation and dissipation of
  the waves provide information on the coronal magnetic structures. In
  particular, MHD waves were observed in coronal active region AR8270
  following a flare with TRACE on July 14, 1998. In this study, three
  dimensional MHD model of the active region field was constructed using
  National Solar Observatory (NSO) Kitt Peak magnetogram and potential
  extrapolation of the magnetic field, together with gravitationally
  stratified density as the initial state. The model was evolved to steady
  state, and a velocity pulse with amplitude of ~100 km/sec was launched
  into the active region from below to mimic the observed effect of the
  flare. It was found that the global oscillations in the model active
  region are in good qualitative agreement with observations. The main
  difference between the observations and the model is in the oscillation
  of several individual loops that damp on longer time scale, compared
  to the corresponding magnetic field line oscillation damping in the
  model. We investigate the effects of global active region magnetic
  structure, as well as local loop structure on the trapping and damping
  of waves in the active region.

---------------------------------------------------------
Title: 3D MHD Wave Behavior in Active Regions: Trapped Modes
Authors: McLaughlin, J. A.; Ofman, L.
2006AGUFMSH33B0413M    Altcode:
  We present the numerical results of a fast magnetoacoustic wave
  propagating within an idealized active region. The active region is
  modeled by an initially force-free, dipole magnetic configuration with
  gravitationally stratified density and contains a loop with a higher
  density than its surroundings. This study represents an extension to
  the model of Ofman &amp;Thompson (2002). As found in their work, we see
  that fast wave propagation is distorted by the Alfvén speed profile
  and that the wave propagation generates fieldline oscillations and
  these oscillations are rapidly damped. Inside the high density loop,
  we find that the amplitude of these oscillations decreases as the
  density contrast, ξ, increases. We also find that the high density
  loop undergoes both vertical and horizontal oscillations. We calculate
  how the rate of wave damping in our loop varies with ξ and find a
  local minimum at about ξ=2.5, and we argue that this is evidence of
  wave trapping. Thus, this work illustrates the importance of obtaining
  accurate loop density measurements for coronal seismology.

---------------------------------------------------------
Title: MHD mode coupling in the neighbourhood of a 2D null point
Authors: McLaughlin, J. A.; Hood, A. W.
2006A&A...459..641M    Altcode: 2007arXiv0712.2402M
  Context: .At this time there does not exist a robust set of rules
  connecting low and high β waves across the β ≈ 1 layer. The work
  here contributes specifically to what happens when a low β fast
  wave crosses the β ≈ 1 layer and transforms into high β fast and
  slow waves.<BR /> Aims: .The nature of fast and slow magnetoacoustic
  waves is investigated in a finite β plasma in the neighbourhood of a
  two-dimensional null point.<BR /> Methods: .The linearised equations are
  solved in both polar and cartesian forms with a two-step Lax-Wendroff
  numerical scheme. Analytical work (e.g. small β expansion and WKB
  approximation) also complement the work.<BR /> Results: .It is found
  that when a finite gas pressure is included in magnetic equilibrium
  containing an X-type null point, a fast wave is attracted towards
  the null by a refraction effect and that a slow wave is generated
  as the wave crosses the β ≈ 1 layer. Current accumulation occurs
  close to the null and along nearby separatrices. The fast wave
  can now pass through the origin due to the non-zero sound speed,
  an effect not previously seen in related papers but clear seen for
  larger values of β. Some of the energy can now leave the region of
  the null point and there is again generation of a slow wave component
  (we find that the fraction of the incident wave converted to a slow
  wave is proportional to β). We conclude that there are two competing
  phenomena; the refraction effect (due to the variable Alfvén speed)
  and the contribution from the non-zero sound speed.<BR /> Conclusions:
  .These experiments illustrate the importance of the magnetic topology
  and of the location of the β ≈ 1 layer in the system.

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Title: Three-Dimensional MHD Models of Waves in Active Regions:
    Application to Coronal Seismology
Authors: McLaughlin, J. A.; Ofman, L.
2006ESASP.617E.102M    Altcode: 2006soho...17E.102M
  We present results from three-dimensional MHD simulations of the
  behaviour of MHD waves in 3D models of coronal active regions and
  loops. The models of the active regions are constructed by using a
  dipole magnetic field and gravitationally stratified coronal density
  structure. We compare the main features of the model with those
  seen recently by the SOHO and TRACE satellites and investigate the
  application of the results to coronal seismology. We discuss the
  possible applications of STEREO data to the improvement of our model.

---------------------------------------------------------
Title: Waves In Active Regions: Comparing Observations And 3D
    MHD Models
Authors: Ofman, Leon; McLaughlin, J.
2006SPD....37.1802O    Altcode: 2006BAAS...38..246O
  Recent TRACE observations of active regions in EUV shows waveactivity
  in coronal active regions following impulsive events.Motivated by
  these observations we construct 3D MHD models of theactive regions
  using photospheric magnetic field as boundarycondition from SOHO
  MDI or Kitt Peak data, and nonuniform densitystructure to model
  individual loops. We introduce several forms ofvelocity and density
  pulses to model the effects of impulsiveevents, such as flares,
  and follow the evolution of the modelactive region. We find good
  agreement between the observedevolution of active regions, and the 3D
  MHD models. Thus, wedemonstrate that the 3D MHD models can be used
  for coronalseismology. In the near future STEREO data may provide
  improvedinput for these models.

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Title: Magnetohydrodynamics wave propagation in the neighbourhood
    of two dipoles
Authors: McLaughlin, J. A.; Hood, A. W.
2006A&A...452..603M    Altcode: 2007arXiv0712.1784M
  Context: .This paper is the third in a series of investigations by the
  authors.<BR /> Aims: .The nature of fast magnetoacoustic and Alfvén
  waves is investigated in a 2D β=0 plasma in the neighbourhood of two
  dipoles.<BR /> Methods: .We use both numerical simulations (two-step
  Lax-Wendroff scheme) and analytical techniques (WKB approximation).<BR
  /> Results: .It is found that the propagation of the linear fast wave
  is dictated by the Alfvén speed profile and that close to the null,
  the wave is attracted to the neutral point. However, it is also found
  that in this magnetic configuration some of the wave can escape the
  refraction effect; this had not been seen in previous investigations by
  the authors. The wave split occurs near the regions of very high Alfvén
  speed (found near the loci of the two dipoles). Also, for the set-up
  investigated it was found that 40% of the wave energy accumulates at
  the null. Ohmic dissipation will then extract the wave energy at this
  point. The Alfvén wave behaves in a different manner in that part of
  the wave accumulates along the separatrices and part escapes. Hence, the
  current density will accumulate at this part of the topology and this
  is where wave heating will occur.<BR /> Conclusions: .The phenomenon
  of wave accumulation at a specific place is a feature of both wave
  types, as is the result that a fraction of the wave can now escape
  the numerical box when propagating in this magnetic configuration.

---------------------------------------------------------
Title: 3d Mhd Wave Behavior In Active Regions: Modeling Techniques
Authors: McLaughlin, James A.; Ofman, L.
2006SPD....37.0116M    Altcode: 2006BAAS...38..218M
  We have performed simulations of three-dimensional MHD wave propagation
  in models of coronal active regions. Here, we present descriptions of
  the methodology and techniques that are used in the construction of such
  simulations. These include:1) The MHD equations solved and the velocity
  perturbations used to simulate, for example, incoming EIT waves.2)
  The construction of the active region model using extrapolations of the
  observed photospheric magnetic field and gravitational stratification of
  the coronal density structure.3) The inclusion of the density structure
  of individual, realistic coronal loops using a new technique.We also
  discuss the application of the model to coronal seismology and the
  possibility of using STEREO data to the improvement of the simulations.

---------------------------------------------------------
Title: 3D MHD models of waves in active regions: application to
    coronal seismology
Authors: McLaughlin, J. A.; Ofman, L.
2006AGUSMSH52A..06M    Altcode:
  We present results from three-dimensional MHD simulations of the
  behavior of MHD waves in realistic models of coronal active regions. The
  models of the active regions are constructed by using the observed
  photospheric magnetic field and gravitationally stratified coronal
  density structure with individual loops. We compare the main features
  of the model with those seen recently by the SOHO and TRACE satellites,
  and investigate the application of the results to coronal seismology. We
  discuss the possible application of STEREO data to the improvement of
  our model.

---------------------------------------------------------
Title: MHD wave propagation in the neighbourhood of two null points
Authors: McLaughlin, J. A.; Hood, A. W.
2005A&A...435..313M    Altcode: 2007arXiv0712.1809M
  The nature of fast magnetoacoustic and Alfvén waves is investigated
  in a zero β plasma in the neighbourhood of a pair of two-dimensional
  null points. This gives an indication of wave propagation in the low
  β solar corona, for a more complicated magnetic configuration than
  that looked at by McLaughlin &amp; Hood (2004, A&amp;A, 420, 1129). It
  is found that the fast wave is attracted to the null points and that
  the front of the wave slows down as it approaches the null point
  pair. Here, the wave splits and part of the wave accumulates at one
  null and the rest at the other. Current density will then accumulate
  at these points and ohmic dissipation will then extract the energy in
  the wave at these points. This suggests locations where wave heating
  will occur in the corona. The Alfvén wave behaves in a different
  manner in that the wave accumulates along the separatrices. Hence,
  the current density will accumulate at this part of the topology and
  this is where wave heating will occur. However, the phenomenon of
  wave accumulation at a specific place is a feature of both wave types,
  and illustrates the importance of studying the topology of the corona
  when considering MHD wave propagation.

---------------------------------------------------------
Title: GRB 050525a: SARA observations.
Authors: Homewood, A.; Hartmann, D. H.; Garimella, K.; Henson, G.;
   McLaughlin, J.; Brimeyer, A.
2005GCN..3491....1H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Preferential Heating in the Neighbourhood of a Two-Dimensional
    Null Point
Authors: McLaughlin, J. A.; Hood, A. W.
2004ESASP.575...74M    Altcode: 2004soho...15...74M
  No abstract at ADS

---------------------------------------------------------
Title: MHD wave propagation in the neighbourhood  of a two-dimensional
    null point
Authors: McLaughlin, J. A.; Hood, A. W.
2004A&A...420.1129M    Altcode: 2007arXiv0712.1792M
  The nature of fast magnetoacoustic and Alfvén waves is investigated
  in a zero β plasma. This gives an indication of wave propagation in
  the low β solar corona. It is found that for a two-dimensional null
  point, the fast wave is attracted to that point and the front of the
  wave slows down as it approaches the null point, causing the current
  density to accumulate there and rise rapidly. Ohmic dissipation will
  extract the energy in the wave at this point. This illustrates that
  null points play an important role in the rapid dissipation of fast
  magnetoacoustic waves and suggests the location where wave heating will
  occur in the corona. The Alfvén wave behaves in a different manner in
  that the wave energy is dissipated along the separatrices. For Alfvén
  waves that are decoupled from fast waves, the value of the plasma β
  is unimportant. However, the phenomenon of dissipating the majority
  of the wave energy at a specific place is a feature of both wave types.

---------------------------------------------------------
Title: MHD Waves in the Neighbourhood of a 2D X-Type Neutral Point
Authors: McLaughlin, J. A.; Hood, A. W.
2004ESASP.547..537M    Altcode: 2004soho...13..537M
  A linear, fast magnetoacoustic wave is generated at a boundary and
  travels towards an magnetic X-type neutral point. Due to refraction,
  the wave wraps itself around the null point, causing a large current
  to accumulate there. Simulations show that the current build up is
  exponential in time. The numerical simulations are in good agreement
  with analytic work based on a WKB solution obtained by the method
  of characteristics.

---------------------------------------------------------
Title: The Use of Zylon Fibers in ULDB Balloons
Authors: Zimmerman, M.; Seely, L.; McLaughlin, J.
2002cosp...34E2817Z    Altcode: 2002cosp.meetE2817Z
  Early in the development of the ULDB balloon, Zylon (PBO) was
  selected as the tendon material due to its favorable stress-strain
  properties. It is a next generation super fiber whose strength and
  modulus are almost double those of the p-Aramid fibers. In addition
  there are two versions of the Zylon, As Spun (AS) and High Modulus
  (HM). Data will be presented on why the HM was chosen. Early in the
  development process, it was learned that this material exhibited an
  unusual sensitivity to degradation by ambient light. This is in addition
  to the expected sensitivity to UV radiation (Ultraviolet). The fiber
  manufacturer reported all of these properties in their literature. Due
  to the operating environment of the ULDB (Ultra Long Duration Balloon)
  it is necessary to protect the tendons from both visible and UV
  radiation. Methods to protect the tendons will be discussed. In
  addition, information on the long term exposure of the braided tendon
  over a thirty-six month period in a controlled manufacturing plant
  will be provided.

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Title: Periodic Comet Swift-Tuttle (1992t)
Authors: Jones, B.; Pina, R. K.; Milone, E. F.; Sarmecanic, J. R.;
   Puetter, R. C.; McLaughlin, J.; Gehrz, R. D.; Lawrence, G.; Flugaur,
   K.; Woodward, C. E.
1992IAUC.5654....2J    Altcode:
  B. Jones and R. K. Pina, University of California at San Diego; and
  E. F. Milone, Rothney Astrophysical Observatory, University of Calgary,
  report that 11.7-micron images (0".83/pixel) of P/Swift- Tuttle were
  obtained on Nov. 7.1 and 8.1 UT by Pina, J. R. Sarmecanic, and Milone
  (field-of-view of 30" x 17") and on Nov. 12.1 and 13.1 by R. C. Puetter
  and J. McLaughlin (19" x 24"), using the UCSD 10-micron array camera
  at the Mt. Lemmon Infrared Observatory. The comet showed a decrease
  in flux of 28 percent between the two dates, going from 37.7 to 27.3
  Jy in a 5".8 beam centered on the nucleus. R. D. Gehrz, G. Lawrence,
  and K. Flugaur, University of Minnesota; and C. E. Woodward, University
  of Wyoming, report thermal infrared measurements of P/Swift-Tuttle on
  Nov. 12.0 UT using a multifilter GaGe bolometer with a 9" diaphragm
  on the 0.76-m telescope of O'Brien Observatory. The chopper throw
  placed the reference beams 45" north and south of the coma center. The
  infrared broadband magnitudes are K [6.53 (3-sigma upper limit), L =
  5.9 +/- 0.3, M = 3.0 +/- 0.3, N (7-14 microns) = -0.2 +/- 0.1, Q (18-22
  microns) [-2.0 (3-sigma upper limit). Additional photometry through the
  narrow-band IRTF silicate filter set gave magnitudes of [7.8 microns]
  = 0.7 +/- 0.3, [8.7 microns] = -0.3 +/- 0.1, [9.8 microns] = -0.7
  +/- 0.15, [10.3 microns] = -0.64 +/- 0.3, [11.6 microns] = -1.4 +/-
  0.3, and [12.5 microns] = -1.1 +/- 0.1. The data are consistent with
  continuum emission from a 367-K blackbody. There is no evidence for
  a strong 10-micron silicate emission feature.

---------------------------------------------------------
Title: An example of the Vilkovisky-de Witt effective action in
    one-loop quantum gravity.
Authors: Allen, B.; McLaughlin, J.; Ottewill, A. C.
1992mgm..conf..545A    Altcode:
  No abstract at ADS

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Title: Renormalised Energy Density on the Horizon of a Kerr Black Hole
Authors: Jensen, B.; McLaughlin, J.; Ottewill, A.
1989grg..conf..697J    Altcode:
  No abstract at ADS