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.
Bibcode: 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-1 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.
Title: The Independence of Oscillatory Reconnection Periodicity from
the Initial Pulse
Authors: Karampelas, Konstantinos; McLaughlin, James A.; Botha,
Gert J. J.; Régnier, Stéphane
Bibcode: 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.
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.
Bibcode: 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.
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.
Bibcode: 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.
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.
Bibcode: 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.
Title: Cosmogenic production of 37Ar 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
Bibcode: 2022PhRvD.105h2004A
Altcode: 2022arXiv220102858A
We estimate the amount of 37Ar 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 37Ar 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 37Ar 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 37Ar
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 37Ar
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 37Ar should be considered when planning for
future liquid-xenon-based experiments.
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
Bibcode: 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.
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.
Bibcode: 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
Bibcode: 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
Bibcode: 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.
Bibcode: 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.
Bibcode: 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 <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.
Bibcode: 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.
Bibcode: 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.
Bibcode: 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 39Ar from 40Ar 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
Bibcode: 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 39Ar in argon extracted
from underground sources, called Underground Argon (UAr), which is used
for dark-matter searches. Indeed, 39Ar 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.
Bibcode: 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 keVnr 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⊙
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.
Bibcode: 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)
×10-12 pb at a WIMP mass of 40 GeV/c2. 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.
Bibcode: 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.
Bibcode: 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
Bibcode: 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 40K
and the 238U and 232Th 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-2s-1. The resulting activity
in the walls of the cavern can be characterised as 220 ± 60 Bq/kg of
40K, 29 ± 15 Bq/kg of 238U, and 13 ± 3 Bq/kg
of 232Th.
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.
Bibcode: 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.
Bibcode: 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
Bibcode: 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-1) 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
Bibcode: 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.
Bibcode: 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
Bibcode: 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.
Bibcode: 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.
Bibcode: 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.
Bibcode: 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.
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.
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.
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.
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.