pith. sign in

arxiv: 2606.05360 · v1 · pith:JTGMSJGJnew · submitted 2026-06-03 · 🌌 astro-ph.SR

Entropy-mode imprints in the solar corona: non-exponential damping and phase shifts of compressive oscillations

Dmitrii Kolotkov , Sergey Belov , Mohamed Sherif This is my paper

Pith reviewed 2026-06-28 03:43 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords entropy modeslow magnetoacoustic wavescoronal loopsthermal conductionMHD oscillationsnon-exponential dampingphase shifts
0
0 comments X

The pith

The entropy mode imprints non-exponential damping, envelope asymmetry, and phase-shift deviations on standing slow-mode oscillations in coronal loops.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines how the entropy mode, a non-oscillatory eigenmode in magnetohydrodynamic systems, affects observable signatures in the solar corona when coupled to the slow magnetoacoustic mode through thermal conduction. In a one-dimensional model of a coronal loop, simultaneous excitation of both modes leads to their superposition in density and temperature perturbations. Because the entropy mode decays faster than the slow mode, the combined signal shows non-exponential damping in the first few cycles, asymmetric upper and lower envelopes, and shifts away from the expected quarter-period phase difference between thermodynamic and velocity perturbations. These effects provide a potential way to detect the entropy mode indirectly through its influence on compressive oscillations.

Core claim

The entropy mode produces observable non-exponential damping, envelope asymmetry, and deviations from the canonical quarter-period phase shift in standing slow-mode oscillations through its faster decay relative to the slow mode.

What carries the argument

The entropy mode, a non-propagating eigenmode whose decay is governed by thermal conduction in the coronal plasma, superposed on the standing slow mode.

Load-bearing premise

The model assumes that standing slow and entropy modes can be simultaneously excited with independent initial amplitudes in a strictly one-dimensional field-aligned geometry with only thermal conduction as the non-adiabatic process.

What would settle it

Direct measurement of purely exponential damping with symmetric envelopes and exact quarter-period phase shifts in coronal loop oscillations would contradict the predicted entropy-mode contribution.

Figures

Figures reproduced from arXiv: 2606.05360 by Dmitrii Kolotkov, Mohamed Sherif, Sergey Belov.

Figure 1
Figure 1. Figure 1: Left: the damping time of the standing slow, τslow (blue) and entropy, τentropy (red) modes, obtained from a numerical solution of Eq. (5) as a function of temperature for a loop of length L = 180 Mm and plasma density ρ0 = 3 × 10−12 kg m−3 . Right: ratio τentropy/τslow from Eq. (5) as a function of loop temperature and density (for the same loop length). Contours of τentropy/τslow = 0.3 and 0.1 are shown … view at source ↗
Figure 2
Figure 2. Figure 2: Left: relative loop temperature perturbation (black), obtained from the numerical solution of Eqs. (1)–(4) at z0 = 0.15 (normalised to the wavelength, λ0 = 2L for L = 180 Mm). The signal’s upper and lower envelopes are shown with the blue line (and red circles) and the orange line, respectively. The green dashed lines show exponential best-fits of the signal’s upper and lower envelopes at t > 3τentropy. Ri… view at source ↗
Figure 3
Figure 3. Figure 3: Panel (a): time evolution of the slow-mode component (red) and the entropy-mode component (blue) given by Eqs. (13)–(14) in the total loop temperature perturbation shown in [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: spatio-temporal evolution of the fundamental harmonic of the slow mode (circles, red), entropy mode (boxes, blue), and full numerical solution of Eqs. (1)–(4) (grey dashed) for loop temperature perturbation. The time-dependence of the slow and entropy modes is given by Eqs. (13)–(14); the spatial structure of their amplitudes AT ,slow(z) and AT ,entropy(z) is obtained as described in Section 3.3. Rig… view at source ↗
Figure 5
Figure 5. Figure 5: Top: slow-mode temperature amplitude (left) and phase shift between temperature and velocity perturbations (right) given by Eqs. (16)–(17). The horizontal dashed line in the top right panel indicates the phase shift of π/2 in the ideal adiabatic regime. Bottom: entropy-mode temperature amplitude as a function of loop temperature and density given by Eq. (18) (left) and that vs. slow-mode temperature amplit… view at source ↗
read the original abstract

Magnetohydrodynamic (MHD) waves in coronal loops provide key seismological diagnostics through their characteristic time signatures. While fast and slow magnetoacoustic modes are routinely exploited, the entropy mode, despite being another eigenmode of the system, remains largely inaccessible due to its non-propagating and non-oscillatory nature. We identify possible observable time-domain signatures of the entropy mode and its indirect effects. Our approach exploits the intrinsically non-adiabatic conditions of the solar corona, under which the entropy mode is closely linked to the compressive slow mode. We consider a one-dimensional coronal loop model with field-aligned thermal conduction, where standing slow and entropy modes are simultaneously excited. We show that the entropy mode leaves distinct imprints on the total loop temperature and density perturbations. Specifically, its rapid decay relative to the slow mode produces a non-exponential damping profile during the initial oscillation cycles and introduces a pronounced asymmetry between the upper and lower temperature and density envelopes. These effects arise naturally from the superposition of two exponentially decaying components with different damping timescales. Furthermore, deviations from the canonical quarter-period phase shift between temperature/density and velocity perturbations in the standing slow mode are explained by the entropy-mode effect. We conclude that the entropy mode may be detected through its impact on compressive oscillations. Revealing its role in non-exponential damping, envelope asymmetry, and phase shifts of compressive oscillations makes the entropy mode potentially accessible to observations and lays the foundation for solar and stellar seismological applications.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The manuscript claims that in a 1D field-aligned coronal loop model with thermal conduction, simultaneous excitation of standing slow and entropy eigenmodes produces observable imprints of the entropy mode on compressive oscillations: non-exponential damping and asymmetric envelopes in the initial cycles (arising from linear superposition of two exponentially decaying components with different timescales), plus deviations from the canonical quarter-period phase shift between velocity and thermodynamic variables.

Significance. If the model implementation and amplitude projections hold, the work would identify a concrete pathway to make the entropy mode accessible to observations via its indirect effects on slow-mode signatures, with potential seismological applications. The underlying linear superposition is mathematically direct once the modes coexist, which is a strength if the excitation amplitudes are shown to be realistic.

major comments (2)
  1. [Abstract, 1D coronal loop model paragraph] Abstract, paragraph on the 1D coronal loop model: the central claim requires that standing slow and entropy modes can be excited simultaneously with independent initial amplitudes such that the faster-decaying entropy component measurably alters damping, envelope asymmetry, and phase shifts. However, eigenmode amplitudes are fixed by projection of any physical initial condition; the manuscript does not demonstrate that realistic coronal perturbations produce an entropy-mode amplitude large enough to dominate the first few cycles or to produce phase deviations beyond those already arising from non-adiabatic effects in the slow mode alone.
  2. [Abstract] The abstract states that the reported effects arise from superposition of two exponentially decaying components, which is mathematically correct, but supplies no explicit equations for the eigenmodes, initial conditions, or numerical verification of the claimed non-exponential profiles and phase shifts. This leaves the load-bearing implementation unshown.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments on our manuscript. We address each major point below and have revised the manuscript accordingly to strengthen the presentation of initial conditions, mode projections, and references to the implementation details.

read point-by-point responses

  1. Referee: [Abstract, 1D coronal loop model paragraph] Abstract, paragraph on the 1D coronal loop model: the central claim requires that standing slow and entropy modes can be excited simultaneously with independent initial amplitudes such that the faster-decaying entropy component measurably alters damping, envelope asymmetry, and phase shifts. However, eigenmode amplitudes are fixed by projection of any physical initial condition; the manuscript does not demonstrate that realistic coronal perturbations produce an entropy-mode amplitude large enough to dominate the first few cycles or to produce phase deviations beyond those already arising from non-adiabatic effects in the slow mode alone.

    Authors: We agree that eigenmode amplitudes are determined by projection of the initial condition. The manuscript examines initial conditions corresponding to localized heating that project onto both modes with sufficient entropy-mode amplitude to produce the reported effects in the first few cycles, as verified by explicit decomposition in the results. We have added a new subsection on eigenmode projection with example calculations for heating-like perturbations, showing that moderate entropy-mode contributions are achievable and lead to observable modifications beyond pure slow-mode non-adiabatic damping. We have also revised the abstract to specify that the signatures are demonstrated for co-excited modes under such conditions. revision: partial

  2. Referee: [Abstract] The abstract states that the reported effects arise from superposition of two exponentially decaying components, which is mathematically correct, but supplies no explicit equations for the eigenmodes, initial conditions, or numerical verification of the claimed non-exponential profiles and phase shifts. This leaves the load-bearing implementation unshown.

    Authors: The abstract is a concise overview and does not contain equations, per standard journal practice. The full manuscript derives the eigenmodes in Section 2, specifies the initial conditions in Section 3, and provides numerical verification of the non-exponential damping, envelope asymmetry, and phase shifts in Section 4 with supporting figures. We have revised the abstract to reference the linear superposition explicitly and to direct readers to the relevant sections for the eigenmode equations, initial conditions, and verification. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper derives observable signatures (non-exponential damping, envelope asymmetry, phase-shift deviations) directly from linear superposition of two standing eigenmodes with distinct decay rates in the stated 1D conduction model. No parameter is fitted to data and then relabeled a prediction, no self-citation chain supplies a uniqueness theorem or ansatz, and no quantity is defined in terms of itself. The claimed effects are algebraic consequences of the assumed initial conditions and the known analytic solutions for each mode; the derivation therefore remains self-contained once the model and coexistence assumption are granted.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The abstract invokes standard MHD linearization and the existence of an entropy eigenmode under non-adiabatic conditions; no free parameters or new entities are introduced in the provided text.

axioms (2)
  • domain assumption The solar corona is intrinsically non-adiabatic, allowing coupling between slow and entropy modes via field-aligned thermal conduction.
    Stated in the abstract as the condition under which the entropy mode is linked to the compressive slow mode.
  • domain assumption A one-dimensional coronal loop geometry with only field-aligned thermal conduction is sufficient to capture the relevant dynamics.
    Explicitly adopted in the model description in the abstract.

pith-pipeline@v0.9.1-grok · 5804 in / 1131 out tokens · 27017 ms · 2026-06-28T03:43:21.690718+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

87 extracted references · 87 canonical work pages

  1. [1]

    2009, SSRv, 149, 3, doi: 10.1007/s11214-009-9561-2

    Andries, J., van Doorsselaere, T., Roberts, B., et al. 2009, SSRv, 149, 3, doi: 10.1007/s11214-009-9561-2

    work page doi:10.1007/s11214-009-9561-2 2009

  2. [2]

    A., Antolin, P., Inglis, A

    Anfinogentov, S. A., Antolin, P., Inglis, A. R., et al. 2022, SSRv, 218, 9, doi: 10.1007/s11214-021-00869-w

    work page doi:10.1007/s11214-021-00869-w 2022

  3. [3]

    2022, Frontiers in Astronomy and Space Sciences, 9, 820116, doi: 10.3389/fspas.2022.820116

    Antolin, P., & Froment, C. 2022, Frontiers in Astronomy and Space Sciences, 9, 820116, doi: 10.3389/fspas.2022.820116

    work page doi:10.3389/fspas.2022.820116 2022

  4. [4]

    D., Goffrey, T., & Ridgers, C

    Arber, T. D., Goffrey, T., & Ridgers, C. 2023, Frontiers in Astronomy and Space Sciences, 10, 1155124, doi: 10.3389/fspas.2023.1155124

    work page doi:10.3389/fspas.2023.1155124 2023

  5. [5]

    2018, Advances in Space Research, 61, 655, doi: 10.1016/j.asr.2017.09.031

    Arregui, I. 2018, Advances in Space Research, 61, 655, doi: 10.1016/j.asr.2017.09.031

    work page doi:10.1016/j.asr.2017.09.031 2018

  6. [6]

    Y., & Nakariakov, V

    Arregui, I., Kolotkov, D. Y., & Nakariakov, V. M. 2023, A&A, 677, A23, doi: 10.1051/0004-6361/202346834

    work page doi:10.1051/0004-6361/202346834 2023

  7. [7]

    2024, in Magnetohydrodynamic Processes in Solar Plasmas, ed

    Arregui, I., & Van Doorsselaere, T. 2024, in Magnetohydrodynamic Processes in Solar Plasmas, ed. A. K. Srivastava, M. Goossens, & I. Arregui, 415–450, doi: 10.1016/B978-0-32-395664-2.00015-3

    work page doi:10.1016/b978-0-32-395664-2.00015-3 2024

  8. [8]

    Title, A. M. 2002, SoPh, 206, 99, doi: 10.1023/A:1014916701283

    work page doi:10.1023/a:1014916701283 2002

  9. [9]

    R., & Teriaca, L

    Banerjee, D., Gupta, G. R., & Teriaca, L. 2011, SSRv, 158, 267, doi: 10.1007/s11214-010-9698-z

    work page doi:10.1007/s11214-010-9698-z 2011

  10. [10]

    2016, Geophysical Monograph Series, 216, 419, doi: 10.1002/9781119055006.ch24

    Banerjee, D., & Krishna Prasad, S. 2016, Geophysical Monograph Series, 216, 419, doi: 10.1002/9781119055006.ch24

    work page doi:10.1002/9781119055006.ch24 2016

  11. [11]

    2021, SSRv, 217, 76, doi: 10.1007/s11214-021-00849-0 15

    Banerjee, D., Krishna Prasad, S., Pant, V., et al. 2021, SSRv, 217, 76, doi: 10.1007/s11214-021-00849-0

    work page doi:10.1007/s11214-021-00849-0 2021

  12. [12]

    A., Goffrey, T., Arber, T

    Belov, S. A., Goffrey, T., Arber, T. D., & Kolotkov, D. Y. 2025, A&A, 693, A186, doi: 10.1051/0004-6361/202452938

    work page doi:10.1051/0004-6361/202452938 2025

  13. [13]

    A., Molevich, N

    Belov, S. A., Molevich, N. E., & Zavershinskii, D. I. 2021, SoPh, 296, 122, doi: 10.1007/s11207-021-01868-4

    work page doi:10.1007/s11207-021-01868-4 2021

  14. [14]

    2012, SoPh, 275, 41, doi: 10.1007/s11207-011-9804-8

    Boerner, P., Edwards, C., Lemen, J., et al. 2012, SoPh, 275, 41, doi: 10.1007/s11207-011-9804-8

    work page doi:10.1007/s11207-011-9804-8 2012

  15. [15]

    Schrijver, C. J. 2014, SoPh, 289, 2377, doi: 10.1007/s11207-013-0452-z

    work page doi:10.1007/s11207-013-0452-z 2014

  16. [16]

    The Astrophysical Journal , keywords =

    Kumar, P. 2016, ApJ, 830, 110, doi: 10.3847/0004-637X/830/2/110 De Moortel, I. 2009, SSRv, 149, 65, doi: 10.1007/s11214-009-9526-5 De Moortel, I., & Hood, A. W. 2003, A&A, 408, 755, doi: 10.1051/0004-6361:20030984

    work page doi:10.3847/0004-637x/830/2/110 2016

  17. [17]

    B., et al

    Dolla, L., Marqué, C., Seaton, D. B., et al. 2012, ApJL, 749, L16, doi: 10.1088/2041-8205/749/1/L16

    work page doi:10.1088/2041-8205/749/1/l16 2012

  18. [18]

    Nakariakov, V. M. 2018, ApJL, 854, L5, doi: 10.3847/2041-8213/aaaaeb

    work page doi:10.3847/2041-8213/aaaaeb 2018

  19. [19]

    Nakariakov, V. M. 2019, A&A, 632, A64, doi: 10.1051/0004-6361/201936822

    work page doi:10.1051/0004-6361/201936822 2019

  20. [20]

    J., Kolotkov, D

    Duckenfield, T. J., Kolotkov, D. Y., & Nakariakov, V. M. 2021, A&A, 646, A155, doi: 10.1051/0004-6361/202039791

    work page doi:10.1051/0004-6361/202039791 2021

  21. [21]

    2015, ApJ, 813, 33, doi: 10.1088/0004-637X/813/1/33

    Xia, C. 2015, ApJ, 813, 33, doi: 10.1088/0004-637X/813/1/33

    work page doi:10.1088/0004-637x/813/1/33 2015

  22. [22]

    V., Nakariakov, V

    Fedenev, V. V., Nakariakov, V. M., & Anfinogentov, S. A. 2024, SoPh, 299, 2, doi: 10.1007/s11207-023-02246-y

    work page doi:10.1007/s11207-023-02246-y 2024

  23. [23]

    R., & Nakariakov, V

    Goddard, C. R., & Nakariakov, V. M. 2016, A&A, 590, L5, doi: 10.1051/0004-6361/201628718

    work page doi:10.1051/0004-6361/201628718 2016

  24. [24]

    2006, Philosophical Transactions of the Royal Society of London Series A, 364, 433, doi: 10.1098/rsta.2005.1708

    Goossens, M., Andries, J., & Arregui, I. 2006, Philosophical Transactions of the Royal Society of London Series A, 364, 433, doi: 10.1098/rsta.2005.1708

    work page doi:10.1098/rsta.2005.1708 2006

  25. [25]

    Goossens, M., Andries, J., & Aschwanden, M. J. 2002, A&A, 394, L39, doi: 10.1051/0004-6361:20021378

    work page doi:10.1051/0004-6361:20021378 2002

  26. [26]

    W., Ruderman, M., Pascoe, D

    Hood, A. W., Ruderman, M., Pascoe, D. J., et al. 2013, A&A, 551, A39, doi: 10.1051/0004-6361/201220617

    work page doi:10.1051/0004-6361/201220617 2013

  27. [27]

    Astronomy and Astrophysics , keywords =

    Inglis, A. R., & Nakariakov, V. M. 2009, A&A, 493, 259, doi: 10.1051/0004-6361:200810473 14

    work page doi:10.1051/0004-6361:200810473 2009

  28. [28]

    2025, Living Reviews in Solar Physics, 22, 4, doi: 10.1007/s41116-025-00043-2

    Keppens, R., Zhou, Y., & Xia, C. 2025, Living Reviews in Solar Physics, 22, 4, doi: 10.1007/s41116-025-00043-2

    work page doi:10.1007/s41116-025-00043-2 2025

  29. [29]

    Kolotkov, D. Y. 2022, Frontiers in Astronomy and Space Sciences, 9, 402, doi: 10.3389/fspas.2022.1073664

    work page doi:10.3389/fspas.2022.1073664 2022

  30. [30]

    Y., & Nakariakov, V

    Kolotkov, D. Y., & Nakariakov, V. M. 2022, MNRAS, 514, L51, doi: 10.1093/mnrasl/slac054

    work page doi:10.1093/mnrasl/slac054 2022

  31. [31]

    Y., Nakariakov, V

    Kolotkov, D. Y., Nakariakov, V. M., & Fihosy, J. B. 2023, Physics, 5, 193, doi: 10.3390/physics5010015

    work page doi:10.3390/physics5010015 2023

  32. [32]

    Y., Nakariakov, V

    Kolotkov, D. Y., Nakariakov, V. M., Moss, G., & Shellard, P. 2021a, MNRAS, 505, 3505, doi: 10.1093/mnras/stab1587

    work page doi:10.1093/mnras/stab1587

  33. [33]

    Y., Nakariakov, V

    Kolotkov, D. Y., Nakariakov, V. M., & Zavershinskii, D. I. 2019, A&A, 628, A133, doi: 10.1051/0004-6361/201936072

    work page doi:10.1051/0004-6361/201936072 2019

  34. [34]

    Y., Zavershinskii, D

    Kolotkov, D. Y., Zavershinskii, D. I., & Nakariakov, V. M. 2021b, Plasma Physics and Controlled Fusion, 63, 124008, doi: 10.1088/1361-6587/ac36a5 Krishna Prasad, S., Banerjee, D., & Van Doorsselaere, T. 2014, ApJ, 789, 118, doi: 10.1088/0004-637X/789/2/118 Krishna Prasad, S., & Van Doorsselaere, T. 2021, ApJ, 914, 81, doi: 10.3847/1538-4357/abfb01 —. 2024...

    work page doi:10.1088/1361-6587/ac36a5 2014

  35. [35]

    E., & Inhester, B

    Kumar, P., Innes, D. E., & Inhester, B. 2013, ApJL, 779, L7, doi: 10.1088/2041-8205/779/1/L7

    work page doi:10.1088/2041-8205/779/1/l7 2013

  36. [36]

    M., & Cho, K.-S

    Kumar, P., Nakariakov, V. M., & Cho, K.-S. 2015, ApJ, 804, 4, doi: 10.1088/0004-637X/804/1/4

    work page doi:10.1088/0004-637x/804/1/4 2015

  37. [37]

    G., Kashapova, L

    Kupriyanova, E. G., Kashapova, L. K., Van Doorsselaere, T., et al. 2019, MNRAS, 483, 5499, doi: 10.1093/mnras/sty3480

    work page doi:10.1093/mnras/sty3480 2019

  38. [38]

    2020, SSRv, 216, 136, doi: 10.1007/s11214-020-00761-z

    Li, B., Antolin, P., Guo, M.-Z., et al. 2020, SSRv, 216, 136, doi: 10.1007/s11214-020-00761-z

    work page doi:10.1007/s11214-020-00761-z 2020

  39. [39]

    2017, ApJ, 842, 99, doi: 10.3847/1538-4357/aa7677

    Li, H., Liu, Y., & Vai Tam, K. 2017, ApJ, 842, 99, doi: 10.3847/1538-4357/aa7677

    work page doi:10.3847/1538-4357/aa7677 2017

  40. [40]

    2016, A&A, 595, A81, doi: 10.1051/0004-6361/201629010

    Magyar, N., & Van Doorsselaere, T. 2016, A&A, 595, A81, doi: 10.1051/0004-6361/201629010

    work page doi:10.1051/0004-6361/201629010 2016

  41. [41]

    2018, ApJ, 853, 134, doi: 10.3847/1538-4357/aaa1a3

    Mandal, S., Krishna Prasad, S., & Banerjee, D. 2018, ApJ, 853, 134, doi: 10.3847/1538-4357/aaa1a3

    work page doi:10.3847/1538-4357/aaa1a3 2018

  42. [42]

    2016, ApJ, 820, 13, doi: 10.3847/0004-637X/820/1/13

    Banerjee, D. 2016, ApJ, 820, 13, doi: 10.3847/0004-637X/820/1/13

    work page doi:10.3847/0004-637x/820/1/13 2016

  43. [43]

    Mariska, J. T. 2006, ApJ, 639, 484, doi: 10.1086/499296 Mendoza-Briceño, C. A., Erdélyi, R., & Sigalotti, L. D. G. 2004, ApJ, 605, 493, doi: 10.1086/382182 Mészárosová, H., Karlický, M., Jelínek, P., & Rybák, J. 2014, ApJ, 788, 44, doi: 10.1088/0004-637X/788/1/44 Mészárosová, H., Karlický, M., & Rybák, J. 2011, SoPh, 273, 393, doi: 10.1007/s11207-011-9794-6

    work page doi:10.1086/499296 2006

  44. [44]

    V., & Nakariakov, V

    Murawski, K., Zaqarashvili, T. V., & Nakariakov, V. M. 2011, A&A, 533, A18, doi: 10.1051/0004-6361/201116942

    work page doi:10.1051/0004-6361/201116942 2011

  45. [45]

    M., Afanasyev, A

    Nakariakov, V. M., Afanasyev, A. N., Kumar, S., & Moon, Y.-J. 2017, ApJ, 849, 62, doi: 10.3847/1538-4357/aa8ea3

    work page doi:10.3847/1538-4357/aa8ea3 2017

  46. [46]

    M., Lacey, C

    Nakariakov, V. M., Arber, T. D., Ault, C. E., et al. 2004, MNRAS, 349, 705, doi: 10.1111/j.1365-2966.2004.07537.x

    work page doi:10.1111/j.1365-2966.2004.07537.x 2004

  47. [47]

    M., & Kolotkov, D

    Nakariakov, V. M., & Kolotkov, D. Y. 2020, ARA&A, 58, 441, doi: 10.1146/annurev-astro-032320-042940

    work page doi:10.1146/annurev-astro-032320-042940 2020

  48. [48]

    M., Kosak, M

    Nakariakov, V. M., Kosak, M. K., Kolotkov, D. Y., et al. 2019, ApJL, 874, L1, doi: 10.3847/2041-8213/ab0c9f

    work page doi:10.3847/2041-8213/ab0c9f 2019

  49. [49]

    M., Zhong, S., Kolotkov, D

    Nakariakov, V. M., Zhong, S., Kolotkov, D. Y., et al. 2024a, Reviews of Modern Plasma Physics, 8, 19, doi: 10.1007/s41614-024-00160-9

    work page doi:10.1007/s41614-024-00160-9

  50. [50]

    M., Zhong, Y., & Kolotkov, D

    Nakariakov, V. M., Zhong, Y., & Kolotkov, D. Y. 2024b, MNRAS, 531, 4611, doi: 10.1093/mnras/stae1483

    work page doi:10.1093/mnras/stae1483

  51. [51]

    Goddard, C. R. 2019, ApJS, 241, 31, doi: 10.3847/1538-4365/ab0e86 Nisticò, G., Nakariakov, V. M., & Verwichte, E. 2013, A&A, 552, A57, doi: 10.1051/0004-6361/201220676

    work page doi:10.3847/1538-4365/ab0e86 2019

  52. [52]

    2002, ApJL, 580, L85, doi: 10.1086/345548

    Ofman, L., & Wang, T. 2002, ApJL, 580, L85, doi: 10.1086/345548

    work page doi:10.1086/345548 2002

  53. [53]

    J., & Davila, J

    Ofman, L., Wang, T. J., & Davila, J. M. 2012, ApJ, 754, 111, doi: 10.1088/0004-637X/754/2/111

    work page doi:10.1088/0004-637x/754/2/111 2012

  54. [54]

    R., De Moortel, I., & Hood, A

    Owen, N. R., De Moortel, I., & Hood, A. W. 2009, A&A, 494, 339, doi: 10.1051/0004-6361:200810828

    work page doi:10.1051/0004-6361:200810828 2009

  55. [55]

    2017, ApJL, 847, L5, doi: 10.3847/2041-8213/aa880f

    Pant, V., Tiwari, A., Yuan, D., & Banerjee, D. 2017, ApJL, 847, L5, doi: 10.3847/2041-8213/aa880f

    work page doi:10.3847/2041-8213/aa880f 2017

  56. [56]

    J., Anfinogentov, S., Nisticò, G., Goddard, C

    Pascoe, D. J., Anfinogentov, S., Nisticò, G., Goddard, C. R., & Nakariakov, V. M. 2017, A&A, 600, A78, doi: 10.1051/0004-6361/201629702

    work page doi:10.1051/0004-6361/201629702 2017

  57. [57]

    J., Goddard, C

    Pascoe, D. J., Goddard, C. R., Nisticò, G., Anfinogentov, S., & Nakariakov, V. M. 2016, A&A, 589, A136, doi: 10.1051/0004-6361/201628255

    work page doi:10.1051/0004-6361/201628255 2016

  58. [58]

    J., Hood, A

    Pascoe, D. J., Hood, A. W., de Moortel, I., & Wright, A. N. 2012, A&A, 539, A37, doi: 10.1051/0004-6361/201117979

    work page doi:10.1051/0004-6361/201117979 2012

  59. [59]

    K., & Wang, T

    Prasad, A., Srivastava, A. K., & Wang, T. 2021, SoPh, 296, 105, doi: 10.1007/s11207-021-01846-w

    work page doi:10.1007/s11207-021-01846-w 2021

  60. [60]

    K., Wang, T., & Sangal, K

    Prasad, A., Srivastava, A. K., Wang, T., & Sangal, K. 2022, SoPh, 297, 5, doi: 10.1007/s11207-021-01940-z

    work page doi:10.1007/s11207-021-01940-z 2022

  61. [61]

    2014, Living Reviews in Solar Physics, 11, 4, doi: 10.12942/lrsp-2014-4 —

    Reale, F. 2014, Living Reviews in Solar Physics, 11, 4, doi: 10.12942/lrsp-2014-4 —. 2016, ApJL, 826, L20, doi: 10.3847/2041-8205/826/2/L20

    work page doi:10.12942/lrsp-2014-4 2014

  62. [62]

    Ruderman, M. S. 2013, A&A, 553, A23, doi: 10.1051/0004-6361/201321175

    work page doi:10.1051/0004-6361/201321175 2013

  63. [63]

    S., Petrukhin, N

    Ruderman, M. S., Petrukhin, N. S., & Kataeva, L. Y. 2025, MNRAS, 542, 1076, doi: 10.1093/mnras/staf1310

    work page doi:10.1093/mnras/staf1310 2025

  64. [64]

    S., & Roberts, B

    Ruderman, M. S., & Roberts, B. 2002, ApJ, 577, 475, doi: 10.1086/342130

    work page doi:10.1086/342130 2002

  65. [65]

    P., & Singh, J

    Sakurai, T., Ichimoto, K., Raju, K. P., & Singh, J. 2002, SoPh, 209, 265, doi: 10.1023/A:1021297313448 15

    work page doi:10.1023/a:1021297313448 2002

  66. [66]

    J., Kauristie, K., Aylward, A

    Schrijver, C. J., Kauristie, K., Aylward, A. D., et al. 2015, Advances in Space Research, 55, 2745, doi: 10.1016/j.asr.2015.03.023

    work page doi:10.1016/j.asr.2015.03.023 2015

  67. [67]

    Selwa, M., Murawski, K., & Solanki, S. K. 2005, A&A, 436, 701, doi: 10.1051/0004-6361:20042319

    work page doi:10.1051/0004-6361:20042319 2005

  68. [68]

    2007, SoPh, 246, 187, doi: 10.1007/s11207-007-9077-4

    Luna-Cardozo, M. 2007, SoPh, 246, 187, doi: 10.1007/s11207-007-9077-4

    work page doi:10.1007/s11207-007-9077-4 2007

  69. [69]

    K., & Goossens, M

    Srivastava, A. K., & Goossens, M. 2013, ApJ, 777, 17, doi: 10.1088/0004-637X/777/1/17 Van Doorsselaere, T., Goossens, M., Magyar, N.,

    work page doi:10.1088/0004-637x/777/1/17 2013

  70. [70]

    S., & Ismayilli, R

    Ruderman, M. S., & Ismayilli, R. 2021, ApJ, 910, 58, doi: 10.3847/1538-4357/abe630 Van Doorsselaere, T., Krishna Prasad, S., Pant, V.,

    work page doi:10.3847/1538-4357/abe630 2021

  71. [71]

    2024, A&A, 683, A109, doi: 10.1051/0004-6361/202347579 Van Doorsselaere, T., Wardle, N., Del Zanna, G., et al

    Banerjee, D., & Hood, A. 2024, A&A, 683, A109, doi: 10.1051/0004-6361/202347579 Van Doorsselaere, T., Wardle, N., Del Zanna, G., et al. 2011, ApJL, 727, L32, doi: 10.1088/2041-8205/727/2/L32 Van Doorsselaere, T., Srivastava, A. K., Antolin, P., et al. 2020, SSRv, 216, 140, doi: 10.1007/s11214-020-00770-y

    work page doi:10.1051/0004-6361/202347579 2024

  72. [72]

    D., & Brady, C

    Verwichte, E., Haynes, M., Arber, T. D., & Brady, C. S. 2008, ApJ, 685, 1286, doi: 10.1086/591077

    work page doi:10.1086/591077 2008

  73. [73]

    2013, A&A, 552, A138, doi: 10.1051/0004-6361/201220456

    Antolin, P. 2013, A&A, 552, A138, doi: 10.1051/0004-6361/201220456

    work page doi:10.1051/0004-6361/201220456 2013

  74. [74]

    2011, SSRv, 158, 397, doi: 10.1007/s11214-010-9716-1

    Wang, T. 2011, SSRv, 158, 397, doi: 10.1007/s11214-010-9716-1

    work page doi:10.1007/s11214-010-9716-1 2011

  75. [75]

    2019, ApJ, 886, 2, doi: 10.3847/1538-4357/ab478f

    Wang, T., & Ofman, L. 2019, ApJ, 886, 2, doi: 10.3847/1538-4357/ab478f

    work page doi:10.3847/1538-4357/ab478f 2019

  76. [76]

    Wang, T., Ofman, L., Sun, X., Provornikova, E., & Davila, J. M. 2015, ApJL, 811, L13, doi: 10.1088/2041-8205/811/1/L13

    work page doi:10.1088/2041-8205/811/1/l13 2015

  77. [77]

    K., & Davila, J

    Wang, T., Ofman, L., Sun, X., Solanki, S. K., & Davila, J. M. 2018, ApJ, 860, 107, doi: 10.3847/1538-4357/aac38a

    work page doi:10.3847/1538-4357/aac38a 2018

  78. [78]

    2021, SSRv, 217, 34, doi: 10.1007/s11214-021-00811-0

    Wang, T., Ofman, L., Yuan, D., et al. 2021, SSRv, 217, 34, doi: 10.1007/s11214-021-00811-0

    work page doi:10.1007/s11214-021-00811-0 2021

  79. [79]

    J., Solanki, S

    Wang, T. J., Solanki, S. K., Curdt, W., et al. 2003a, A&A, 406, 1105, doi: 10.1051/0004-6361:20030858

    work page doi:10.1051/0004-6361:20030858

  80. [80]

    2003b, A&A, 402, L17, doi: 10.1051/0004-6361:20030448

    Marsch, E. 2003b, A&A, 402, L17, doi: 10.1051/0004-6361:20030448

    work page doi:10.1051/0004-6361:20030448

Showing first 80 references.