pith. sign in

arxiv: 2606.06082 · v1 · pith:QZCFZQAQnew · submitted 2026-06-04 · 🌌 astro-ph.SR

Interaction of Fast Magnetoacoustic Wave with the Localized Coronal Null and Generation of the Energetic Alfv\'en Wave Packet

Akash Bairagi , Abhishekh K. Srivastava , Sripan Mondal , T.V. Zaqarashvili , Astrid Veronig , P. Bourdin , Ding Yuan , Ryun-Young Kwon This is my paper

Pith reviewed 2026-06-27 23:37 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords fast magnetoacoustic wavesAlfvén wave packetsmagnetic null pointsmode conversionsolar coronaMHD simulationscoronal heating
0
0 comments X

The pith

Fast magnetoacoustic waves generate energetic Alfvén wave packets via mode conversion at coronal null points.

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

The paper uses 2.5D resistive MHD simulations to examine what happens when a fast magnetoacoustic wave encounters a localized magnetic null point in the solar corona. The interaction leads to mode conversion that produces an incompressible Alfvén wave packet propagating along the separatrices at the local Alfvén speed. Nonlinear effects also create field-aligned plasma flows, and a secondary fast wave emerges. Synthetic observations show the Alfvén packet produces no intensity changes, suggesting it can transport energy invisibly in certain wavelengths.

Core claim

In 2.5D resistive MHD simulations, the interaction of a fast magnetoacoustic wave with a localized coronal null point generates an Alfvén wave packet through mode conversion. Out-of-plane velocity fluctuations and in-phase magnetic field fluctuations propagate along the separatrices with the local Alfvén speed, behaving as an incompressible and energetic disturbance. Some wavefront parts refract around the null while others trap there, and nonlinear effects produce field-aligned flows, with a secondary fast wave also generated.

What carries the argument

Mode conversion at the magnetic null point, where part of the fast magnetoacoustic wavefront produces out-of-plane velocity and magnetic fluctuations that propagate along separatrices as an incompressible Alfvén packet.

Load-bearing premise

The chosen 2.5D resistive MHD setup with its specific initial conditions, resistivity, and null geometry is sufficient to capture the physical mode conversion without 3D or kinetic effects altering the outcome.

What would settle it

High-resolution coronal observations detecting incompressible velocity and magnetic fluctuations propagating along separatrices at Alfvén speed with no intensity signature after a fast wave reaches a null point would support the claim; absence of such signatures would challenge it.

Figures

Figures reproduced from arXiv: 2606.06082 by Abhishekh K. Srivastava, Akash Bairagi, Astrid Veronig, Ding Yuan, P. Bourdin, Ryun-Young Kwon, Sripan Mondal, T.V. Zaqarashvili.

Figure 1
Figure 1. Figure 1: The density map at t = 26 s is shown with bipolar magnetic field topology over plotted as cyan streamlines. The yellow dashed box is the region of interest for our further analysis and the black contour is a β = 1 region. The fast magnetoacoustic wave-like perturbations is evident in the bottom-right part moving towards the null region. An animation of real time duration 10 s showing the entire dynamics in… view at source ↗
Figure 2
Figure 2. Figure 2: First, second and third columns are v total xy (planar velocity), AIA 193 synthesized Intensity, and vz (out-of-plane velocity) map at t = 103 s, 237 s, 294 s, 376 s and 701 s, respectively. At t = 103 s, the velocity pulse is incident on the null region (black contour) and further deformed it, which is visible in v total xy , synthesized AIA 193 running difference and vz maps. In the vz map at t = 237 s a… view at source ↗
Figure 3
Figure 3. Figure 3: First column is the map of total planar Lorentz force (L total xy ) plus the plasma pressure gradient force (−∇P) at t = 103 s, 237 s, 294 s, 376 s and 701 s, respectively. The signal in the planar Lorentz force has been observed for the fast wavefront propagation, but no detectable signal is present in conjunction with the generation of vz fluctuations. Also, the magnitude of plasma pressure gradient forc… view at source ↗
Figure 4
Figure 4. Figure 4: From left to right: v total xy , vz and compressibility (∇ · ⃗ ⃗v) on the x-y plane for four time steps. The yellow and blue contour represent the fast magnetoacoustic and Alfv´en part, respectively to distinguish v total xy and vz components of the velocity. The associated velocity amplitude range of the contour has been taken 30 km s−1 to 35 km s−1 . The FOV of all the panel shown here is equivalent to t… view at source ↗
Figure 5
Figure 5. Figure 5: The left panel shows the vz map at t = 701 s with a curved slit S3, starting from right to left along the path of the propagating Alfv´en wave packet. The independent points a (yellow), b (blue), c (green), d (red), e (magenta), f (cyan), g (orange), h (purple) and i (gray) have been taken on the S3 to understand the properties of vz at different locations. Panel (A) and (B) are time-distance profiles of v… view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: Zoomed region of the plasma beta map with range 0 to 1 at t = 283 s. The black solid contour is β = 1 layer, whereas the black dotted curved slit (S2) is taken from bottom right to top left through the null region. Middle panel: time distance profile with embedded β = 1 layer of vz along S2. Through the equipartition layer the periodic fluctuations are seen to generate and propagate along the s… view at source ↗
Figure 7
Figure 7. Figure 7: Temporal evolution of the wave energy flux (WEF) for the Alfv´en wave packet at the different positions on the slit S3 (see [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Top left panel is v/cA map of the fast magnetoacoustic perturbation at t = 5 s and dotted red line represents a curved slit chosen from bottom to top through the null region. The FOV of the zoomed region of the numerical domain is, x = [−20 Mm, 60 Mm], y = [0 Mm, 80 Mm], respectively, and the black circular contour represent the β = 1 layer. Top right panel is the spatial variation of the normalized Alfv´e… view at source ↗
read the original abstract

In the present paper, we have performed 2.5D resistive magnetohydrodynamic simulations of the interaction of a fast magnetoacoustic wave with a localized coronal magnetic null point. As a result, an Alfv\'en wave packet is generated by the mode conversion when a fast magnetoacoustic perturbation interacts with the null point. The field-aligned plasma flows are also generated due to the non-linear effects. When the fast mode wavefront interacts with the null, some parts of this wavefront get refracted around it, while some other part is trapped at the null region. Subsequently, the velocity fluctuation out of the plane and in-phase magnetic field fluctuations have evolved and propagated with the local Alfv\'en speed along the separatrixes at one side of the coronal null region. The resulting disturbance behaves as an incompressible and energetic Alfv\'en wave packet. A secondary fast magnetoacoustic wave is also produced and propagates. In the synthetic SDO/AIA observations, no intensity fluctuations are evident in the region where the Alfv\'en wave packet propagates, while the fast magnetoacoustic wave fronts are clearly evident. Our results suggest that given the appropriate physical conditions at the null, when the fast mode wave is incident, Alfv\'en packets can be excited due to the mode conversion, further carrying substantial momentum and energy flux in the solar corona.

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

3 major / 2 minor

Summary. The paper claims that 2.5D resistive MHD simulations of a fast magnetoacoustic wave interacting with a localized coronal magnetic null point show mode conversion generating an incompressible energetic Alfvén wave packet (identified via out-of-plane velocity and in-phase magnetic fluctuations propagating at local v_A along separatrices), plus nonlinear field-aligned plasma flows and a secondary fast wave; synthetic SDO/AIA images exhibit no intensity fluctuations where the Alfvén packet propagates.

Significance. If the results hold, the work identifies a concrete mechanism for Alfvén-wave generation and energy/momentum transport in the corona via null-point mode conversion, with the synthetic AIA prediction offering a falsifiable observational test. The direct numerical integration of the MHD equations (low circularity) is a strength, but the absence of reported resolution or convergence data limits immediate impact.

major comments (3)
  1. [Methods] Methods section: no grid resolution, resistivity value, time-step criterion, or convergence tests are supplied. This is load-bearing for the central claim that the generated disturbance is a robust, incompressible Alfvén packet, because the mode-conversion outcome and its propagation depend on numerical dissipation and the chosen resistive MHD setup.
  2. [Results/Discussion] Results and Discussion: the entire analysis is performed in 2.5D. The spine-fan topology and additional separatrix surfaces present in 3D can alter current-sheet formation and out-of-plane coupling; the paper provides no test or argument showing that the reported incompressibility, energy flux, or conversion efficiency survive the extra degree of freedom.
  3. [Results] Results: no comparison is made to linear MHD theory or analytic expectations for fast-to-Alfvén conversion at a null. Without this benchmark, it is difficult to separate physical mode conversion from numerical or initial-condition artifacts.
minor comments (2)
  1. [Abstract] Abstract and text: the initial wave amplitude, null field strength, and resistivity are free parameters; their specific values and sensitivity should be stated explicitly.
  2. [Figures] Figure captions and text: clarify how the synthetic AIA intensity is computed (e.g., which emission lines or temperature response) to allow direct comparison with observations.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below and have revised the manuscript to incorporate additional methodological details and discussion where feasible.

read point-by-point responses

  1. Referee: [Methods] Methods section: no grid resolution, resistivity value, time-step criterion, or convergence tests are supplied. This is load-bearing for the central claim that the generated disturbance is a robust, incompressible Alfvén packet, because the mode-conversion outcome and its propagation depend on numerical dissipation and the chosen resistive MHD setup.

    Authors: We agree these parameters are necessary for reproducibility and to demonstrate robustness. In the revised manuscript we will add the grid resolution employed, the resistivity value used, the CFL-based time-step criterion, and results of convergence tests performed at multiple resolutions showing that the properties of the generated Alfvén packet (propagation speed, incompressibility, and energy flux) remain consistent. revision: yes

  2. Referee: [Results/Discussion] Results and Discussion: the entire analysis is performed in 2.5D. The spine-fan topology and additional separatrix surfaces present in 3D can alter current-sheet formation and out-of-plane coupling; the paper provides no test or argument showing that the reported incompressibility, energy flux, or conversion efficiency survive the extra degree of freedom.

    Authors: We acknowledge that full 3D topology introduces additional separatrix surfaces that could modify current-sheet dynamics. Our 2.5D configuration isolates the essential fast-to-Alfvén conversion process along the fan separatrices that are directly relevant to the out-of-plane Alfvénic perturbation. We will add a dedicated paragraph in the Discussion section explicitly noting this limitation, arguing that the local mode-conversion physics at the null is expected to persist, and stating that a 3D extension is reserved for future work. revision: partial

  3. Referee: [Results] Results: no comparison is made to linear MHD theory or analytic expectations for fast-to-Alfvén conversion at a null. Without this benchmark, it is difficult to separate physical mode conversion from numerical or initial-condition artifacts.

    Authors: We will expand the Results section to include an explicit comparison of the simulated disturbance properties (propagation at the local Alfvén speed, transverse polarization, absence of density fluctuations confirming incompressibility) against standard linear MHD expectations for Alfvén waves. While an exact analytic solution for the nonlinear interaction at a null point is not available in the literature, this benchmark will help distinguish the physical mode conversion from possible artifacts. revision: yes

Circularity Check

0 steps flagged

No circularity: results from direct numerical integration of MHD equations

full rationale

The paper reports outcomes of 2.5D resistive MHD simulations of wave-null interaction. No analytical derivation chain exists that could reduce predictions to fitted inputs, self-definitions, or self-citation load-bearing steps. Identification of the Alfvén packet follows from the evolved fields and velocities in the simulation output, not from any redefinition or renaming of inputs. Self-citations, if present, are not required to close the central claim.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The claim rests on the validity of the resistive MHD equations in 2.5D for this geometry and on the numerical realization of mode conversion at the chosen null strength and wave amplitude; no independent analytic benchmark is cited in the abstract.

free parameters (3)
  • initial wave amplitude
    Perturbation strength chosen to drive the interaction
  • magnetic resistivity
    Value enabling resistive effects at the null
  • null field strength
    Background field configuration defining the null
axioms (2)
  • domain assumption Ideal and resistive MHD equations govern the plasma dynamics near the coronal null
    Standard assumption invoked for all such simulations
  • domain assumption 2.5D geometry with translational invariance is adequate to capture the essential mode conversion
    Modeling choice stated in the abstract

pith-pipeline@v0.9.1-grok · 5817 in / 1287 out tokens · 27449 ms · 2026-06-27T23:37:46.828794+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

86 extracted references · 81 canonical work pages

  1. [1]

    2015, Philosophical Transactions of the Royal Society of London Series A, 373, 20140261, doi: 10.1098/rsta.2014.0261

    Arregui, I. 2015, Philosophical Transactions of the Royal Society of London Series A, 373, 20140261, doi: 10.1098/rsta.2014.0261

    work page doi:10.1098/rsta.2014.0261 2015

  2. [2]

    Banerjee, D., P´ erez-Su´ arez, D., & Doyle, J. G. 2009, A&A, 501, L15, doi: 10.1051/0004-6361/200912242

    work page doi:10.1051/0004-6361/200912242 2009

  3. [3]

    S., & Priest, E

    Brown, D. S., & Priest, E. R. 2001, A&A, 367, 339, doi: 10.1051/0004-6361:20010016

    work page doi:10.1051/0004-6361:20010016 2001

  4. [4]

    Cally, P. S. 2011, in Astronomical Society of India Conference Series, Vol. 2, Astronomical Society of India Conference Series, 221–227

    2011

  5. [5]

    S., & Goossens, M

    Cally, P. S., & Goossens, M. 2008, SoPh, 251, 251, doi: 10.1007/s11207-007-9086-3

    work page doi:10.1007/s11207-007-9086-3 2008

  6. [6]

    2016, ApJ, 822, 106, doi: 10.3847/0004-637X/822/2/106

    Uddin, W. 2016, ApJ, 822, 106, doi: 10.3847/0004-637X/822/2/106

    work page doi:10.3847/0004-637x/822/2/106 2016

  7. [7]

    F., Fang, C., Chandra, R., & Srivastava, A

    Chen, P. F., Fang, C., Chandra, R., & Srivastava, A. K. 2016, SoPh, 291, 3195, doi: 10.1007/s11207-016-0920-3

    work page doi:10.1007/s11207-016-0920-3 2016

  8. [8]

    Srivastava, A. K. 2014, ApJ, 793, 43, doi: 10.1088/0004-637X/793/1/43

    work page doi:10.1088/0004-637x/793/1/43 2014

  9. [9]

    M., Parnell, C

    Close, R. M., Parnell, C. E., & Priest, E. R. 2004, SoPh, 225, 21, doi: 10.1007/s11207-004-3259-0 De Moortel, I., Ireland, J., Hood, A. W., & Walsh, R. W. 2002a, A&A, 387, L13, doi: 10.1051/0004-6361:20020436 De Moortel, I., Ireland, J., Walsh, R. W., & Hood, A. W. 2002b, SoPh, 209, 61, doi: 10.1023/A:1020956421063 De Pontieu, B., McIntosh, S. W., Carlsso...

    work page doi:10.1007/s11207-004-3259-0 2004

  10. [10]

    P., Landi, E., Young, P

    Dere, K. P., Landi, E., Young, P. R., et al. 2009, A&A, 498, 915, doi: 10.1051/0004-6361/200911712

    work page doi:10.1051/0004-6361/200911712 2009

  11. [11]

    P., Keppens, R., & Poedts, S

    Goedbloed, J. P., Keppens, R., & Poedts, S. 2010, Advanced Magnetohydrodynamics

    2010

  12. [12]

    2001, Physics of Plasmas, 8, 2371, doi: 10.1063/1.1343090

    Goossens, M., & De Groof, A. 2001, Physics of Plasmas, 8, 2371, doi: 10.1063/1.1343090

    work page doi:10.1063/1.1343090 2001

  13. [13]

    Goossens, M., Erd´ elyi, R., & Ruderman, M. S. 2011, SSRv, 158, 289, doi: 10.1007/s11214-010-9702-7

    work page doi:10.1007/s11214-010-9702-7 2011

  14. [14]

    K., & Ofman, L

    Gruszecki, M., Murawski, K., Solanki, S. K., & Ofman, L. 2007, A&A, 469, 1117, doi: 10.1051/0004-6361:20066924

    work page doi:10.1051/0004-6361:20066924 2007

  15. [15]

    C., & Cally, P

    Hansen, S. C., & Cally, P. S. 2012, ApJ, 751, 31, doi: 10.1088/0004-637X/751/1/31

    work page doi:10.1088/0004-637x/751/1/31 2012

  16. [16]

    M., & Melosh , H

    Harten, A. 1997, Journal of Computational Physics, 135, 260, doi: 10.1006/jcph.1997.5713

    work page doi:10.1006/jcph.1997.5713 1997

  17. [17]

    Heyvaerts, J., & Priest, E. R. 1983, A&A, 117, 220

    1983

  18. [18]

    Hollweg, J. V. 1978, SoPh, 56, 305, doi: 10.1007/BF00152474

    work page doi:10.1007/bf00152474 1978

  19. [19]

    Ionson, J. A. 1978, ApJ, 226, 650, doi: 10.1086/156648

    work page doi:10.1086/156648 1978

  20. [20]

    Ireland, J., & Priest, E. R. 1997, SoPh, 173, 31, doi: 10.1023/A:1004903128146

    work page doi:10.1023/a:1004903128146 1997

  21. [21]

    B., Keys, P

    Jess, D. B., Jafarzadeh, S., Keys, P. H., et al. 2023, Living Reviews in Solar Physics, 20, 1, doi: 10.1007/s41116-022-00035-6

    work page doi:10.1007/s41116-022-00035-6 2023

  22. [22]

    J., et al

    Keppens, R., Meliani, Z., van Marle, A. J., et al. 2012, Journal of Computational Physics, 231, 718, doi: 10.1016/j.jcp.2011.01.020

    work page doi:10.1016/j.jcp.2011.01.020 2012

  23. [23]

    2023, A&A, 673, A66, doi: 10.1051/0004-6361/202245359

    Keppens, R., Popescu Braileanu, B., Zhou, Y., et al. 2023, A&A, 673, A66, doi: 10.1051/0004-6361/202245359

    work page doi:10.1051/0004-6361/202245359 2023

  24. [24]

    V., & Khutsishvili, E

    Kukhianidze, V., Zaqarashvili, T. V., & Khutsishvili, E. 2006, A&A, 449, L35, doi: 10.1051/0004-6361:200600018

    work page doi:10.1051/0004-6361:200600018 2006

  25. [25]

    M., Karpen, J

    Kumar, P., Nakariakov, V. M., Karpen, J. T., & Cho, K.-S. 2024, Nature Communications, 15, 2667, doi: 10.1038/s41467-024-46736-4

    work page doi:10.1038/s41467-024-46736-4 2024

  26. [26]

    2013, ApJ, 766, 55, doi: 10.1088/0004-637X/766/1/55

    Kwon, R.-Y., Ofman, L., Olmedo, O., et al. 2013, ApJ, 766, 55, doi: 10.1088/0004-637X/766/1/55

    work page doi:10.1088/0004-637x/766/1/55 2013

  27. [27]

    2014, ApJ, 794, 148, doi: 10.1088/0004-637X/794/2/148

    Kwon, R.-Y., Zhang, J., & Olmedo, O. 2014, ApJ, 794, 148, doi: 10.1088/0004-637X/794/2/148

    work page doi:10.1088/0004-637x/794/2/148 2014

  28. [28]

    2015, ApJL, 799, L29, doi: 10.1088/2041-8205/799/2/L29

    Kwon, R.-Y., Zhang, J., & Vourlidas, A. 2015, ApJL, 799, L29, doi: 10.1088/2041-8205/799/2/L29

    work page doi:10.1088/2041-8205/799/2/l29 2015

  29. [29]

    2025, A&A, 696, A158, doi: 10.1051/0004-6361/202453300

    Liakh, V., & Keppens, R. 2025, A&A, 696, A158, doi: 10.1051/0004-6361/202453300

    work page doi:10.1051/0004-6361/202453300 2025

  30. [30]

    M., Bloomfield, D

    Long, D. M., Bloomfield, D. S., Chen, P. F., et al. 2017, SoPh, 292, 7, doi: 10.1007/s11207-016-1030-y

    work page doi:10.1007/s11207-016-1030-y 2017

  31. [31]

    2017, Scientific Reports, 7, 14820, doi: 10.1038/s41598-017-13660-1

    Magyar, N., Van Doorsselaere, T., & Goossens, M. 2017, Scientific Reports, 7, 14820, doi: 10.1038/s41598-017-13660-1

    work page doi:10.1038/s41598-017-13660-1 2017

  32. [32]

    2019, ApJ, 882, 50, doi: 10.3847/1538-4357/ab357c

    Magyar, N., Van Doorsselaere, T., & Goossens, M. 2019, ApJ, 882, 50, doi: 10.3847/1538-4357/ab357c

    work page doi:10.3847/1538-4357/ab357c 2019

  33. [33]

    2023, A&A, 675, A129, doi: 10.1051/0004-6361/202346378

    Mann, G., Warmuth, A., & ¨Onel, H. 2023, A&A, 675, A129, doi: 10.1051/0004-6361/202346378

    work page doi:10.1051/0004-6361/202346378 2023

  34. [34]

    A., Ferguson, J

    McLaughlin, J. A., Ferguson, J. S. L., & Hood, A. W. 2008, SoPh, 251, 563, doi: 10.1007/s11207-007-9107-2

    work page doi:10.1007/s11207-007-9107-2 2008

  35. [35]

    A., & Hood, A

    McLaughlin, J. A., & Hood, A. W. 2004, A&A, 420, 1129, doi: 10.1051/0004-6361:20035900

    work page doi:10.1051/0004-6361:20035900 2004

  36. [36]

    A., & Hood, A

    McLaughlin, J. A., & Hood, A. W. 2005, A&A, 435, 313, doi: 10.1051/0004-6361:20042361

    work page doi:10.1051/0004-6361:20042361 2005

  37. [37]

    A., & Hood, A

    McLaughlin, J. A., & Hood, A. W. 2006, A&A, 452, 603, doi: 10.1051/0004-6361:20054575

    work page doi:10.1051/0004-6361:20054575 2006

  38. [38]

    A., Hood, A

    McLaughlin, J. A., Hood, A. W., & De Moortel, I. 2010, Space Science Reviews, 158, 205–236, doi: 10.1007/s11214-010-9654-y

    work page doi:10.1007/s11214-010-9654-y 2010

  39. [39]

    Mondal, S., Bairagi, A., & Srivastava, A. K. 2025a, ApJ, 979, 207, doi: 10.3847/1538-4357/ada1d6

    work page doi:10.3847/1538-4357/ada1d6

  40. [40]

    Mondal, S., Srivastava, A., Bairagi, A., Martinez Sykora, J., & De Pontieu, B. e. a. 2026, ApJL, 000, 00, doi: inpreparation

    2026

  41. [41]

    K., Pontin, D

    Mondal, S., Srivastava, A. K., Pontin, D. I., & Priest, E. R. 2025b, ApJ, 989, 222, doi: 10.3847/1538-4357/adf18e

    work page doi:10.3847/1538-4357/adf18e

  42. [42]

    Priest, E. R. 2024, ApJ, 963, 139, doi: 10.3847/1538-4357/ad2079

    work page doi:10.3847/1538-4357/ad2079 2024

  43. [43]

    E., & Ramsey, H

    Moreton, G. E., & Ramsey, H. E. 1960, PASP, 72, 357, doi: 10.1086/127549

    work page doi:10.1086/127549 1960

  44. [44]

    1997, SoPh, 175, 571, doi: 10.1023/A:1004902913117

    Moses, D., Clette, F., Delaboudini` ere, J.-P., et al. 1997, SoPh, 175, 571, doi: 10.1023/A:1004902913117

    work page doi:10.1023/a:1004902913117 1997

  45. [45]

    M., Kienreich, I

    Muhr, N., Veronig, A. M., Kienreich, I. W., et al. 2014, SoPh, 289, 4563, doi: 10.1007/s11207-014-0594-7

    work page doi:10.1007/s11207-014-0594-7 2014

  46. [46]

    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

  47. [47]

    M., Roberts, B., & Murawski, K

    Nakariakov, V. M., Roberts, B., & Murawski, K. 1997, SoPh, 175, 93, doi: 10.1023/A:1004965725929

    work page doi:10.1023/a:1004965725929 1997

  48. [48]

    M., & Verwichte, E

    Nakariakov, V. M., & Verwichte, E. 2005, Living Reviews in Solar Physics, 2, 3, doi: 10.12942/lrsp-2005-3

    work page doi:10.12942/lrsp-2005-3 2005

  49. [49]

    V., Schrijver, C

    Nitta, N. V., Schrijver, C. J., Title, A. M., & Liu, W. 2013, ApJ, 776, 58, doi: 10.1088/0004-637X/776/1/58

    work page doi:10.1088/0004-637x/776/1/58 2013

  50. [50]

    2009, SSRv, 149, 153, doi: 10.1007/s11214-009-9501-1

    Ofman, L. 2009, SSRv, 149, 153, doi: 10.1007/s11214-009-9501-1

    work page doi:10.1007/s11214-009-9501-1 2009

  51. [51]

    Ofman, L., & Davila, J. M. 1995, J. Geophys. Res., 100, 23413, doi: 10.1029/95JA02222

    work page doi:10.1029/95ja02222 1995

  52. [52]

    2018, ApJ, 860, 54, doi: 10.3847/1538-4357/aac2e8

    Ofman, L., & Liu, W. 2018, ApJ, 860, 54, doi: 10.3847/1538-4357/aac2e8

    work page doi:10.3847/1538-4357/aac2e8 2018

  53. [53]

    J., Tsuneta, S., Berger, T

    Okamoto, T. J., Tsuneta, S., Berger, T. E., et al. 2007, Science, 318, 1577, doi: 10.1126/science.1145447

    work page doi:10.1126/science.1145447 2007

  54. [54]

    I., Priest, E

    Pontin, D. I., Priest, E. R., & Galsgaard, K. 2013, ApJ, 774, 154, doi: 10.1088/0004-637X/774/2/154 19

    work page doi:10.1088/0004-637x/774/2/154 2013

  55. [55]

    J., Klimchuk, J

    Porter, L. J., Klimchuk, J. A., & Sturrock, P. A. 1994, ApJ, 435, 482, doi: 10.1086/174830

    work page doi:10.1086/174830 1994

  56. [56]

    P., & Keppens, R

    Porth, O., Xia, C., Hendrix, T., Moschou, S. P., & Keppens, R. 2014, ApJS, 214, 4, doi: 10.1088/0067-0049/214/1/4

    work page doi:10.1088/0067-0049/214/1/4 2014

  57. [57]

    2022, ApJ, 924, 126, doi: 10.3847/1538-4357/ac3b5f

    Sabri, S., Ebadi, H., & Poedts, S. 2022, ApJ, 924, 126, doi: 10.3847/1538-4357/ac3b5f

    work page doi:10.3847/1538-4357/ac3b5f 2022

  58. [58]

    2017, A&A, 602, A43, doi: 10.1051/0004-6361/201629729

    Vicente, A. 2017, A&A, 602, A43, doi: 10.1051/0004-6361/201629729

    work page doi:10.1051/0004-6361/201629729 2017

  59. [59]

    2022, A&A, 666, A28, doi: 10.1051/0004-6361/202244152

    Sen, S., & Keppens, R. 2022, A&A, 666, A28, doi: 10.1051/0004-6361/202244152

    work page doi:10.1051/0004-6361/202244152 2022

  60. [60]

    2012, ApJL, 752, L23, doi: 10.1088/2041-8205/752/2/L23

    Shen, Y., & Liu, Y. 2012, ApJL, 752, L23, doi: 10.1088/2041-8205/752/2/L23

    work page doi:10.1088/2041-8205/752/2/l23 2012

  61. [61]

    K., Lagg, A., Woch, J., Krupp, N., & Collados, M

    Solanki, S. K., Lagg, A., Woch, J., Krupp, N., & Collados, M. 2003, Nature, 425, 692, doi: 10.1038/nature02035

    work page doi:10.1038/nature02035 2003

  62. [62]

    1962, Physics of Fully Ionized Gases

    Spitzer, L. 1962, Physics of Fully Ionized Gases

    1962

  63. [63]

    K., Shetye, J., Murawski, K., et al

    Srivastava, A. K., Shetye, J., Murawski, K., et al. 2017, Scientific Reports, 7, 43147, doi: 10.1038/srep43147

    work page doi:10.1038/srep43147 2017

  64. [64]

    K., Ballester, J

    Srivastava, A. K., Ballester, J. L., Cally, P. S., et al. 2021, Journal of Geophysical Research (Space Physics), 126, e029097, doi: 10.1029/2020JA029097

    work page doi:10.1029/2020ja029097 2021

  65. [65]

    The Astrophysical Journal , keywords =

    Srivastava, A. K., Mondal, S., Priest, E. R., et al. 2025, ApJ, 984, 36, doi: 10.3847/1538-4357/adc379

    work page doi:10.3847/1538-4357/adc379 2025

  66. [66]

    Syntelis, P., & Priest, E. R. 2020, ApJ, 891, 52, doi: 10.3847/1538-4357/ab6ffc

    work page doi:10.3847/1538-4357/ab6ffc 2020

  67. [67]

    A., Linton, M., & Leake, J

    Tarr, L. A., Linton, M., & Leake, J. 2017, ApJ, 837, 94, doi: 10.3847/1538-4357/aa5e4e

    work page doi:10.3847/1538-4357/aa5e4e 2017

  68. [68]

    J., Plunkett, S

    Thompson, B. J., Plunkett, S. P., Gurman, J. B., et al. 1998, Geophys. Res. Lett., 25, 2465, doi: 10.1029/98GL50429

    work page doi:10.1029/98gl50429 1998

  69. [69]

    O., & McLaughlin, J

    Thurgood, J. O., & McLaughlin, J. A. 2013, A&A, 555, A86, doi: 10.1051/0004-6361/201321338

    work page doi:10.1051/0004-6361/201321338 2013

  70. [70]

    1968, SoPh, 4, 30, doi: 10.1007/BF00146996

    Uchida, Y. 1968, SoPh, 4, 30, doi: 10.1007/BF00146996

    work page doi:10.1007/bf00146996 1968

  71. [71]

    M., Muhr, N., Kienreich, I

    Veronig, A. M., Muhr, N., Kienreich, I. W., Temmer, M., & Vrˇ snak, B. 2010, ApJL, 716, L57, doi: 10.1088/2041-8205/716/1/L57

    work page doi:10.1088/2041-8205/716/1/l57 2010

  72. [72]

    2004, ApJL, 605, L149, doi: 10.1086/420927

    Voitenko, Y., & Goossens, M. 2004, ApJL, 605, L149, doi: 10.1086/420927

    work page doi:10.1086/420927 2004

  73. [73]

    2026, arXiv e-prints, arXiv:2603.13456, doi: 10.48550/arXiv.2603.13456

    Wang, T., Liu, W., Ofman, L., Sun, X., & Jin, M. 2026, arXiv e-prints, arXiv:2603.13456, doi: 10.48550/arXiv.2603.13456

    work page doi:10.48550/arxiv.2603.13456 2026

  74. [74]

    2015, Living Reviews in Solar Physics, 12, 3, doi: 10.1007/lrsp-2015-3

    Warmuth, A. 2015, Living Reviews in Solar Physics, 12, 3, doi: 10.1007/lrsp-2015-3

    work page doi:10.1007/lrsp-2015-3 2015

  75. [75]

    2011, A&A, 532, A151, doi: 10.1051/0004-6361/201116685

    Warmuth, A., & Mann, G. 2011, A&A, 532, A151, doi: 10.1051/0004-6361/201116685

    work page doi:10.1051/0004-6361/201116685 2011

  76. [76]

    Wentzel, D. G. 1974, SoPh, 39, 129, doi: 10.1007/BF00154975

    work page doi:10.1007/bf00154975 1974

  77. [77]

    L., & Noyes, R

    Withbroe, G. L., & Noyes, R. W. 1977, ARA&A, 15, 363, doi: 10.1146/annurev.aa.15.090177.002051

    work page doi:10.1146/annurev.aa.15.090177.002051 1977

  78. [78]

    Wright, A. N. 1991, Geophys. Res. Lett., 18, 1951, doi: 10.1029/91GL02630

    work page doi:10.1029/91gl02630 1991

  79. [79]

    2018, ApJS, 234, 30, doi: 10.3847/1538-4365/aaa6c8

    Xia, C., Teunissen, J., El Mellah, I., Chan´ e, E., & Keppens, R. 2018, ApJS, 234, 30, doi: 10.3847/1538-4365/aaa6c8

    work page doi:10.3847/1538-4365/aaa6c8 2018

  80. [80]

    2022, A&A, 660, A21, doi: 10.1051/0004-6361/202142688

    Yadav, N., Keppens, R., & Popescu Braileanu, B. 2022, A&A, 660, A21, doi: 10.1051/0004-6361/202142688

    work page doi:10.1051/0004-6361/202142688 2022

Showing first 80 references.