pith. sign in

arxiv: 2606.19335 · v1 · pith:ZTADVH3Unew · submitted 2026-06-17 · 🌌 astro-ph.SR

Fine-scale downflows above flare ribbons captured by Solar Orbiter/EUI

Zheng Sun , Alexander G.M. Pietrow , Malcolm K. Druett , Hui Tian , Juli\'an D. Alvarado-G\'omez , Song Tan , Alexander Warmuth , Jiasheng Wang
show 3 more authors
Yuhang Gao Zhenyong Hou Alexandros Stork
This is my paper

Pith reviewed 2026-06-26 19:15 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar flaresflare ribbonsEUV downflowsribletsdownflowsSolar Orbitermagnetic reconnectionenergy deposition
0
0 comments X

The pith

EUV observations from Solar Orbiter capture fine-scale downflows above flare ribbons matching chromospheric riblets at 10^6 K

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

The paper reports detection of small downward-moving bright thread-like structures in high-resolution EUV images of solar flares taken by Solar Orbiter/EUI. These features show velocities around 100 km/s, lifetimes near 15 seconds, and lengths of about 1.6 Mm, appearing directly above flare ribbons. The authors match these properties to earlier chromospheric riblets seen in H-alpha and H-beta and conclude the EUV versions are the same structures viewed at higher temperatures. If the identification holds, the structures supply a new means to track how reconnection energy moves and deposits in the flare atmosphere. The paper proposes the downflows arise either from particle beams compressing pre-existing fibrils or from compression driven by plasma falling from the corona.

Core claim

High-resolution EUV observations reveal downward-propagating bright thread-like structures above flare ribbons with velocities of approximately 100 km s^{-1}, lifetimes of approximately 15 s, and lengths of approximately 1.6 Mm. Based on their morphological and dynamical properties, these are interpreted as the EUV counterparts of chromospheric riblets, representing downflows at temperatures around 10^6 K that result from energisation and compression of pre-existing chromospheric fibrils due to particle beams or from adiabatic or shock-driven compression induced by downward-propagating plasma from the corona.

What carries the argument

Morphological and dynamical property matching (velocity, lifetime, length, and location above ribbons) used to identify the EUV thread-like downflows as riblet counterparts

If this is right

  • The downflows arise from particle beam energisation and compression of fibrils or from adiabatic or shock-driven compression by downward plasma.
  • EUV riblets provide a diagnostic tool for the dynamics of magnetic reconnection during solar flares.
  • These features enable study of energy transport and deposition in flares at temperatures around 10^6 K.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Coordinated multi-wavelength campaigns could test whether the temperature and density profiles align across the proposed riblet layers.
  • Flare reconnection models could be examined for whether they naturally produce fine-scale downflows with these speeds and sizes at both chromospheric and transition-region heights.
  • If the structures are general, similar riblet signatures might appear in other wavelength bands or even in stellar flare observations with sufficient resolution.

Load-bearing premise

Similarities in velocity, lifetime, length, and location above ribbons suffice to identify the EUV structures as the same physical objects as the chromospheric riblets, without spectroscopic or multi-temperature confirmation.

What would settle it

Simultaneous chromospheric and EUV observations of the same flare ribbon showing mismatched velocities, lifetimes, or spatial scales between the two sets of downflows would undermine the counterpart identification.

Figures

Figures reproduced from arXiv: 2606.19335 by Alexander G.M. Pietrow, Alexander Warmuth, Alexandros Stork, Hui Tian, Jiasheng Wang, Juli\'an D. Alvarado-G\'omez, Malcolm K. Druett, Song Tan, Yuhang Gao, Zheng Sun, Zhenyong Hou.

Figure 1
Figure 1. Figure 1: Overview of the positions (a) and viewing geometry from Solar Orbiter (b), and SDO (c). The cyan square denotes the field of view (FoV) of HRIEUV. Since the HRIEUV FoV partially lies outside the solar disk, we define a smaller on-disk region (green square) within the FoV and re-project this region onto the SDO perspective. 2012; Zhao et al. 2016; Janvier 2017; Sun et al. 2025). Ob￾servations of emission fr… view at source ↗
Figure 2
Figure 2. Figure 2: Overview of the downflows in this event. Panel (a) shows the field of view of the HRIEUV observation. The boxes labeled R1 and R2 mark two different flare-ribbon regions. Panels (b) and (c) present zoomed-in views of regions R1 and R2. Panels (b1–b4) and (c1–c4) display the detailed temporal evolution of two selected individual downflows. The fields of view of these panels are indicated by the black square… view at source ↗
Figure 3
Figure 3. Figure 3: Overview of the same active region as in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Temporal evolution of Region 2 observed by EUI and the SXR and HXR emission of the flare. Panels (a)–(d) show the evolution of Region 2, while panel (e) displays the GOES 1–8 Å SXR light curve together with the STIX 4–10 keV and 25–50 keV HXR light curves. Details of the HXR data processing are described in Tan et al. (2025a). The gray shaded region indicates the EUI observing time span. The vertical dashe… view at source ↗
Figure 5
Figure 5. Figure 5: Histograms of the statistical properties of the downflows iden￾tified in Region 1 and Region 2. The values marked in each panel in￾dicate the corresponding mean values. The starting time in panel (d) corresponds to the first appearance of the downflow. count for the recurrent nature of the downflows. However, these interpretations primarily focus on the association with magnetic reconnection but do not exp… view at source ↗
Figure 6
Figure 6. Figure 6: Cartoon scenarios of the observed downflows. The five-pointed star symbol indicates the magnetic reconnection site. This sketch is adapted from Lysenko et al. (2020). When newly reconnected flare field lines in the current sheet retract and relax, they form coronal loops anchored at their chro￾mospheric footpoints, which correspond to the leading edges of the flare ribbons. This magnetic restructuring sign… view at source ↗
read the original abstract

In solar flares, flare ribbons map chromospheric footpoints where flare energy deposition occurs. These locations are associated with field aligned energy transport from the corona that results from energy liberated during magnetic reconnection. Recent chromospheric observations in the H$\alpha$ and H$\beta$ bands have revealed fine-scale downflow structures above flare ribbons, referred to as riblets. In this study, we identify similar downflow structures in the extreme-ultraviolet (EUV) wavelength using high-resolution observations from Solar Orbiter/EUI. These fine-scale downflows appear as downward-propagating, bright, and thread-like structures. They exhibit typical velocities of $\sim100~\mathrm{km\ s^{-1}}$, lifetimes of $\sim15$~s, and lengths of $\sim1.6$~Mm. Based on their morphological and dynamical properties, we interpret these observed downflows as the EUV counterparts of the riblets that have previously been reported from chromospheric observations. This study presents EUV imaging of $\sim 10^6$~K downflows above flare ribbons. We interpret these downflows as a result of (1) the energisation and subsequent compression of pre-existing chromospheric fibrils due to particle beams or (2) adiabatic or shock-driven compression induced by the downward-propagating plasma from the corona. These fine-scale EUV riblets provide a new diagnostic tool for probing the dynamics of magnetic reconnection as well as energy transport and deposition during solar flares.

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 / 1 minor

Summary. The manuscript reports high-resolution EUV observations from Solar Orbiter/EUI of fine-scale, downward-propagating, thread-like bright structures above flare ribbons. These downflows exhibit typical velocities of ~100 km s^{-1}, lifetimes of ~15 s, and lengths of ~1.6 Mm. The authors interpret the features as the EUV (~10^6 K) counterparts of chromospheric riblets previously seen in Hα/Hβ, and propose formation via beam-driven fibril compression or coronal downflow compression. The work claims these EUV riblets provide a new diagnostic for flare reconnection and energy transport.

Significance. If the identification is substantiated, the result supplies the first reported EUV imaging of ~10^6 K downflows above flare ribbons and extends the riblet phenomenon to coronal temperatures. This would add an observational constraint on the multi-temperature structure of flare energy deposition and reconnection outflows, with potential utility for future multi-instrument campaigns.

major comments (2)
  1. [Abstract] Abstract: The central identification of the EUV downflows as riblet counterparts rests on stated similarities in velocity (~100 km s^{-1}), lifetime (~15 s), length (~1.6 Mm), and location, yet the text supplies no quantitative measurements, error bars, histograms, or explicit data-selection criteria. Without these, the morphological/dynamical match remains unverified and the interpretation is not data-driven.
  2. [Abstract] Abstract: The EUV features are formed at ~10^6 K while riblets are reported from chromospheric lines; no spectroscopic line profiles, emission-measure analysis, or simultaneous multi-temperature imaging is invoked to demonstrate that the same plasma volume or magnetic structure is observed. This leaves the two proposed formation mechanisms observationally indistinguishable.
minor comments (1)
  1. [Abstract] Abstract: The phrase 'fine-scale downflows' is used before the term 'riblets' is introduced; a brief parenthetical definition on first use would improve readability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major comment point by point below, indicating where revisions will be made to strengthen the paper.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central identification of the EUV downflows as riblet counterparts rests on stated similarities in velocity (~100 km s^{-1}), lifetime (~15 s), length (~1.6 Mm), and location, yet the text supplies no quantitative measurements, error bars, histograms, or explicit data-selection criteria. Without these, the morphological/dynamical match remains unverified and the interpretation is not data-driven.

    Authors: We agree that additional quantitative detail is needed to support the identification. The revised manuscript will include histograms of the measured velocities, lifetimes, and lengths with associated uncertainties, along with a clear description of the feature selection criteria and measurement methods. These additions will make the comparison with chromospheric riblets more rigorous and data-driven. revision: yes

  2. Referee: [Abstract] Abstract: The EUV features are formed at ~10^6 K while riblets are reported from chromospheric lines; no spectroscopic line profiles, emission-measure analysis, or simultaneous multi-temperature imaging is invoked to demonstrate that the same plasma volume or magnetic structure is observed. This leaves the two proposed formation mechanisms observationally indistinguishable.

    Authors: The EUI observations are obtained in an EUV passband with formation temperature around 10^6 K, which sets the thermal context. As an imaging instrument, EUI does not provide spectroscopic line profiles or emission-measure diagnostics, and the dataset lacks simultaneous multi-temperature coverage. We will revise the discussion to explicitly note that the two formation mechanisms cannot be distinguished observationally with the available data and to frame this as a limitation. The core result remains the first reported EUV imaging of these downflows and their morphological/dynamical similarity to chromospheric riblets. revision: partial

Circularity Check

0 steps flagged

No circularity: purely observational report with no derivations or self-referential reductions

full rationale

The paper is an observational study that reports EUV downflows with measured properties (velocities ~100 km s^{-1}, lifetimes ~15 s, lengths ~1.6 Mm) and interprets them as counterparts to chromospheric riblets based on morphological and dynamical matches. No equations, parameter fits, predictions, or derivations are present. The central claim does not reduce to any self-citation chain or input by construction; it is a direct comparison of observed features. This is self-contained observational work with no load-bearing circular steps.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard solar-physics assumptions about flare energy transport and on the external prior identification of chromospheric riblets; no free parameters, new entities, or ad-hoc axioms are introduced.

axioms (1)
  • domain assumption Standard model of field-aligned energy transport from coronal reconnection to chromospheric footpoints.
    Invoked when linking the observed EUV downflows to flare energy deposition.

pith-pipeline@v0.9.1-grok · 5840 in / 1152 out tokens · 25627 ms · 2026-06-26T19:15:15.713430+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

98 extracted references

  1. [1]

    C., Alaoui, M., Kowalski, A

    Allred, J. C., Alaoui, M., Kowalski, A. F., & Kerr, G. S. 2020, ApJ, 902, 16

    2020

  2. [2]

    Ashfield, W. H. & Longcope, D. W. 2021, ApJ, 912, 25

    2021

  3. [3]

    2012, A&A, 543, A110

    Aulanier, G., Janvier, M., & Schmieder, B. 2012, A&A, 543, A110

    2012

  4. [4]

    2002, A&A, 384, 273

    Aurass, H., Vršnak, B., & Mann, G. 2002, A&A, 384, 273

    2002

  5. [5]

    2015, ApJ, 813, 113

    Battaglia, M., Kleint, L., Krucker, S., & Graham, D. 2015, ApJ, 813, 113

    2015

  6. [6]

    Benz, A. O. 2017, Living Reviews in Solar Physics, 14, 2

    2017

  7. [7]

    M., et al

    Berghmans, D., Auchère, F., Long, D. M., et al. 2021, A&A, 656, L4

    2021

  8. [8]

    Brosius, J. W. 2012, ApJ, 754, 54

    2012

  9. [9]

    Brown, J. C. 1973, Sol. Phys., 28, 151

    1973

  10. [10]

    K., Patel, R., et al

    Bura, A., Shrivastav, A. K., Patel, R., et al. 2025, ApJ, 988, L65

    2025

  11. [11]

    C., et al

    Cai, Q., Shen, C., Raymond, J. C., et al. 2019, MNRAS, 489, 3183

    2019

  12. [12]

    Canfield, R. C. & Gayley, K. G. 1987, ApJ, 322, 999

    1987

  13. [13]

    1964, in NASA Special Publication, ed

    Carmichael, H. 1964, in NASA Special Publication, ed. W. N. Hess, V ol. 50, 451

    1964

  14. [14]

    2025, A&A, 701, A294

    Chandra, S., Cameron, R., Przybylski, D., et al. 2025, A&A, 701, A294

    2025

  15. [15]

    2026, Earth and Planetary Physics, 10, 438

    Chen, C. 2026, Earth and Planetary Physics, 10, 438

    2026

  16. [16]

    2022, A&A, 659, A107

    Chen, H., Tian, H., Li, L., et al. 2022, A&A, 659, A107

    2022

  17. [17]

    2021, A&A, 656, L7

    Chen, Y ., Przybylski, D., Peter, H., et al. 2021, A&A, 656, L7

    2021

  18. [18]

    P., Pontin, D

    Chitta, L. P., Pontin, D. I., Priest, E. R., et al. 2026, A&A, 705, A113 ¸ Sahin, S. & Antolin, P. 2024, ApJ, 970, 106

    2026

  19. [19]

    T., Antiochos, S

    Dahlin, J. T., Antiochos, S. K., Wyper, P. F., Qiu, J., & DeV ore, C. R. 2025, ApJ, 993, 31 De Pontieu, B., De Moortel, I., Martinez-Sykora, J., & McIntosh, S. W. 2017, ApJ, 845, L18 De Pontieu, B., Hansteen, V . H., Rouppe van der V oort, L., van Noort, M., &

    2025

  20. [20]

    2007, ApJ, 655, 624 De Pontieu, B., Title, A

    Carlsson, M. 2007, ApJ, 655, 624 De Pontieu, B., Title, A. M., Lemen, J. R., et al. 2014, Sol. Phys., 289, 2733 De Wilde, M., Pietrow, A. G. M., Druett, M. K., et al. 2025, A&A, 700, A275

    2007

  21. [21]

    C., Priest, E

    Demoulin, P., Henoux, J. C., Priest, E. R., & Mandrini, C. H. 1996, A&A, 308, 643

    1996

  22. [22]

    2024, A&A, 684, A171

    Druett, M., Ruan, W., & Keppens, R. 2024, A&A, 684, A171

    2024

  23. [23]

    2017, Nature Communications, 8, 15905

    Druett, M., Scullion, E., Zharkova, V ., et al. 2017, Nature Communications, 8, 15905

    2017

  24. [24]

    K., Ruan, W., & Keppens, R

    Druett, M. K., Ruan, W., & Keppens, R. 2023, Sol. Phys., 298, 134

    2023

  25. [25]

    Emslie, A. G. 1978, ApJ, 224, 241

    1978

  26. [26]

    H., Canfield, R

    Fisher, G. H., Canfield, R. C., & McClymont, A. N. 1985, ApJ, 289, 414

    1985

  27. [27]

    R., Hudson, H

    Fletcher, L., Dennis, B. R., Hudson, H. S., et al. 2011, Space Sci. Rev., 159, 19

    2011

  28. [28]

    & Hudson, H

    Fletcher, L. & Hudson, H. S. 2002, Sol. Phys., 210, 307

    2002

  29. [29]

    & Hudson, H

    Fletcher, L. & Hudson, H. S. 2008, ApJ, 675, 1645

    2008

  30. [30]

    Forbes, T. G. & Priest, E. R. 1983, Sol. Phys., 84, 169

    1983

  31. [31]

    J., Kazachenko, M

    French, R. J., Kazachenko, M. D., Berghmans, D., et al. 2025, ApJ, 995, L54

    2025

  32. [32]

    2025, ApJ, 985, L12

    Gao, Y ., Tian, H., Berghmans, D., et al. 2025, ApJ, 985, L12

    2025

  33. [33]

    2006, ApJ, 647, L73

    Carlsson, M. 2006, ApJ, 647, L73

    2006

  34. [34]

    1974, Sol

    Hirayama, T. 1974, Sol. Phys., 34, 323

    1974

  35. [35]

    Hollweg, J. V . 1981, Sol. Phys., 70, 25

    1981

  36. [36]

    D., Aschwanden, M

    Holman, G. D., Aschwanden, M. J., Aurass, H., et al. 2011, Space Sci. Rev., 159, 107

    2011

  37. [37]

    1981, ApJ, 244, L153

    Hoyng, P., Duijveman, A., Boelee, A., et al. 1981, ApJ, 244, L153

    1981

  38. [38]

    Isenberg, P. A. & Forbes, T. G. 2007, ApJ, 670, 1453

    2007

  39. [39]

    2017, Journal of Plasma Physics, 83, 535830101

    Janvier, M. 2017, Journal of Plasma Physics, 83, 535830101

    2017

  40. [40]

    2026, A&A, 706, A369

    Joshi, R., Rouppe van der V oort, L., Aulanier, G., et al. 2026, A&A, 706, A369

    2026

  41. [41]

    Kerr, G. S. 2022, Frontiers in Astronomy and Space Sciences, 9, 1060856

    2022

  42. [42]

    S., Krucker, S., Allred, J

    Kerr, G. S., Krucker, S., Allred, J. C., et al. 2026, Nature Astronomy

    2026

  43. [43]

    Kopp, R. A. & Pneuman, G. W. 1976, Sol. Phys., 50, 85

    1976

  44. [44]

    S., Jeffrey, N

    Krucker, S., Hudson, H. S., Jeffrey, N. L. S., et al. 2011, ApJ, 739, 96

    2011

  45. [45]

    J., Grimm, O., et al

    Krucker, S., Hurford, G. J., Grimm, O., et al. 2020, A&A, 642, A15 Article number, page 7 of 9 A&A proofs:manuscript no. aa

    2020

  46. [46]

    S., et al

    Krucker, S., Saint-Hilaire, P., Hudson, H. S., et al. 2015, ApJ, 802, 19

    2015

  47. [47]

    2020, ApJ, 896, 120

    Kuridze, D., Mathioudakis, M., Heinzel, P., et al. 2020, ApJ, 896, 120

    2020

  48. [48]

    R., Title, A

    Lemen, J. R., Title, A. M., Akin, D. J., et al. 2012, Sol. Phys., 275, 17

    2012

  49. [49]

    2022, ApJ, 926, 23

    Li, D., Hong, Z., & Ning, Z. 2022, ApJ, 926, 23

    2022

  50. [50]

    2024, Science in China E: Technological Sciences, 67, 1592

    Li, D., Hou, Z., Bai, X., et al. 2024, Science in China E: Technological Sciences, 67, 1592

    2024

  51. [51]

    2023, ApJ, 954, 7

    Li, D., Li, C., Qiu, Y ., et al. 2023, ApJ, 954, 7

    2023

  52. [52]

    & Zhang, J

    Li, T. & Zhang, J. 2014, ApJ, 791, L13

    2014

  53. [53]

    & Zhang, J

    Li, T. & Zhang, J. 2015, ApJ, 804, L8

    2015

  54. [54]

    2025, Earth and Planetary Physics, 9, 171

    Li, Y ., Huang, S., Xu, S., et al. 2025, Earth and Planetary Physics, 9, 171

    2025

  55. [55]

    W., Ding, M

    Li, Y ., Qiu, J., Longcope, D. W., Ding, M. D., & Yang, K. 2016, ApJ, 823, L13 Lörinˇcík, J., Polito, V ., De Pontieu, B., Yu, S., & Freij, N. 2022, Frontiers in Astronomy and Space Sciences, 9, 334

    2016

  56. [56]

    L., Frederiks, D

    Lysenko, A. L., Frederiks, D. D., Fleishman, G. D., et al. 2020, Physics-Uspekhi, 63, 818

    2020

  57. [57]

    2009, A&A, 494, 669 Martínez Oliveros, J.-C., Hudson, H

    Mann, G., Warmuth, A., & Aurass, H. 2009, A&A, 494, 669 Martínez Oliveros, J.-C., Hudson, H. S., Hurford, G. J., et al. 2012, ApJ, 753, L26 Martínez Oliveros, J.-C., Krucker, S., Hudson, H. S., et al. 2014, ApJ, 780, L28

    2009

  58. [58]

    Masson, S., Pariat, E., Aulanier, G., & Schrijver, C. J. 2009, ApJ, 700, 559

    2009

  59. [59]

    Milligan, R. O. & Dennis, B. R. 2009, ApJ, 699, 968

    2009

  60. [60]

    D., Thompson, B

    Pesnell, W. D., Thompson, B. J., & Chamberlin, P. C. 2012, Sol. Phys., 275, 3

    2012

  61. [61]

    S., Xu, Y ., Sadykov, V

    Polito, V ., Kerr, G. S., Xu, Y ., Sadykov, V . M., & Lorincik, J. 2023, ApJ, 944, 104

    2023

  62. [62]

    & Forbes, T

    Priest, E. & Forbes, T. 2000, Magnetic Reconnection: MHD Theory and Appli- cations

    2000

  63. [63]

    2024, ApJ, 973, 57

    Qiao, F., Li, L., Tian, H., et al. 2024, ApJ, 973, 57

    2024

  64. [64]

    Reep, J. W. & Russell, A. J. B. 2016, ApJ, 818, L20

    2016

  65. [65]

    Ricchiazzi, P. J. & Canfield, R. C. 1983, ApJ, 272, 739

    1983

  66. [66]

    2020, A&A, 642, A8

    Rochus, P., Auchère, F., Berghmans, D., et al. 2020, A&A, 642, A8

    2020

  67. [67]

    2020, ApJ, 896, 97

    Ruan, W., Xia, C., & Keppens, R. 2020, ApJ, 896, 97

    2020

  68. [68]

    2023, ApJ, 947, 67

    Ruan, W., Yan, L., & Keppens, R. 2023, ApJ, 947, 67

    2023

  69. [69]

    2021, ApJ, 920, L15

    Ruan, W., Zhou, Y ., & Keppens, R. 2021, ApJ, 920, L15

    2021

  70. [70]

    Russell, A. J. B. & Fletcher, L. 2013, ApJ, 765, 81

    2013

  71. [71]

    2019, Science, 366, 890

    Samanta, T., Tian, H., Yurchyshyn, V ., et al. 2019, Science, 366, 890

    2019

  72. [72]

    B., Bjelksjo, K., Korhonen, T

    Scharmer, G. B., Bjelksjo, K., Korhonen, T. K., Lindberg, B., & Petterson, B. 2003, in Proc. SPIE, V ol. 4853, Innovative Telescopes and Instrumentation for Solar Astrophysics, ed. S. L. Keil & S. V . Avakyan, 341–350

    2003

  73. [73]

    2016, ApJ, 833, 184

    Scullion, E., Rouppe van der V oort, L., Antolin, P., et al. 2016, ApJ, 833, 184

    2016

  74. [74]

    Sharykin, I. N. & Kosovichev, A. G. 2014, ApJ, 788, L18

    2014

  75. [75]

    & Tanuma, S

    Shibata, K. & Tanuma, S. 2001, Earth, Planets and Space, 53, 473

    2001

  76. [76]

    Singh, V ., Scullion, E., Botha, G. J. J., et al. 2025, arXiv e-prints, arXiv:2507.01169

    arXiv 2025

  77. [77]

    V ., Syrovatskii, S

    Somov, B. V ., Syrovatskii, S. I., & Spektor, A. R. 1981, Sol. Phys., 73, 145

    1981

  78. [78]

    Sturrock, P. A. 1966, Nature, 211, 695

    1966

  79. [79]

    2025, ApJ, 990, 45

    Sun, Z., Li, T., Bian, X., et al. 2025, ApJ, 990, 45

    2025

  80. [80]

    2023, ApJ, 953, 148

    Sun, Z., Li, T., Tian, H., et al. 2023, ApJ, 953, 148

    2023

Showing first 80 references.