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arxiv: 2606.25469 · v1 · pith:ZM4XDS4Knew · submitted 2026-06-24 · 🌌 astro-ph.SR

Solar Radio Burst Fine Structures

Eduard Kontar , Daniel Clarkson , Hamish Reid , Yingjie Luo , Nicolina Chrysaphi , Alexey Kuznetsov , Galina Motorina , Carine Briand This is my paper

Pith reviewed 2026-06-25 20:21 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar radio burstsfine structuresimaging spectroscopyType III burstsType II burstselectron accelerationmagnetic reconnection
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The pith

Recent sub-second imaging spectroscopy shows fine structures in solar radio bursts that existing models cannot explain.

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

The paper reviews the intricate fine frequency-time structures seen in solar radio bursts, including spikes, drift pairs, striae, and herringbone patterns. Limited resolution previously prevented detailed study of these narrow-band, rapidly evolving features. New sub-second imaging spectroscopy indicates that many of these structures do not fit existing theoretical models of radio emission. A sympathetic reader would care because clarifying their origins would improve understanding of electron acceleration, magnetic reconnection, and plasma turbulence during solar events.

Core claim

Sub-second imaging spectroscopy has revealed that many fine structures in solar radio bursts challenge existing theoretical models, pointing to the need for new frameworks and a reassessment of current interpretations of the emission processes.

What carries the argument

Fine frequency-time structures in solar radio bursts observed via high-resolution imaging spectroscopy, which encode details of small-scale physical conditions in the emitting plasma.

If this is right

  • A clearer picture of how electrons are accelerated and transported in the solar atmosphere.
  • Revised views on the role of magnetic reconnection in generating radio emission.
  • Better characterization of turbulence in the solar corona.
  • More reliable estimates of how solar energetic events affect space weather.

Where Pith is reading between the lines

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

  • The same mismatch between observation and model may occur in radio emission from other astrophysical environments, implying a wider revision of plasma emission theory.
  • Simultaneous multi-wavelength data could test whether the radio fine structures directly trace the sites of particle acceleration.
  • Higher-resolution observations in additional frequency bands could isolate which emission mechanism is most deficient in current models.

Load-bearing premise

The fine frequency-time structures observed in recent sub-second imaging spectroscopy cannot be explained by existing theoretical models of solar radio emission processes.

What would settle it

A single theoretical model that reproduces the full set of observed fine structures while remaining within current frameworks for radio emission processes would falsify the need for new frameworks.

Figures

Figures reproduced from arXiv: 2606.25469 by Alexey Kuznetsov, Carine Briand, Daniel Clarkson, Eduard Kontar, Galina Motorina, Hamish Reid, Nicolina Chrysaphi, Yingjie Luo.

Figure 1
Figure 1. Figure 1: Solar flare with X-ray emission and type III and type II radio emissions. (a) GOES X-ray light curves. (b) LOFAR dynamic spectrum showing a series of bright Type III bursts followed by type II bursts (Chrysaphi et al., 2020) and myriad of fine structures. (c) Dynamic spectrum of the circular polarization from the NDA. The image is adapted from (Clarkson et al., 2021) [PITH_FULL_IMAGE:figures/full_fig_p003… view at source ↗
Figure 2
Figure 2. Figure 2: Zoomed in dynamic spectra. (a) Numerous fine structures are visible in the region bounded by white white box in [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Left: Average spike 1/e decay times against frequency. The solid black line represents the power￾law fit to the data given by 𝜏𝑑 = (11.22 ± 1.9) 𝑓 −1.01±0.03. The dash-dotted gray lines represent the plasma collision time for various coronal temperatures. The gray region shows the typical scattering decay time where the spread accounts for halving and doubling of the scattering rate (see Kontar et al., 202… view at source ↗
Figure 4
Figure 4. Figure 4: Top Left: LOFAR dynamic spectrum of an individual spike. Top Right: LOFAR image of the spike peak flux at 34.5 MHz. The oval in the lower left corner represents the beam size. Lower Left: LOFAR observed centroid positions of hundreds of spikes between 35-40 MHz with time increasing from dark to light. Lower Right: As in the lower left panel but for spikes observed between 30-35 MHz. Lower panels adapted fr… view at source ↗
Figure 5
Figure 5. Figure 5: (a) Dynamic spectrum of solar radio emission with a drift-pair burst recorded with LOFAR on 2017 July 12 (Sun-integrated, in relative units). (b) Time profile of the radio flux at a single frequency (32 MHz). (c) Corresponding time profile of the visible radio source position (distance from the solar disk center). (d) Corresponding time profile of the visible radio source area (at half-maximum level). Red … view at source ↗
Figure 6
Figure 6. Figure 6: Type II solar radio burst exhibiting band splitting and highly-fragmented bands. LOFAR imaging spectroscopy observations allowed for the simultaneous imaging of both subbands at several moments in time, as shown by the red crosses. Figure taken from Chrysaphi et al. (2018) and reproduced by permission of the AAS. such studies. Imaging spectroscopy is particularly beneficial as it allows us to identify the … view at source ↗
Figure 7
Figure 7. Figure 7: Intriguing fine structures observed within the stationary part of a Type II burst that transitions from a stationary to drifting state. The stationary parts of the Type II burst consist of two bands, both of which exhibit band splitting. The white-line annotations highlight fine structures that alternate between negative and positive frequency-drift rates. Figure taken from Chrysaphi et al. (2020) and repr… view at source ↗
Figure 8
Figure 8. Figure 8: Type II solar radio burst exhibiting herringbone structures. Top: Stokes I dynamic spectrum Top: Polarization (Stokes V/I) dynamic spectrum. The spectra are from https://nenufar.obs-nancay.fr. the next-generation SKA-Mid. Building on MeerKAT’s demonstrated capabilities, SKA-Mid will take solar flare diagnostics with radio imaging spectroscopy to a fundamentally new level. With improved solutions for handli… view at source ↗
Figure 9
Figure 9. Figure 9: MeerKAT observations of fine structures in a solar flare by Luo et al. (2026). (A) MeerKAT Stokes I cross-power dynamic spectrum with GOES 1−8 Å soft X-ray flux (red) over-plotted. (B) MeerKAT Stokes V cross-power spectrum. (C) MeerKAT full-disk integrated dynamic spectrum during the burst with STIX light curves overlaid; bad channels and time intervals are flagged. (D) ORFEES (Hamini et al., 2021) dynamic… view at source ↗
Figure 10
Figure 10. Figure 10: Top: Dynamic spectrum of solar radio emission observed by NenuFAR on 2024 July 11 (Sun￾integrated, in relative units). Bottom: Polarization of the same time interval showing reverse of polarization around 11:19:30 UT. The spectra are from https://nenufar.obs-nancay.fr. 2026), whose rapid evolution contains critical information about the transport of energetic electrons and their interaction with the surro… view at source ↗
read the original abstract

Solar radio bursts exhibit intricate variability in time, space, and frequency, often displaying a rich variety of fine frequency-time structures such as spikes, drift pairs, striae in Type III bursts, and herringbone patterns in Type II bursts, etc. Historically, limited spatial, spectral, and temporal resolution has hindered detailed investigation of these narrow-band, rapidly evolving features, restricting progress in identifying their physical origins and underlying processes at these scales. Advances in high-time-frequency-resolution solar imaging now offer transformative opportunities. Recent sub-second imaging spectroscopy has revealed that many fine structures challenge existing theoretical models, pointing to the need for new frameworks and a reassessment of current interpretations. The Square Kilometre Array (SKA), with its full-Stokes imaging spectroscopy at sub-second cadences, will provide unprecedented data essential for resolving these long-standing questions. These capabilities promise to significantly deepen our understanding of electron acceleration and transport, magnetic reconnection, and coronal plasma turbulence, thereby advancing our knowledge of solar energetic processes and improving assessments of their space-weather impacts.

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

1 major / 1 minor

Summary. The manuscript is a review summarizing known fine frequency-time structures in solar radio bursts (spikes, drift pairs, striae in Type III bursts, herringbone patterns in Type II bursts). It notes that historical limits on spatial/spectral/temporal resolution have impeded progress, states that recent sub-second imaging spectroscopy has revealed many such structures to challenge existing theoretical models (necessitating new frameworks), and argues that the Square Kilometre Array (SKA) with full-Stokes sub-second imaging spectroscopy will supply the data needed to resolve open questions on electron acceleration, magnetic reconnection, coronal turbulence, and space-weather impacts.

Significance. If the assessment that recent observations cannot be accommodated by existing models is correct and properly documented, the review would usefully articulate the scientific motivation for SKA solar observations and could help prioritize observing strategies that advance understanding of solar energetic processes.

major comments (1)
  1. [Abstract] Abstract: The central claim that 'recent sub-second imaging spectroscopy has revealed that many fine structures challenge existing theoretical models' is presented without any citations, specific observational examples, error analysis, or identification of the models in question. This assertion is load-bearing for the paper's motivation yet is unsupported in the provided text.
minor comments (1)
  1. [Abstract] Abstract: The phrase 'etc.' at the end of the list of fine structures is informal; replace with a more complete enumeration or a pointer to a comprehensive review.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive comments, which help strengthen the manuscript's motivation and clarity. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that 'recent sub-second imaging spectroscopy has revealed that many fine structures challenge existing theoretical models' is presented without any citations, specific observational examples, error analysis, or identification of the models in question. This assertion is load-bearing for the paper's motivation yet is unsupported in the provided text.

    Authors: We agree the claim in the abstract requires explicit support. In the revised version we will (1) insert 2-3 key citations to recent sub-second imaging spectroscopy results (e.g., LOFAR and MWA studies of spikes and Type-III striae), (2) give one or two concrete observational examples that are difficult to reconcile with standard plasma-emission or beam-instability models, (3) briefly note the relevant observational uncertainties, and (4) identify the models being challenged. These additions will be placed in both the abstract and a short new paragraph in the introduction so the motivation for SKA observations rests on documented evidence rather than assertion. revision: yes

Circularity Check

0 steps flagged

No significant circularity; purely descriptive review

full rationale

This is a forward-looking review summarizing observed fine structures in solar radio bursts and advocating SKA capabilities. The central claim—that recent sub-second imaging spectroscopy reveals structures challenging existing models—is presented as established motivation from external observations rather than derived via equations, fits, or self-citation chains within the paper. No derivations, parameters, or load-bearing logical steps exist that could reduce to inputs by construction; the text contains no equations or quantitative predictions.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only perspective paper; no free parameters, axioms, or invented entities can be extracted as no mathematical or empirical claims with supporting structure are detailed.

pith-pipeline@v0.9.1-grok · 5726 in / 1012 out tokens · 24017 ms · 2026-06-25T20:21:28.412246+00:00 · methodology

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Works this paper leans on

64 extracted references · 59 canonical work pages · 1 internal anchor

  1. [1]

    doi: 10.1007/BF00150141. H. Alvarez and F. T. Haddock. Sol. Phys., 29(1):197–209, Mar

    work page doi:10.1007/bf00150141

  2. [2]

    doi: 10.1007/BF00153449. S. Armatas et al. A&A, 624:A76, Apr

    work page doi:10.1007/bf00153449

  3. [3]

    doi: 10.1051/0004-6361/201834982. M. G. Aubier, Y . Leblanc, and B. Moller-Pedersen. A&A, 70:685, Nov

    work page doi:10.1051/0004-6361/201834982

  4. [4]

    Planck Collaboration et al.Astron

    doi: 10.1051/0004-6361/ 200912143. 16 Solar radio burst fine structures Kontar et al. A. O. Benz. Sol. Phys., 96(2):357–370, Apr

    work page doi:10.1051/0004-6361/

  5. [5]

    doi: 10.1007/BF00149690. A. O. Benz. Living Reviews in Solar Physics, 14(1):2, Dec

    work page doi:10.1007/bf00149690

  6. [6]

    doi: 10.1007/s41116-016-0004-3. A. O. Benz, M. Jaeggi, and P . Zlobec. A&A, 109(2):305–313, May

    work page doi:10.1007/s41116-016-0004-3

  7. [7]

    doi: 10.1051/0004-6361/201527229. R. Braun et al. Anticipated performance of the square kilometre array – phase 1 (ska1),

    work page doi:10.1051/0004-6361/201527229

  8. [8]

    URL https://arxiv.org/abs/1912.12699. A. I. Brazhenko et al. Kinematika i Fizika Nebesnykh Tel Supplement , 5:43–46, June

    arXiv 1912

  9. [9]

    doi: 10.12942/ lrsp-2013-2. I. H. Cairns and R. D. Robinson. Sol. Phys., 111(2):365–383, Sept

    2013

  10. [10]

    doi: 10.3847/1538-4357/ac1acd. A. P . Cerruti et al. Space Weather, 6(10):S10D07, Oct

    work page doi:10.3847/1538-4357/ac1acd

  11. [11]

    doi: 10.1029/2007SW000375. B. Chen et al. Science, 350(6265):1238–1242, Dec

    work page doi:10.1029/2007sw000375

  12. [12]

    doi: 10.1126/science.aac8467. L. Chen et al. ApJ, 915(1):L22, July

    work page doi:10.1126/science.aac8467

  13. [13]

    doi: 10.3847/2041-8213/ac0b43. X. Chen et al. ApJ, 856(1):73, Mar

    work page doi:10.3847/2041-8213/ac0b43 2041

  14. [14]

    doi: 10.3847/1538-4357/aaa9bf. X. Chen et al. ApJ, 905(1):43, Dec

    work page doi:10.3847/1538-4357/aaa9bf

  15. [15]

    doi: 10.3847/1538-4357/abc24e. G. P . Chernov. Fine Structure of Solar Radio Bursts , volume

    work page doi:10.3847/1538-4357/abc24e

  16. [16]

    doi: 10.1007/978-3-642-20015-1. N. Chrysaphi, E. P . Kontar, G. D. Holman, and M. Temmer. ApJ, 868(2):79, Dec

    work page doi:10.1007/978-3-642-20015-1

  17. [17]

    doi: 10.3847/1538-4357/aae9e5. N. Chrysaphi, H. A. S. Reid, and E. P . Kontar. ApJ, 893(2):115, Apr

    work page doi:10.3847/1538-4357/aae9e5

  18. [18]

    doi: 10.3847/1538-4357/ ab80c1. D. L. Clarkson and E. P . Kontar. ApJ, 978(1):73, Jan

    work page doi:10.3847/1538-4357/

  19. [19]

    doi: 10.3847/1538-4357/ad969c. D. L. Clarkson and E. P . Kontar. ApJ, 999(1):134, Mar. 2026a. doi: 10.3847/1538-4357/ae3dae. D. L. Clarkson and E. P . Kontar.arXiv e-prints, art. arXiv:2605.31450, May 2026b. doi: 10.48550/ arXiv.2605.31450. D. L. Clarkson et al. ApJ, 917(2):L32, Aug

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad969c

  20. [20]

    doi: 10.3847/2041-8213/ac1a7d. D. L. Clarkson et al. ApJ, 946(1):33, Mar

    work page doi:10.3847/2041-8213/ac1a7d 2041

  21. [21]

    doi: 10.3847/1538-4357/acbd3f. E. W. Cliver, D. F. Webb, and R. A. Howard. Sol. Phys., 187(1):89–114, June

    work page doi:10.3847/1538-4357/acbd3f

  22. [22]

    doi: 10.1023/A: 1005115119661. E. W. Cliver, S. M. White, and K. S. Balasubramaniam. ApJ, 743(2):145, Dec

    work page doi:10.1023/a:

  23. [23]

    doi: 10.1007/s11214-011-9802-z. B. P . Dąbrowski, P . Rudawy, and M. Karlický. Sol. Phys., 273(2):377–392, Nov

    work page doi:10.1007/s11214-011-9802-z

  24. [24]

    1007/s11207-011-9756-z. V . V . Dorovskyy et al. Sol. Phys., 290(7):2031–2042, July

    2031

  25. [25]

    doi: 10.1007/s11207-015-0725-9. M. Gordovskyy et al. ApJ, 925(2):140, Feb

    work page doi:10.1007/s11207-015-0725-9

  26. [26]

    doi: 10.3847/1538-4357/ac3bb7. M. Guedel and A. O. Benz. A&A, 231(1):202–212, May

    work page doi:10.3847/1538-4357/ac3bb7

  27. [27]

    doi: 10.1051/ swsc/2021039. G. A. Hampson et al. Journal of Astronomical Telescopes, Instruments, and Systems , 8:011018, Jan

    arXiv

  28. [28]

    doi: 10.1117/1.JATIS.8.1.011018. G. D. Holman and M. E. Pesses. ApJ, 267:837–843, Apr

    work page doi:10.1117/1.jatis.8.1.011018

  29. [29]

    doi: 10.1086/160918. G. D. Holman et al. Space Sci. Rev., 159(1-4):107–166, Sept

    work page doi:10.1086/160918

  30. [30]

    doi: 10.22323/1.277.0001. P . M. Kintner, B. O’Hanlon, D. E. Gary, and P . M. S. Kintner.Radio Science, 44(2):RS0A08, June

    work page doi:10.22323/1.277.0001

  31. [31]

    doi: 10.1029/2008RS004039. E. P . Kontar et al. Space Sci. Rev., 159(1-4):301–355, Sept

    work page doi:10.1029/2008rs004039

  32. [32]

    doi: 10.1038/s41467-017-01307-8. E. P . Kontar et al. ApJ, 884(2):122, Oct

    work page doi:10.1038/s41467-017-01307-8

  33. [33]

    doi: 10.3847/1538-4357/ab40bb. E. P . Kontar et al. ApJ, 956(2):112, Oct

    work page doi:10.3847/1538-4357/ab40bb

  34. [34]

    doi: 10.3847/1538-4357/acf6c1. E. P . Kontar, A. G. Emslie, D. L. Clarkson, and A. Pitňa. ApJ, 991(2):L57, Oct

    work page doi:10.3847/1538-4357/acf6c1

  35. [35]

    3847/2041-8213/ae09b0. A. Kontogeorgos et al. Experimental Astronomy , 21(1):41–55, Feb

    2041

  36. [36]

    doi: 10.3847/1538-4357/acdbcc. S. Krucker and A. O. Benz. A&A, 285:1038–1046, May

    work page doi:10.3847/1538-4357/acdbcc

  37. [37]

    doi: 10.3847/2041-8213/add688. A. A. Kuznetsov and E. P . Kontar. A&A, 631:L7, Nov

    work page doi:10.3847/2041-8213/add688 2041

  38. [38]

    doi: 10.1051/0004-6361/201936447. A. A. Kuznetsov, N. Chrysaphi, E. P . Kontar, and G. Motorina. ApJ, 898(2):94, Aug

    work page doi:10.1051/0004-6361/201936447

  39. [39]

    doi: 10.3847/1538-4357/aba04a. J. R. Lemen et al. Sol. Phys., 275(1-2):17–40, Jan

    work page doi:10.3847/1538-4357/aba04a

  40. [40]

    doi: 10.1007/s11207-011-9776-8. Y . Luo et al. ApJ, 911(1):4, Apr

    work page doi:10.1007/s11207-011-9776-8

  41. [41]

    doi: 10.3847/1538-4357/abe5a4. Y . Luo et al. ApJ, 998(2):L46, Feb

    work page doi:10.3847/1538-4357/abe5a4

  42. [42]

    doi: 10.3847/2041-8213/ae42c1. S. Ma et al. Nature Communications, 17(1):5131, June

    work page doi:10.3847/2041-8213/ae42c1 2041

  43. [43]

    doi: 10.1038/s41467-026-74137-2. G. Mann and A. Klassen. A&A, 441(1):319–326, Oct

    work page doi:10.1038/s41467-026-74137-2

  44. [44]

    doi: 10.1051/0004-6361:20034396. G. Mann et al. A&A, 609:A41, Jan

    work page doi:10.1051/0004-6361:20034396

  45. [45]

    doi: 10.1051/0004-6361/201730546. E. Marsch. Reviews in Modern Astronomy , 4:145–156, Jan

    work page doi:10.1051/0004-6361/201730546

  46. [46]

    66380.a4

    doi: 10.1023/B:SOLA.0000036854. 66380.a4. V . N. Melnik et al. In S. K. Chakrabarti, A. I. Zhuk, and G. S. Bisnovatyi-Kogan, editors, American Institute of Physics Conference Series, volume 1206 of American Institute of Physics Conference Series, pages 445–449. AIP, Jan

    work page doi:10.1023/b:sola.0000036854

  47. [47]

    doi: 10.1063/1.3292552. V . N. Melnik et al. Sol. Phys., 289(5):1701–1714, May

    work page doi:10.1063/1.3292552

  48. [48]

    doi: 10.1007/s11207-013-0434-1. V . N. Melnik et al. Sol. Phys., 293(2):26, Feb

    work page doi:10.1007/s11207-013-0434-1

  49. [49]

    doi: 10.1007/s11207-017-1234-9. D. B. Melrose and G. A. Dulk. ApJ, 259:844–858, Aug

    work page doi:10.1007/s11207-017-1234-9

  50. [50]

    18 Solar radio burst fine structures Kontar et al

    doi: 10.1086/160219. 18 Solar radio burst fine structures Kontar et al. V . Mugundhan, K. Hariharan, and R. Ramesh. Sol. Phys., 292(11):155, Nov

    work page doi:10.1086/160219

  51. [51]

    doi: 10.33232/001c.120317. V . Nakariakov et al. In Advancing Astrophysics with the Square Kilometre Array (AASKA14), page 169, Apr

    work page doi:10.33232/001c.120317

  52. [52]

    doi: 10.22323/1.215.0169. A. Nindos, E. P . Kontar, and D. Oberoi.Advances in Space Research, 63(4):1404–1424, Feb

    work page doi:10.22323/1.215.0169

  53. [53]

    doi: 10.1016/j.asr.2018.10.023. M. Pulupa et al. ApJS, 246(2):49, Feb

    work page doi:10.1016/j.asr.2018.10.023 2018

  54. [54]

    doi: 10.3847/1538-4365/ab5dc0. H. A. S. Reid and E. P . Kontar. Nature Astronomy , 5:796–804, May

    work page doi:10.3847/1538-4365/ab5dc0

  55. [55]

    doi: 10.1071/PH580215. J. A. Roberts. Australian Journal of Physics , 12:327, Dec

    work page doi:10.1071/ph580215

  56. [56]

    doi: 10.1071/PH590327. I. N. Sharykin, E. P . Kontar, and A. A. Kuznetsov. Sol. Phys., 293(8):115, Aug

    work page doi:10.1071/ph590327

  57. [57]

    doi: 10.1007/s11207-015-0799-4. S. F. Smerd, K. V . Sheridan, and R. T. Stewart. In G. A. Newkirk, editor, Coronal Disturbances, volume 57 of IAU Symposium, page 389,

    work page doi:10.1007/s11207-015-0799-4

  58. [58]

    doi: 10.1007/BF00159952. R. T. Stewart. Australian Journal of Physics , 19:209, Apr

    work page doi:10.1007/bf00159952

  59. [59]

    doi: 10.1071/PH660209. S. Suzuki and D. E. Gary. PASA, 3(5-6):379–383, Jan

    work page doi:10.1071/ph660209

  60. [60]

    doi: 10.1017/S1323358000026151. T. Takakura and S. Y ousef. Sol. Phys., 40(2):421–438, Feb

    work page doi:10.1017/s1323358000026151

  61. [61]

    doi: 10.1007/BF00162389. G. L. Tarnstrom and K. W. Philip. A&A, 16:21, Jan. 1972a. G. L. Tarnstrom and K. W. Philip. A&A, 17:267, Mar. 1972b. M. P . van Haarlem et al. A&A, 556:A2, Aug

    work page doi:10.1007/bf00162389

  62. [62]

    doi: 10.1051/0004-6361/201220873. S. M. White et al. Space Sci. Rev., 159(1-4):225–261, Sept

    work page doi:10.1051/0004-6361/201220873

  63. [63]

    doi: 10.1071/PH500399. P . Zhang et al. A&A, 639:A115, July

    work page doi:10.1071/ph500399

  64. [64]

    doi: 10.1051/0004-6361/202037733. 19

    work page doi:10.1051/0004-6361/202037733