Pith. sign in

REVIEW 5 major objections 6 minor 81 references

X-ray/Radio Quasi-periodic Pulsations Associated with Plasmoids in Solar Flare Current Sheets

T0 review · 5 major / 6 minor · reviewed 2026-08-11 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Plasmoid ejection and coalescence drive the 10-second and 100-second X-ray and radio pulsations of solar flares.

desk verdict A rich two-flare case study that directly images plasmoids in a flare current sheet alongside double coronal X-ray sources and QPPs; the association is plausible but the strongest conclusion outruns the evidence. read the letter →

arxiv 2412.05193 v2 pith:MW232NLD submitted 2024-12-06 astro-ph.SR astro-ph.HE

Pankaj Kumar , Judith T. Karpen , Joel T. Dahlin This is my paper · ORCID
classification astro-ph.SRastro-ph.HE
keywords solarflaresquasi-periodicpulsationsplasmoidsmagneticreconnectioncurrentsheethardX-raysdecimetricradioburstsfluxropekinkinstability
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper reports that the quasi-periodic X-ray and radio pulsations seen in two successive solar flares on 2015 April 22 were produced by the ejection and coalescence of plasmoids in the flare current sheet beneath an erupting flux rope. Using extreme-ultraviolet images, the authors track bright plasma blobs moving up and down along a current sheet and interpret them as reconnection plasmoids, with speeds between about 80 and 370 kilometres per second. The X-ray and decimetric radio light curves show pulsations with periods of roughly 10 and 100 seconds that are temporally aligned with the blob ejections and mergings. If this association is correct, it means quasi-periodic particle acceleration in flares is directly modulated by plasmoid dynamics, turning a ubiquitous but poorly understood flare signal into a diagnostic of plasmoid-mediated reconnection.

What carries the argument

The central object is the plasmoid, or magnetic island: a distinct blob of plasma and magnetic flux that forms when a stretched current sheet becomes unstable to the tearing mode, and whose ejection and coalescence the paper proposes as the driver of quasi-periodic particle acceleration. The argument is carried by direct EUV imaging of the current sheet, which allows individual plasmoids to be tracked in time–distance plots while X-ray and decimetric radio light curves record the associated pulsations. A supporting mechanism is the MHD model of a kink-unstable flux rope, which predicts the double plasma-sheet structure observed along the rope legs and a central flare current sheet; the paper compares its images to that simulation rather than to a purely theoretical construct.

What would settle it

A direct test would be to observe a flare current sheet with EUV cadence faster than 10 seconds together with X-ray and radio light curves: if the 10-second radio pulsation persists while no plasmoid ejection, merging, or transient X-ray source is seen between the double coronal sources, the proposed association would be contradicted. A second test is to determine, through stereoscopic or forward-model analysis, whether the blobs are genuinely distinct magnetic islands rather than line-of-sight projections of loop structures; if they are projections, the causal link between plasmoids and the pulsations would not be established.

Watch

Extended reading notes

Core claim

The authors observed two confined (failed-eruption) flares from solar active region NOAA 12322 on the west limb on 2015 April 22. In both events, extreme-ultraviolet images showed a bright plasma/current sheet below an erupting flux rope, containing multiple blobs of 2–3 arcsecond width that propagate bidirectionally along the sheet; the authors identify these blobs as plasmoids formed by tearing-mode reconnection. X-ray images during the first flare revealed double coronal sources at the two ends of the sheet, plus a transient faint 6–12 keV source between them that was co-spatial with the plasmoids and moved at about 150 km per second, matching the EUV blobs. Simultaneous X-ray and radio observations showed quasi-periodic pulsations of about 10 seconds (decimetric radio) and about 100 seconds (X-ray 12–25 keV) that are temporally related to plasmoid ejection and coalescence. The paper concludes that energetic electrons are accelerated during the ejection and coalescence of multiple plasmoids in the flare current sheet, and that the observed radio/X-ray pulsations are the radiative signature of this plasmoid-mediated reconnection, consistent with the predictions of MHD simulations of kink-unstable flux ropes.

Load-bearing premise

The load-bearing premise is that the bright EUV blobs really are reconnection plasmoids in a current sheet viewed edge-on; if they are instead projections of unrelated coronal loops or wave-like features along the line of sight, the claimed plasmoid-QPP connection would lose its physical basis.

Editorial extensions

If this is right

  • X-ray and radio quasi-periodic pulsations can be read as diagnostics of plasmoid-mediated reconnection in flare current sheets, not merely as generic MHD oscillations.
  • Energetic electrons are accelerated at the flare current sheet during the ejection and coalescence of plasmoids, supporting kinetic and MHD models of fast reconnection as a particle-acceleration site.
  • Double coronal X-ray sources are located at the two ends of the current sheet with the energy-release site between them, and the transient source between them is associated with upward-moving plasmoids.
  • Confined/failed eruptions still generate substantial current-sheet reconnection and particle acceleration, with the kink instability organizing the sheet into a double structure along the flux-rope legs.
  • The 10-second radio periodicity is consistent with MHD sausage-mode oscillations of plasmoids: for a plasmoid width of about 2000 km, the implied Alfvén speed is about 200 km/s, matching the observed plasmoid speeds.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Outside the paper's claims: if plasmoid dynamics are the common driver, then quasi-periodic pulsations seen in flares where individual plasmoids are not resolved (for example in microwave or hard X-ray light curves) could also be attributed to plasmoid-mediated reconnection, greatly widening the diagnostic reach of this result.
  • Outside the paper's claims: the 10-second periodicity could be directly tested with next-generation EUV imaging at sub-10-second cadence; if the pulsations continue without corresponding plasmoid oscillations, the MHD-wave alternative would be favoured.
  • Outside the paper's claims: the same plasmoid-QPP link could be looked for in magnetospheric or laboratory reconnection events, where current-sheet plasmoids and particle fluxes are measured directly, providing a controlled test of the mechanism.
  • Outside the paper's claims: the repeated arrest of both flux ropes near 45 Mm suggests a shared overlying strapping-field constraint; comparing kinking versus non-kinking confined eruptions would isolate the kink instability's specific role in forming the double current sheet.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

5 major / 6 minor

Summary. This paper analyzes two successive confined flares observed on 2015 April 22 in AR 12322 using SDO/AIA EUV imaging, RHESSI X-ray images, Fermi GBM light curves, and metric/decimetric radio spectra. The authors report direct imaging of multiple small plasma blobs moving along bright plasma/current sheets beneath erupting flux ropes, which they interpret as plasmoids. They detect double coronal X-ray sources at both ends of the current/plasma sheet, a transient faint X-ray source between them, and quasi-periodic pulsations (QPPs) with periods near 100 s in soft/hard X-rays and near 10 s in radio, which they associate with plasmoid ejection and coalescence. The observational phenomenology is compared with an MHD simulation of a kink-unstable flux rope, and the paper concludes that energetic electrons are accelerated during the ejection and coalescence of multiple plasmoids.

Significance. If the association between QPPs and plasmoids is correct, this would provide one of the first direct observational links between plasmoid dynamics in flare current sheets and quasi-periodic particle acceleration, with broad implications for plasmoid-mediated reconnection and particle acceleration models. The paper's strengths include the multi-instrument dataset, direct EUV imaging with time-distance analysis of multiple moving blobs, the detection of double coronal X-ray sources with a candidate interposed source, wavelet analysis of QPPs with 95% significance contours, and DEM analysis of the plasma sheet. The supplementary movies and data in Zenodo are an asset, and the use of a publicly available wavelet code aids reproducibility. However, the interpretation rests on the morphological identification of blobs as plasmoids and on qualitative temporal correlations; these are the load-bearing points that need quantitative support before the central claim can be considered established.

major comments (5)
  1. [§3.3, Conclusion (vi)] The central claim that the 100-s and 10-s QPPs are associated with plasmoid ejection and coalescence is supported only by visual temporal association: the text states that blob ejections are 'nearly associated' with X-ray peaks (Figure 3(c), Movie S2) and that the 100-s periodicity is 'correlated with the creation of multiple plasmoids' without presenting any cross-correlation, phase-folding, or event-count significance test. For the 10-s period, the authors explicitly acknowledge in §3.3 that the AIA 12-s cadence is not sufficient to detect oscillations, so the sausage-mode interpretation is a hypothesis supported only by a consistency check using P=L/VA. To make the association load-bearing, I recommend computing a quantitative correlation between the detrended GBM light curves and the blob occurrence/merger times extracted from the time-distance plots, with an appropriate null-hypothesis significance level, and rephrasing the 10-s-period claim as a suggested mechanism rather than an observed association.
  2. [§2.1, Figures 3(a,c) and 8(b-d)] Blob speeds and QPP periods are quoted without uncertainties. For example, the upward blob speeds of 228, 203, 208, 295, 323, 370, and 210 km/s during the first flare and 134-330 km/s during the second flare are read from time-distance plots, but no error bars are given despite the finite AIA pixel scale (0.6 arcsec) and 12-s cadence. Wavelet periods of ~100 s and ~10 s are reported as point values without confidence intervals or the number of significant cycles. Because the paper's physical comparisons (the 100-s period versus plasmoid cadence and the 10-s period versus the Alfvén speed) depend on these values, formal uncertainties are needed.
  3. [§2.1, Figure 5] The faint X-ray source S3 that appears between the double coronal sources is a critical piece of evidence for particle acceleration co-spatial with plasmoids. It is reconstructed as a 6-12 keV CLEAN feature at 40-80% peak contours in a single 60-s integration, near the limb and in the vicinity of the much brighter sources S1 and S2. The paper does not report the source's significance relative to CLEAN residuals, the number of counts in the source region, or the synthesized beam size. I recommend showing the clean-residual map, comparing with a different imaging algorithm such as MEM, and quantifying the flux and its uncertainty before interpreting S3 as a real, transient X-ray source.
  4. [§3.1, §4] The identification of the EUV blobs as reconnection plasmoids in an edge-on flare current sheet is inferred from morphology and from qualitative similarity to the MHD simulation. The text states 'We interpret these blobs as plasmoids formed by reconnection in the flare current sheet' and conclusion (i) and (iii) use the word 'confirm.' Because projection effects at the limb can produce apparent moving brightenings from unrelated coronal structures or wave-like features, the stated conclusions are stronger than the evidence. Please either soften the wording or provide a quantitative test, such as comparing the observed blob trajectories and DEM profiles with synthetic observations generated from the MHD simulation, rather than a side-by-side visual comparison.
  5. [§3.1, Figure 9] The MHD simulation used to support the plasmoid interpretation is cited as 'Dahlin et al., in preparation,' and the setup is described only minimally ('the lower resolution was employed'; no initial equilibrium, domain size, or Lundquist number is given). Since the comparison is used to validate the interpretation of the observations, the simulation parameters and relevant run details must be provided in the text or in an appendix, or the figure should be based on a published simulation. As written, the claimed 'strikingly similar' comparison cannot be reproduced or independently evaluated.
minor comments (6)
  1. [§2] In the sentence 'The active region NOAA 12322 was located on the west limb (N11W91) on 22 April 22 2015,' the date contains a duplicate '22'; it should read '22 April 2015.'
  2. [Movie S2 and Figure 3] The instrument name is written consistently as 'ORFEES' in the text but appears as 'ORFESS' in the Movie S2 description; please unify the spelling.
  3. [§1] The Introduction mentions the Nancay Radioheliograph (NRH) and its relevance to decimetric sources, but no NRH data are analyzed in the paper; please either include NRH observations or explicitly state that NRH data were not available for this event.
  4. [Figure A.3, A.4] The wavelet analysis uses a 'red trend' for detrending but does not specify the detrending method or the mother wavelet used; adding these details would improve reproducibility.
  5. [Table 1] The spectral fitting intervals are labeled '1, 2, 3' and '4,5' for the first flare and '1,2' for the second, but the actual UTC intervals are not defined in the table; please list the corresponding times.
  6. [§3.3] In the consistency estimate P=L/VA, L is described as the plasmoid width; please clarify whether L is the diameter or radius and provide a reference for the sausage-mode period relation used.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the QPP periods and plasmoid kinematics are measured from independent observations, and the MHD simulation comparison is illustrative rather than load-bearing.

full rationale

The paper's central chain is observational, not derivational: AIA time-distance plots yield plasmoid sizes, speeds, and ejection times; Fermi/RHESSI and RSTN/e-Callisto light curves yield 100-s and 10-s QPP periods through wavelet analysis; and the claimed plasmoid-QPP association is drawn from temporal and spatial coincidence in these independent datasets. No parameter is fitted to the X-ray or radio signal and then reused to predict that same signal. The 10-s period is explicitly acknowledged to be unresolvable in EUV at AIA cadence, which limits support but does not create a circular reduction. The authors' MHD simulation (Dahlin et al., in preparation) and the Kliem et al. (2010) simulation are used as morphological comparisons; the observational conclusion does not reduce to accepting those simulations. Self-citations (Dahlin et al. 2022, Kumar et al. 2023) provide context but are not the source of the measured periods. Hence no circular step is present; the only caveat is minor non-load-bearing self-citation.

Assumptions & free parameters 0 free parameters · 5 assumptions · 0 invented entities

The central claim rests primarily on the interpretation of observed blobs as reconnection plasmoids and on the assumed edge-on geometry of the current sheet. No free parameters are fitted to produce the main result; the QPP periods are measured. Standard spectral and plasma-emission models are used for secondary density and temperature estimates.

assumptions (5)
  • domain assumption EUV blobs are plasmoids formed by magnetic reconnection in the flare current sheet
    This identification underlies the entire interpretation of bidirectional motions and QPP association; it is inferred from morphology and kinematics, not directly measured.
  • domain assumption The bright plasma sheets are current sheets viewed approximately edge-on beneath the erupting flux rope
    Used to map blob motions along the reconnection outflow; if the geometry is different, the bidirectional plasmoid interpretation changes.
  • domain assumption Radio decimetric bursts are plasma emission from accelerated electrons interacting with ambient plasma
    Used to convert radio frequencies to plasma densities and to link bursts to electron beams; an alternative emission mechanism would alter the inferred source conditions.
  • domain assumption Fermi GBM X-ray spectra can be fit with thin-target bremsstrahlung plus thermal components
    Used to derive temperature, emission measure, and electron spectral index; systematic errors in the assumed radiation model propagate to those values.
  • standard math Wavelet significance levels (95%) are valid for detrended light curves
    Standard Torrence and Compo wavelet method; assumptions about noise and detrending are not discussed in detail.

how reviews work

0 comments
Cite this review

Pith. "Pith review of X-ray/Radio Quasi-periodic Pulsations Associated with Plasmoids in Solar Flare Current Sheets." pith.science (2026). https://pith.science/paper/MW232NLD

@misc{pith2026241205193,
  author       = {Pith},
  title        = {Pith review of: X-ray/Radio Quasi-periodic Pulsations Associated with Plasmoids in Solar Flare Current Sheets},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MW232NLD}},
  note         = {Machine review of arXiv:2412.05193}
}
abstract

Plasmoids (or magnetic islands) are believed to play an important role in the onset of fast magnetic reconnection and particle acceleration during solar flares and eruptions. Direct imaging of flare current sheets and formation/ejection of multiple plasmoids in extreme ultraviolet (EUV) images, along with simultaneous X-ray and radio observations, offers significant insights into the mechanisms driving particle acceleration in solar flares. Here we present direct imaging of the formation and ejection of multiple plasmoids in flare plasma/current sheets and associated quasi-periodic pulsations (QPPs) observed in X-ray and radio wavelengths, using observations from SDO/AIA, RHESSI, and Fermi GBM. These plasmoids propagate bidirectionally upward and downward along the flare current sheet beneath the erupting flux rope during two successive flares associated with confined/failed eruptions. The flux rope exhibits evidence of helical kink instability with formation and ejection of multiple plasmoids in the flare current sheet, as predicted in an MHD simulation of a kink-unstable flux rope. RHESSI X-ray images show double coronal sources (``loop-top" and higher coronal sources) located at both ends of the flare current/plasma sheet. Moreover, we detected an additional transient faint X-ray source (6-12 keV) located between the double coronal sources, which was co-spatial with multiple plasmoids in the flare current sheet. X-ray (soft and hard) and radio (decimetric) observations unveil QPPs (periods$\approx$10-s and 100-s) associated with the ejection and coalescence of plasmoids. These observations suggest that energetic electrons are accelerated during the ejection and coalescence of multiple plasmoids in the flare current sheet.

Figures

Figures reproduced from arXiv: 2412.05193 by the authors.

Figure 1
Figure 1. NOAA active region 12322 and associated flares. [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Flux rope and blobs during the first flare (C3.8). [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. X-ray and radio emissions associated with the ejection [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Evolution of X-ray sources (6-12 keV) during the first flare (C3.8) from 08:10-08:13 UT. [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]
Figure 5
Figure 5. Figure 5: Evolution of X-ray sources (6-12 keV) during the first flare (C3.8) from 08:14-08:19 UT. [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]
Figure 6
Figure 6. Figure 6: Initiation of the second flare (M1.1) associated with a filament (F) eruption (08:28-08:34 UT). [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: Evolution of plasma sheets and blobs during the second flare (M1.1) from 08:37-08:40 UT. [PITH_FULL_IMAGE:figures/full_fig_p010_7.png]
Figure 8
Figure 8. Figure 8: Formation and ejection of upward/downward moving blobs and associated decimetric/metric radio bursts during the second flare (M1.1). (a) e-Callisto dynamic radio spectrum (250-350 MHz) from the KRIM station (Crimean Astrophysical Observatory). The dotted curve is the G…
Figure 9
Figure 9. Figure 9: 3D MHD simulation of formation and evolution of multiple plasmoids in a flare current sheet underneath an erupting flux [PITH_FULL_IMAGE:figures/full_fig_p012_9.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

81 extracted references · 29 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    * _=U `@b www6 -1) o ?VK< *) #p. Hy`ph VuގgI zXA305 SIk8 _l/ pi v& N

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    2021

  4. [4]

    Alexander , D., Liu , R., & Gilbert , H. R. 2006, , 653, 719, 10.1086/508137

    work page doi:10.1086/508137 2006

  5. [5]

    F., Swisdak , M., et al

    Arnold , H., Drake , J. F., Swisdak , M., et al. 2021, , 126, 135101, 10.1103/PhysRevLett.126.135101

    doi:10.1103/physrevlett.126.135101 2021

  6. [6]

    J., Metcalf, T

    Aschwanden, M. J., Metcalf, T. R., Krucker, S., et al. 2004, SoPh, 219, 149, 10.1023/b:sola.0000021801.83038.aa

    arXiv 2004

  7. [7]

    2004, , 615, 526, 10.1086/424374

    Aurass , H., & Mann , G. 2004, , 615, 526, 10.1086/424374

    work page doi:10.1086/424374 2004

  8. [8]

    2002, , 384, 273, 10.1051/0004-6361:20011735

    Aurass , H., Vr s nak , B., & Mann , G. 2002, , 384, 273, 10.1051/0004-6361:20011735

    doi:10.1051/0004-6361:20011735 2002

Show all 81 references
  1. [9]

    2011, , 737, 24, 10.1088/0004-637X/737/1/24

    B \'a rta , M., B \"u chner , J., Karlick \'y , M., & Sk \'a la , J. 2011, , 737, 24, 10.1088/0004-637X/737/1/24

    2011 doi

  2. [10]

    2008, , 477, 649, 10.1051/0004-6361:20078266

    B \'a rta , M., Vr s nak , B., & Karlick \'y , M. 2008, , 477, 649, 10.1051/0004-6361:20078266

    2008 doi

  3. [11]

    Benz , A. O. 2017, Living Reviews in Solar Physics, 14, 2, 10.1007/s41116-016-0004-3

    2017 doi

  4. [12]

    O., Battaglia , M., & Vilmer , N

    Benz , A. O., Battaglia , M., & Vilmer , N. 2011, , 273, 363, 10.1007/s11207-011-9760-3

    2011 doi

  5. [13]

    O., Monstein , C., Meyer , H., et al

    Benz , A. O., Monstein , C., Meyer , H., et al. 2009, Earth Moon and Planets, 104, 277, 10.1007/s11038-008-9267-6

    2009 doi

  6. [14]

    2009, Physics of Plasmas, 16, 112102, 10.1063/1.3264103

    Bhattacharjee , A., Huang , Y.-M., Yang , H., & Rogers , B. 2009, Physics of Plasmas, 16, 112102, 10.1063/1.3264103

    2009 doi

  7. [15]

    L., Kaiser , M

    Bougeret , J. L., Kaiser , M. L., Kellogg , P. J., et al. 1995, , 71, 231, 10.1007/BF00751331

    1995 doi

  8. [16]

    S., Shen , C., et al

    Chen , B., Bastian , T. S., Shen , C., et al. 2015, Science, 350, 1238, 10.1126/science.aac8467

    2015 doi

  9. [17]

    E., et al

    Chen , B., Shen , C., Gary , D. E., et al. 2020, Nature Astronomy, 4, 1140, 10.1038/s41550-020-1147-7

    2020 doi

  10. [18]

    J., Bhattacharjee , A., Puhl-Quinn , P

    Chen , L. J., Bhattacharjee , A., Puhl-Quinn , P. A., et al. 2008, Nature Physics, 4, 19, 10.1038/nphys777

    2008 doi

  11. [19]

    Chen , P. F. 2011, Living Reviews in Solar Physics, 8, 1

    2011

  12. [20]

    Cheung , M. C. M., Boerner , P., Schrijver , C. J., et al. 2015, Astrophys. J., 807, 143, 10.1088/0004-637X/807/2/143

    2015 doi

  13. [21]

    2009, , 703, 1, 10.1088/0004-637X/703/1/1

    Cho , K.-S., Lee , J., Bong , S.-C., et al. 2009, , 703, 1, 10.1088/0004-637X/703/1/1

    2009 doi

  14. [22]

    T., Antiochos , S

    Dahlin , J. T., Antiochos , S. K., Qiu , J., & DeVore , C. R. 2022, , 932, 94, 10.3847/1538-4357/ac6e3d

    2022 doi

  15. [23]

    T., Drake , J

    Dahlin , J. T., Drake , J. F., & Swisdak , M. 2014, Physics of Plasmas, 21, 092304, 10.1063/1.4894484

    2014 doi

  16. [24]

    2017, Physics of Plasmas, 24, 092110, 10.1063/1.4986211

    ---. 2017, Physics of Plasmas, 24, 092110, 10.1063/1.4986211

    2017 doi

  17. [25]

    DeForest , C. E. 2017, , 838, 155, 10.3847/1538-4357/aa67f1

    2017 doi

  18. [26]

    Y., Hurford , G

    Dennis , B., Shih , A. Y., Hurford , G. J., & Saint-Hilaire , P. 2022, in Handbook of X-ray and Gamma-ray Astrophysics, ed. C. Bambi & A. Sangangelo , 63, 10.1007/978-981-16-4544-0_169-1

    2022 doi

  19. [27]

    R., & Antiochos , S

    DeVore , C. R., & Antiochos , S. K. 2008, , 680, 740, 10.1086/588011

    2008 doi

  20. [28]

    F., Swisdak , M., Che , H., & Shay , M

    Drake , J. F., Swisdak , M., Che , H., & Shay , M. A. 2006, Nature, 443, 553, 10.1038/nature05116

    2006 doi

  21. [29]

    F., Swisdak , M., & Fermo , R

    Drake , J. F., Swisdak , M., & Fermo , R. 2013, , 763, L5, 10.1088/2041-8205/763/1/L5

    2013 doi

  22. [30]

    E., DeVore , C

    Guidoni , S. E., DeVore , C. R., Karpen , J. T., & Lynch , B. J. 2016, Astrophys. J., 820, 60, 10.3847/0004-637X/820/1/60

    2016 doi

  23. [31]

    2021, Journal of Space Weather and Space Climate, 11, 57, 10.1051/swsc/2021039

    Hamini , A., Auxepaules , G., Bir \'e e , L., et al. 2021, Journal of Space Weather and Space Climate, 11, 57, 10.1051/swsc/2021039

    2021

  24. [32]

    A., Inglis , A

    Hayes , L. A., Inglis , A. R., Christe , S., Dennis , B., & Gallagher , P. T. 2020, , 895, 50, 10.3847/1538-4357/ab8d40

    2020 doi

  25. [33]

    2010, Physics of Plasmas, 17, 062104, 10.1063/1.3420208

    Huang , Y.-M., & Bhattacharjee , A. 2010, Physics of Plasmas, 17, 062104, 10.1063/1.3420208

    2010 doi

  26. [34]

    R., Nakariakov , V

    Inglis , A. R., Nakariakov , V. M., & Melnikov , V. F. 2008, , 487, 1147, 10.1051/0004-6361:20079323

    2008 doi

  27. [35]

    2017, , 847, 98, 10.3847/1538-4357/aa88a6

    Jel \' nek , P., Karlick \'y , M., Van Doorsselaere , T., & B \'a rta , M. 2017, , 847, 98, 10.3847/1538-4357/aa88a6

    2017 doi

  28. [36]

    R., Kai , K., Kosugi , T., et al

    Kane , S. R., Kai , K., Kosugi , T., et al. 1983, , 271, 376, 10.1086/161203

    1983 doi

  29. [37]

    2004, , 417, 325, 10.1051/0004-6361:20034249

    Karlick \'y , M. 2004, , 417, 325, 10.1051/0004-6361:20034249

    2004 doi

  30. [38]

    2011, , 733, 107, 10.1088/0004-637X/733/2/107

    Karlick \'y , M., & B \'a rta , M. 2011, , 733, 107, 10.1088/0004-637X/733/2/107

    2011 doi

  31. [39]

    2010, , 514, A28, 10.1051/0004-6361/200913547

    Karlick \'y , M., B \'a rta , M., & Ryb \'a k , J. 2010, , 514, A28, 10.1051/0004-6361/200913547

    2010 doi

  32. [40]

    2010, , 266, 71, 10.1007/s11207-010-9606-4

    Karlick \'y , M., & Kliem , B. 2010, , 266, 71, 10.1007/s11207-010-9606-4

    2010 doi

  33. [41]

    T., Antiochos , S

    Karpen , J. T., Antiochos , S. K., & DeVore , C. R. 2012, Astrophys. J., 760, 81, 10.1088/0004-637X/760/1/81

    2012 doi

  34. [42]

    Kliem , B., Karlick \'y , M., & Benz , A. O. 2000, , 360, 715, 10.48550/arXiv.astro-ph/0006324

    2000 doi arXiv

  35. [43]

    G., T \"o r \"o k , T., & Karlick \'y , M

    Kliem , B., Linton , M. G., T \"o r \"o k , T., & Karlick \'y , M. 2010, , 266, 91, 10.1007/s11207-010-9609-1

    2010 doi

  36. [44]

    J., et al

    Krucker , S., Battaglia , M., Cargill , P. J., et al. 2008, , 16, 155, 10.1007/s00159-008-0014-9

    2008 doi

  37. [45]

    2013, Astronomy and Astrophysics, 557, A115, 10.1051/0004-6361/201220999

    Kumar , P., & Cho , K.-S. 2013, Astronomy and Astrophysics, 557, A115, 10.1051/0004-6361/201220999

    2013 doi

  38. [46]

    T., Antiochos , S

    Kumar , P., Karpen , J. T., Antiochos , S. K., et al. 2023, , 943, 156, 10.3847/1538-4357/acaea4

    2023 doi

  39. [47]

    T., Antiochos , S

    Kumar , P., Karpen , J. T., Antiochos , S. K., Wyper , P. F., & DeVore , C. R. 2019, , 885, L15, 10.3847/2041-8213/ab45f9

    2019 doi

  40. [48]

    T., Yurchyshyn , V., DeVore , C

    Kumar , P., Karpen , J. T., Yurchyshyn , V., DeVore , C. R., & Antiochos , S. K. 2024, arXiv e-prints, arXiv:2407.07687, 10.48550/arXiv.2407.07687

    2024 doi arXiv

  41. [49]

    M., & Cho , K.-S

    Kumar , P., Nakariakov , V. M., & Cho , K.-S. 2016, , 822, 7, 10.3847/0004-637X/822/1/7

    2016 doi

  42. [50]

    2017 a , , 836, 121, 10.3847/1538-4357/836/1/121

    ---. 2017 a , , 836, 121, 10.3847/1538-4357/836/1/121

    2017 doi

  43. [51]

    2017 b , Astrophys

    ---. 2017 b , Astrophys. J., 844, 149, 10.3847/1538-4357/aa7d53

    2017 doi

  44. [52]

    M., Karpen , J

    Kumar , P., Nakariakov , V. M., Karpen , J. T., Richard DeVore , C., & Cho , K.-S. 2022, , 932, L9, 10.3847/2041-8213/ac6e3e

    2022 doi

  45. [53]

    R., Title , A

    Lemen , J. R., Title , A. M., Akin , D. J., et al. 2012, Sol. Phys., 275, 17, 10.1007/s11207-011-9776-8

    2012 doi

  46. [54]

    P., Dennis , B

    Lin , R. P., Dennis , B. R., Hurford , G. J., et al. 2002, Sol. Phys., 210, 3, 10.1023/A:1022428818870

    2002 doi

  47. [55]

    R., & Jiang , Y

    Liu , W., Petrosian , V., Dennis , B. R., & Jiang , Y. W. 2008, , 676, 704, 10.1086/527538

    2008 doi

  48. [56]

    F., Schekochihin , A

    Loureiro , N. F., Schekochihin , A. A., & Cowley , S. C. 2007, Physics of Plasmas, 14, 100703, 10.1063/1.2783986

    2007 doi

  49. [57]

    J., & Edmondson , J

    Lynch , B. J., & Edmondson , J. K. 2013, Astrophys. J., 764, 87, 10.1088/0004-637X/764/1/87

    2013 doi

  50. [58]

    J., Masson , S., Li , Y., et al

    Lynch , B. J., Masson , S., Li , Y., et al. 2016, Journal of Geophysical Research (Space Physics), 121, 10677, 10.1002/2016JA023432

    2016 doi

  51. [59]

    1994, , 371, 495, 10.1038/371495a0

    Masuda , S., Kosugi , T., Hara , H., Tsuneta , S., & Ogawara , Y. 1994, , 371, 495, 10.1038/371495a0

    1994 doi

  52. [60]

    A., Nakariakov , V

    McLaughlin , J. A., Nakariakov , V. M., Dominique , M., Jel \' nek , P., & Takasao , S. 2018, , 214, 45, 10.1007/s11214-018-0478-5

    2018 doi

  53. [61]

    N., et al

    Meegan , C., Lichti , G., Bhat , P. N., et al. 2009, , 702, 791, 10.1088/0004-637X/702/1/791

    2009 doi

  54. [62]

    O., McAteer , R

    Milligan , R. O., McAteer , R. T. J., Dennis , B. R., & Young , C. A. 2010, , 713, 1292, 10.1088/0004-637X/713/2/1292

    2010 doi

  55. [63]

    M., & Melnikov , V

    Nakariakov , V. M., & Melnikov , V. F. 2009, Space Sci. Rev., 149, 119, 10.1007/s11214-009-9536-3

    2009 doi

  56. [64]

    M., Melnikov , V

    Nakariakov , V. M., Melnikov , V. F., & Reznikova , V. E. 2003, , 412, L7, 10.1051/0004-6361:20031660

    2003 doi

  57. [65]

    Neupert , W. M. 1968, , 153, L59, 10.1086/180220

    1968 doi

  58. [66]

    D., Krucker , S., Fujimoto , M., & Shinohara , I

    Oka , M., Phan , T. D., Krucker , S., Fujimoto , M., & Shinohara , I. 2010, , 714, 915, 10.1088/0004-637X/714/1/915

    2010 doi

  59. [67]

    Petschek , H. E. 1964, in NASA Special Publication, ed. W. N. Hess , Vol. 50, 425

    1964

  60. [68]

    D., Drake , J

    Phan , T. D., Drake , J. F., Larson , D., et al. 2024, , 971, L42, 10.3847/2041-8213/ad6841

    2024 doi

  61. [69]

    2005, , 625, 1019, 10.1086/429530

    Pick , M., D \'e moulin , P., Krucker , S., Malandraki , O., & Maia , D. 2005, , 625, 1019, 10.1086/429530

    2005 doi

  62. [70]

    2011, Living Reviews in Solar Physics, 8, 6

    Shibata , K., & Magara , T. 2011, Living Reviews in Solar Physics, 8, 6

    2011

  63. [71]

    2001, Earth, Planets, and Space, 53, 473

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

    2001

  64. [72]

    Sui , L., & Holman , G. D. 2003, , 596, L251, 10.1086/379343

    2003 doi

  65. [73]

    D., & Dennis , B

    Sui , L., Holman , G. D., & Dennis , B. R. 2004, , 612, 546, 10.1086/422515

    2004 doi

  66. [74]

    2012, Astrophys

    Takasao , S., Asai , A., Isobe , H., & Shibata , K. 2012, Astrophys. J. Lett., 745, L6, 10.1088/2041-8205/745/1/L6

    2012 doi

  67. [75]

    2016, , 828, 103, 10.3847/0004-637X/828/2/103

    ---. 2016, , 828, 103, 10.3847/0004-637X/828/2/103

    2016 doi

  68. [76]

    2020, OSPEX: Object Spectral Executive , Astrophysics Source Code Library, record ascl:2007.018

    Tolbert , K., & Schwartz , R. 2020, OSPEX: Object Spectral Executive , Astrophysics Source Code Library, record ascl:2007.018

    2020

  69. [77]

    Torrence , C., & Compo , G. P. 1998, Bulletin of the American Meteorological Society, 79, 61, 10.1175/1520-0477(1998)079<0061:APGTWA>2.0.CO;2

    1998 doi

  70. [78]

    P., & The Rhessi Team

    Vilmer , N., Krucker , S., Lin , R. P., & The Rhessi Team . 2002, , 210, 261, 10.1023/A:1022492414597

    2002 doi

  71. [79]

    2007, , 661, L207, 10.1086/519004

    Wang , T., Sui , L., & Qiu , J. 2007, , 661, L207, 10.1086/519004

    2007 doi

  72. [80]

    P., Brooks , D

    Warren , H. P., Brooks , D. H., Ugarte-Urra , I., et al. 2018, Astrophys. J., 854, 122, 10.3847/1538-4357/aaa9b8

    2018 doi

  73. [81]

    V., McLaughlin , J

    Zimovets , I. V., McLaughlin , J. A., Srivastava , A. K., et al. 2021, , 217, 66, 10.1007/s11214-021-00840-9

    2021 doi

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.