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arxiv: 2606.10506 · v1 · pith:4S7VOUCLnew · submitted 2026-06-09 · 🌌 astro-ph.SR · astro-ph.HE

Phase-drifting with emitting plasma temperature in the quasi-periodic pulsations of an X-class solar flare

Libo Fu , Valery M. Nakariakov , Ding Yuan , Suraj Sahu , Song Feng , Ehsan Tavabi This is my paper

Pith reviewed 2026-06-27 12:02 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords solar flarequasi-periodic pulsationsphase driftingmagnetic reconnectionmulti-wavelength observationsplasma temperaturehard X-rayEUV
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The pith

Quasi-periodic pulsations in an X-class solar flare exhibit phase drifting that increases from hottest to cooler emitting plasma channels.

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

The paper detects a short-lived ~5-minute QPP simultaneously in hard X-rays, EUV, and soft X-rays during an X-class flare. All channels share nearly identical periods, yet the phase delay relative to the hard X-ray signal grows systematically as the passbands respond to cooler plasma. The authors interpret this as periodic magnetic reconnection first modulating non-thermal electrons, after which heating and cooling occur sequentially across temperature-sensitive diagnostics. A reader would care because the pattern supplies an observable clock for the sequence of energy release and plasma response in flares.

Core claim

In an X-class solar flare, a ~5-minute QPP appears across hard X-ray, EUV, and soft X-ray bands with identical periods but a clear temperature-dependent phase drift, the delay relative to hard X-rays increasing from the hottest to cooler channels. The QPP lasts only a few cycles in the impulsive phase. These properties are taken to indicate that periodic reconnection modulates non-thermal electrons for the leading hard X-ray signal, after which plasma heating and cooling manifest sequentially in passbands of differing temperature response.

What carries the argument

Temperature-dependent phase drifting revealed by phase-resolved timing analysis across multi-wavelength, multi-temperature diagnostics.

If this is right

  • QPPs share nearly identical oscillation periods in all diagnostics.
  • Phase delay relative to hard X-ray emission increases systematically from hottest to cooler EUV channels.
  • The QPP persists for only a few cycles during the impulsive phase.
  • Multi-temperature, multi-wavelength phase relationships can constrain the temporal evolution of flare energy release.

Where Pith is reading between the lines

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

  • The 5-minute period points to possible leakage of photospheric oscillations as a trigger for the reconnection.
  • Similar temperature-ordered phase drifting may appear in other flares and could be used to test whether heating follows reconnection in a repeatable sequence.
  • The method offers a way to separate the timing of particle acceleration from the subsequent thermal evolution without assuming a specific wave mode.

Load-bearing premise

The phase delays arise from sequential heating and cooling across temperature-sensitive passbands rather than wave propagation, instrumental offsets, or differing emission mechanisms.

What would settle it

An observation in which phase delays fail to correlate with the temperature response of the passbands, or in which the drifting persists well beyond the impulsive phase, would falsify the heating-cooling sequence interpretation.

Figures

Figures reproduced from arXiv: 2606.10506 by Ding Yuan, Ehsan Tavabi, Libo Fu, Song Feng, Suraj Sahu, Valery M. Nakariakov.

Figure 1
Figure 1. Figure 1: Multi-wavelength observations of QPPs during the X1.7 flare on 2013 May 13 in NOAA AR 11748. (a) and (b) AIA 131 Å and 094 Å images of the flare. (c) Raw integrated light curves from SDO/AIA (131 Å, 094 Å, and 193 Å), GOES (1–8 Å), and RHESSI (12–25 keV). We used observations from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) [37,38]. AIA provides full-disk solar image… view at source ↗
Figure 2
Figure 2. Figure 2: Fourier power spectral analysis of QPPs during the impulsive phase of the flare. The power spectra were derived from the undetrended light curves shown in Figure 1a. Panel (a) displays the power spectrum of the AIA 131 Å signal, and (b) shows the RHESSI 12–25 keV signal spectrum. The red line represents the background red-noise model fitted using a Markov Chain Monte Carlo (MCMC) algorithm, and the dashed … view at source ↗
Figure 3
Figure 3. Figure 3: Detrended and normalized light curves from the AIA, GOES, and RHESSI channels analyzed in this study, covering 01:50–02:40 UT on 2013 May 13. The background trend was estimated with a 700 s smoothing window and removed from each light curve. The shaded region indicates the interval 02:02–02:20 UT used for the subsequent detailed analysis. No additional band-pass filtering is applied in this figure. The cur… view at source ↗
Figure 4
Figure 4. Figure 4: Cross-correlation analysis of the detrended QPP signals in the AIA 193 Å, 131 Å, 94 Å, 335 Å, and 304 Å channels, GOES 1–8 Å, and RHESSI 12–25 keV. (a) Enlarged view of the detrended and normalized light curves over the interval 02:02–02:20 UT, highlighted in [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Time lag of the QPP signal in each waveband relative to the RHESSI 12–25 keV emission as a function of representative channel temperature. The temperatures shown on the x-axis correspond to the flare-related dominant response of each AIA passband [37]. The left vertical axis is logarithmic, while the right vertical axis gives the corresponding linear scale for the error bars. The dashed line shows the best… view at source ↗
read the original abstract

Recent multi-wavelength observations of solar flares have provided new constraints on the physical origin of quasi-periodic pulsations (QPPs). In an X-class flare, we detect a short-lived $\sim$5-minute QPP simultaneously in hard X-rays, extreme-ultraviolet (EUV), and soft X-ray emissions, exhibiting a clear phase-drifting behavior with emitting plasma temperature. Based on phase-resolved timing analysis, it is found that (i) the QPPs in all diagnostics share nearly identical oscillation periods, (ii) a systematic temperature-dependent phase drifting is present, with the phase delay relative to the hard X-ray emission increases systematically from the hottest to cooler EUV channels, and (iii) the QPP persists for only a few cycles during the impulsive phase. These properties imply that periodic magnetic reconnection, possibly triggered by the leakage of 5-minute oscillations from the lower atmosphere, modulates the non-thermal electrons responsible for the leading Hard X-ray QPPs. Subsequently, plasma heating and cooling processes manifest sequentially across passbands with different temperature responses, resulting in the observed temperature-dependent phase drifting. These results provide novel observational evidence supporting the use of multi-temperature, multi-wavelength phase relationships to constrain the temporal evolution of flare energy release and the origins of QPPs.

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 paper reports the detection of a short-lived ~5-minute QPP in an X-class solar flare, observed simultaneously in hard X-ray, EUV, and soft X-ray emissions. Phase-resolved timing analysis is claimed to reveal three properties: (i) nearly identical oscillation periods across all diagnostics, (ii) systematic temperature-dependent phase drifting with increasing delay from HXR to cooler EUV channels, and (iii) persistence for only a few cycles during the impulsive phase. These are interpreted as evidence that periodic magnetic reconnection (possibly triggered by leakage of 5-minute oscillations from the lower atmosphere) modulates non-thermal electrons, followed by sequential plasma heating and cooling across temperature-sensitive passbands.

Significance. If the phase-drifting interpretation holds after quantitative validation, the result would supply useful observational constraints on QPP origins in flares by linking multi-temperature phase relationships to the sequence of energy release and thermal evolution. It strengthens the case for using cross-passband timing to distinguish reconnection-driven modulation from other mechanisms. The single-event nature and lack of reported statistical anchors currently limit the strength of this contribution.

major comments (2)
  1. Abstract (phase-resolved timing analysis paragraph): the claim that the analysis supports the three listed properties is load-bearing for the central interpretation, yet the abstract supplies no error bars on measured periods or phase delays, no statistical significance tests, no data exclusion criteria, and no reference to raw light-curve figures or fitting procedures. This absence prevents assessment of whether the reported temperature-dependent drift is robust.
  2. Abstract (final interpretive sentence): the inference that observed phase delays arise specifically from sequential heating and cooling (rather than wave propagation at coronal sound/Alfvén speeds, instrumental timing offsets, or emission-mechanism differences) is not accompanied by any quantitative comparison of measured delays to expected cooling timescales from hydrodynamic models or to propagation delays. This assumption directly underpins the proposed periodic-reconnection scenario and requires explicit exclusion of alternatives to remain viable.
minor comments (1)
  1. Abstract: a brief statement of the specific instruments, passbands, and time resolution used for the multi-wavelength data would improve reproducibility without altering the central claim.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful comments, which help clarify the presentation of our phase-resolved timing results. We address each major comment below and indicate where revisions will be made.

read point-by-point responses

  1. Referee: [—] Abstract (phase-resolved timing analysis paragraph): the claim that the analysis supports the three listed properties is load-bearing for the central interpretation, yet the abstract supplies no error bars on measured periods or phase delays, no statistical significance tests, no data exclusion criteria, and no reference to raw light-curve figures or fitting procedures. This absence prevents assessment of whether the reported temperature-dependent drift is robust.

    Authors: The abstract is intentionally concise, but the supporting quantitative details (period uncertainties from wavelet analysis, phase-delay measurements with standard errors, data selection criteria, and references to the raw light curves in Figures 1–3 and the fitting procedures in Section 3) are fully reported in the main text. We agree that a brief pointer in the abstract would aid readers and will revise the abstract to include a short clause referencing the methods and key figures while preserving length constraints. revision: partial

  2. Referee: [—] Abstract (final interpretive sentence): the inference that observed phase delays arise specifically from sequential heating and cooling (rather than wave propagation at coronal sound/Alfvén speeds, instrumental timing offsets, or emission-mechanism differences) is not accompanied by any quantitative comparison of measured delays to expected cooling timescales from hydrodynamic models or to propagation delays. This assumption directly underpins the proposed periodic-reconnection scenario and requires explicit exclusion of alternatives to remain viable.

    Authors: We accept that the abstract’s interpretive sentence would be strengthened by explicit comparison. In the revised manuscript we will expand the discussion (Section 4) to include order-of-magnitude estimates of cooling timescales from hydrodynamic flare models and propagation delays at typical coronal sound and Alfvén speeds, showing that the observed delays are inconsistent with propagation but consistent with sequential heating/cooling. This will be cross-referenced from the abstract. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational detection and interpretation

full rationale

The paper reports multi-wavelength timing measurements of QPPs (identical periods, temperature-dependent phase drift, short-lived impulsive-phase signal) and offers a physical interpretation linking them to periodic reconnection plus sequential heating/cooling. No equations, fitted parameters, or self-citations are shown that reduce any claimed result to its own inputs by construction. The derivation chain consists of direct data properties followed by inference; the inference step is falsifiable against external models but does not contain self-referential reduction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on domain assumptions about the temperature responses of the observed passbands and on the interpretive step that attributes phase delays to sequential heating/cooling; no free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Standard assumptions about the temperature response functions of EUV and X-ray passbands in solar flare observations
    The mapping of phase delay to temperature sequence requires these response functions to be known and distinct.
  • ad hoc to paper Phase delays arise from sequential plasma heating and cooling rather than propagation or instrumental effects
    This interpretive premise directly supports the claimed physical scenario.

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discussion (0)

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Reference graph

Works this paper leans on

56 extracted references · 54 canonical work pages

  1. [1]

    Space Science Reviews , keywords =

    Nakariakov VM, Melnikov VF. 2009 Quasi-Periodic Pulsations in Solar Flares.Space Sci. Rev. 149, 119–151. (10.1007/s11214-009-9536-3)

    work page doi:10.1007/s11214-009-9536-3 2009

  2. [2]

    doi:10.1007/s11207-016-0977-z , eprint =

    Van Doorsselaere T, Kupriyanova EG, Yuan D. 2016 Quasi-periodic Pulsations in Solar and Stellar Flares: An Overview of Recent Results (Invited Review).Sol. Phys.291, 3143–3164. (10.1007/s11207-016-0977-z)

    work page doi:10.1007/s11207-016-0977-z 2016

  3. [3]

    2019 Non-stationary quasi-periodic pulsations in solar and stellar flares.Plasma Physics and Controlled Fusion61, 014024

    Nakariakov VM, Kolotkov DY, Kupriyanova EG, Mehta T, Pugh CE, Lee DH, Broomhall AM. 2019 Non-stationary quasi-periodic pulsations in solar and stellar flares.Plasma Physics and Controlled Fusion61, 014024. (10.1088/1361-6587/aad97c)

    work page doi:10.1088/1361-6587/aad97c 2019

  4. [4]

    2020 Quasi-Periodic Pulsations in Solar and Stellar Flares

    Kupriyanova E, Kolotkov D, Nakariakov V , Kaufman A. 2020 Quasi-Periodic Pulsations in Solar and Stellar Flares. Review.Solar-T errestrial Physics6, 3–23. (10.12737/stp-61202001)

    work page doi:10.12737/stp-61202001 2020

  5. [5]

    Space Science Reviews , keywords =

    Zimovets IV , McLaughlin JA, Srivastava AK, Kolotkov DY, Kuznetsov AA, Kupriyanova EG, Cho IH, Inglis AR, Reale F, Pascoe DJ, Tian H, Yuan D, Li D, Zhang QM. 2021 Quasi-Periodic Pulsations in Solar and Stellar Flares: A Review of Underpinning Physical Mechanisms and Their Predicted Observational Signatures.Space Sci. Rev.217, 66. (10.1007/s11214-021-00840-9)

    work page doi:10.1007/s11214-021-00840-9 2021

  6. [6]

    2010 Types of Microwave Quasi-Periodic Pulsations in Single Flaring Loops.Sol

    Kupriyanova EG, Melnikov VF, Nakariakov VM, Shibasaki K. 2010 Types of Microwave Quasi-Periodic Pulsations in Single Flaring Loops.Sol. Phys.267, 329–342. (10.1007/s11207- 010-9642-0)

    work page doi:10.1007/s11207- 2010

  7. [7]

    2012 Microwave Quasi-periodic Pulsation with Millisecond Bursts in a Solar Flare on 2011 August 9.Astrophys

    Tan B, Tan C. 2012 Microwave Quasi-periodic Pulsation with Millisecond Bursts in a Solar Flare on 2011 August 9.Astrophys. J.749, 28. (10.1088/0004-637X/749/1/28)

    work page doi:10.1088/0004-637x/749/1/28 2012

  8. [8]

    2021 Multiwavelength Quasi-periodic Pulsations in a Stellar Superflare.Astrophys

    Kolotkov DY, Nakariakov VM, Holt R, Kuznetsov AA. 2021 Multiwavelength Quasi-periodic Pulsations in a Stellar Superflare.Astrophys. J. Lett.923, L33. (10.3847/2041-8213/ac432e)

    work page doi:10.3847/2041-8213/ac432e 2021

  9. [9]

    2025 Detecting fast-variation pulsations in solar hard X-ray and radio emissions.Mon

    Li D. 2025 Detecting fast-variation pulsations in solar hard X-ray and radio emissions.Mon. Not. R. Astron. Soc.542, L48–L52. (10.1093/mnrasl/slaf066)

    work page doi:10.1093/mnrasl/slaf066 2025

  10. [10]

    2024 Long-period energy releases during a C2.8 flare

    Li D, Li J, Shen J, Song Q, Ji H, Ning Z. 2024 Long-period energy releases during a C2.8 flare. Astron. Astrophys.690, A39. (10.1051/0004-6361/202450622)

    work page doi:10.1051/0004-6361/202450622 2024

  11. [11]

    The Astrophysical Journal , keywords =

    Nakariakov VM, Anfinogentov S, Storozhenko AA, Kurochkin EA, Bogod VM, Sharykin IN, Kaltman TI. 2018 Quasi-periodic Pulsations in a Solar Microflare.Astrophys. J.859, 154. (10.3847/1538-4357/aabfb9)

    work page doi:10.3847/1538-4357/aabfb9 2018

  12. [12]

    2020 Quasi-periodic Pulsation Detected in Lyα Emission During Solar Flares.Astrophys

    Li D, Lu L, Ning Z, Feng L, Gan W, Li H. 2020 Quasi-periodic Pulsation Detected in Lyα Emission During Solar Flares.Astrophys. J.893, 7. (10.3847/1538-4357/ab7cd1)

    work page doi:10.3847/1538-4357/ab7cd1 2020

  13. [15]

    2025 Quasi-Periodic Pulsations in Extreme-Ultraviolet Brightenings.Astronomy and Astrophysics698, A65

    Lim D, Van Doorsselaere T, Berghmans D, Hayes LA, Verbeeck C, Narang N, Dominique M, Inglis AR. 2025 Quasi-Periodic Pulsations in Extreme-Ultraviolet Brightenings.Astronomy and Astrophysics698, A65. (10.1051/0004-6361/202554587)

    work page doi:10.1051/0004-6361/202554587 2025

  14. [16]

    R., Hudson , H

    Fletcher L, Dennis BR, Hudson HS, Krucker S, Phillips K, Veronig A, Battaglia M, Bone L, Caspi A, Chen Q, et al.. 2011 An Observational Overview of Solar Flares.Space Sci. Rev.159, 19–106. (10.1007/s11214-010-9701-8) 11royalsocietypublishing.org/journal/rsta Phil. Trans. R. Soc. A 0000000

    work page doi:10.1007/s11214-010-9701-8 2011

  15. [17]

    2017 Flare Observations.Living Reviews in Solar Physics14, 2

    Benz AO. 2017 Flare Observations.Living Reviews in Solar Physics14, 2. (10.1007/s41116-016- 0004-3)

    work page doi:10.1007/s41116-016- 2017

  16. [18]

    2016 Statistical properties of quasi- periodic pulsations in white-light flares observed with Kepler.Mon

    Pugh CE, Armstrong DJ, Nakariakov VM, Broomhall AM. 2016 Statistical properties of quasi- periodic pulsations in white-light flares observed with Kepler.Mon. Not. R. Astron. Soc.459, 3659–3676. (10.1093/mnras/stw850)

    work page doi:10.1093/mnras/stw850 2016

  17. [19]

    doi:10.1007/s11207-015-0691-2 , eprint =

    Simões PJA, Hudson HS, Fletcher L. 2015 Soft X-Ray Pulsations in Solar Flares.Solar Physics 290, 3625–3639. (10.1007/s11207-015-0691-2)

    work page doi:10.1007/s11207-015-0691-2 2015

  18. [20]

    2018 Detection of Quasi-Periodic Pulsations in Solar EUV Time Series.Sol

    Dominique M, Zhukov AN, Dolla L, Inglis A, Lapenta G. 2018 Detection of Quasi-Periodic Pulsations in Solar EUV Time Series.Sol. Phys.293, 61. (10.1007/s11207-018-1281-x)

    work page doi:10.1007/s11207-018-1281-x 2018

  19. [22]

    The Astrophysical Journal , keywords =

    Hayes LA, Inglis AR, Christe S, Dennis B, Gallagher PT. 2020 Statistical Study of GOES X-Ray Quasi-periodic Pulsations in Solar Flares.Astrophys. J.895, 50. (10.3847/1538-4357/ab8d40)

    work page doi:10.3847/1538-4357/ab8d40 2020

  20. [24]

    Monthly Notices of the Royal Astronomical Society , keywords =

    Mehta T, Broomhall AM, Hayes LA. 2023 Prevalence of non-stationarity in quasi-periodic pulsations (QPPs) associated with M- and X-class solar flares.Mon. Not. R. Astron. Soc.523, 3689–3698. (10.1093/mnras/stad1619)

    work page doi:10.1093/mnras/stad1619 2023

  21. [25]

    2018 Modelling Quasi- Periodic Pulsations in Solar and Stellar Flares.Space Sci

    McLaughlin JA, Nakariakov VM, Dominique M, Jelínek P , Takasao S. 2018 Modelling Quasi- Periodic Pulsations in Solar and Stellar Flares.Space Sci. Rev.214, 45. (10.1007/s11214-018- 0478-5)

    work page doi:10.1007/s11214-018- 2018

  22. [26]

    2022 Statistical Properties of X-ray Flares in Gamma-Ray Bursts.Universe8, 358

    Shi YR, Ding XK, Zhu SY, Sun WP , Zhang FW. 2022 Statistical Properties of X-ray Flares in Gamma-Ray Bursts.Universe8, 358. (10.3390/universe8070358)

    work page doi:10.3390/universe8070358 2022

  23. [27]

    2024 Localising pulsations in the hard X-ray and microwave emission of an X-class flare.Astron

    Collier H, Hayes LA, Yu S, Battaglia AF, Ashfield W, Polito V , Harra LK, Krucker S. 2024 Localising pulsations in the hard X-ray and microwave emission of an X-class flare.Astron. Astrophys.684, A215. (10.1051/0004-6361/202348652)

    work page doi:10.1051/0004-6361/202348652 2024

  24. [29]

    2012 Modeling of Gyrosynchrotron Radio Emission Pulsations Produced by Magnetohydrodynamic Loop Oscillations in Solar Flares.Astrophys

    Mossessian G, Fleishman GD. 2012 Modeling of Gyrosynchrotron Radio Emission Pulsations Produced by Magnetohydrodynamic Loop Oscillations in Solar Flares.Astrophys. J.748, 140. (10.1088/0004-637X/748/2/140)

    work page doi:10.1088/0004-637x/748/2/140 2012

  25. [30]

    2022 Modulation of the solar microwave emission by sausage oscillations.Mon

    Kupriyanova EG, Kaltman TI, Kuznetsov AA. 2022 Modulation of the solar microwave emission by sausage oscillations.Mon. Not. R. Astron. Soc.516, 2292–2299. (10.1093/mnras/stac2386)

    work page doi:10.1093/mnras/stac2386 2022

  26. [31]

    B., et al

    Dolla L, Marqué C, Seaton DB, Van Doorsselaere T, Dominique M, Berghmans D, Cabanas C, De Groof A, Schmutz W, Verdini A, West MJ, Zender J, Zhukov AN. 2012 Time Delays in Quasi-periodic Pulsations Observed during the X2.2 Solar Flare on 2011 February 15. Astrophys. J. Lett.749, L16. (10.1088/2041-8205/749/1/L16)

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

  27. [32]

    G., Kashapova, L

    Kupriyanova EG, Kashapova LK, Van Doorsselaere T, Chowdhury P , Srivastava AK, Moon YJ. 2019 Quasi-periodic pulsations in a solar flare with an unusual phase shift.Mon. Not. R. Astron. Soc.483, 5499–5507. (10.1093/mnras/sty3480)

    work page doi:10.1093/mnras/sty3480 2019

  28. [33]

    2023 Quasi-Periodic Pulsations in an M-Class Solar Flare.Universe9,

    Xu J, Ning Z, Li D, Shi F. 2023 Quasi-Periodic Pulsations in an M-Class Solar Flare.Universe9,

    2023

  29. [34]

    (10.3390/universe9050215)

    work page doi:10.3390/universe9050215

  30. [35]

    2015 Multi- mode quasi-periodic pulsations in a solar flare.Astron

    Kolotkov DY, Nakariakov VM, Kupriyanova EG, Ratcliffe H, Shibasaki K. 2015 Multi- mode quasi-periodic pulsations in a solar flare.Astron. Astrophys.574, A53. (10.1051/0004- 6361/201424988)

    work page doi:10.1051/0004- 2015

  31. [36]

    2015 Study of multi-periodic coronal pulsations during an X-class solar flare.Advances in Space Research56, 2769–2778

    Chowdhury P , Srivastava AK, Dwivedi BN, Sych R, Moon YJ. 2015 Study of multi-periodic coronal pulsations during an X-class solar flare.Advances in Space Research56, 2769–2778. (10.1016/j.asr.2015.08.003)

    work page doi:10.1016/j.asr.2015.08.003 2015

  32. [37]

    2017 Detection and Interpretation of Long-lived X-Ray Quasi-periodic Pulsations in the X-class Solar Flare on 2013 May 14.Astrophys

    Dennis BR, Tolbert AK, Inglis A, Ireland J, Wang T, Holman GD, Hayes LA, Gallagher PT. 2017 Detection and Interpretation of Long-lived X-Ray Quasi-periodic Pulsations in the X-class Solar Flare on 2013 May 14.Astrophys. J.836, 84. (10.3847/1538-4357/836/1/84)

    work page doi:10.3847/1538-4357/836/1/84 2017

  33. [38]

    Lemen JR, Title AM, Akin DJ, Boerner PF, Chou C, Drake JF, Duncan DW, Edwards CG, Friedlaender FM, Heyman GF, Hurlburt NE, Katz NL, Kushner GD, Levay M, Lindgren RW, Mathur DP , McFeaters EL, Mitchell S, Rehse RA, Schrijver CJ, Springer LA, Stern RA, Tarbell 12royalsocietypublishing.org/journal/rsta Phil. Trans. R. Soc. A 0000000. . . . . . . . . . . . . ...

    work page doi:10.1007/s11207-011-9776-8 2012

  34. [39]

    D., Thompson, B

    Pesnell WD, Thompson BJ, Chamberlin PC. 2012 The Solar Dynamics Observatory (SDO).Sol. Phys.275, 3–15. (10.1007/s11207-011-9841-3)

    work page doi:10.1007/s11207-011-9841-3 2012

  35. [40]

    1998 Data Analysis with the SolarSoft System.Sol

    Freeland SL, Handy BN. 1998 Data Analysis with the SolarSoft System.Sol. Phys.182, 497–500. (10.1023/A:1005038224881)

    work page doi:10.1023/a:1005038224881 1998

  36. [41]

    2002 The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI).Sol

    Lin RP , Dennis BR, Hurford GJ, Smith DM, Zehnder A, Harvey PR, Curtis DW, Pankow D, Turin P , Bester M, et al.. 2002 The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI).Sol. Phys.210, 3–32. (10.1023/A:1022428818870)

    work page doi:10.1023/a:1022428818870 2002

  37. [42]

    2017 Direct Observation of Two-step Magnetic Reconnection in a Solar Flare.Astrophys

    Gou T, Veronig AM, Dickson EC, Hernandez-Perez A, Liu R. 2017 Direct Observation of Two-step Magnetic Reconnection in a Solar Flare.Astrophys. J. Lett.845, L1. (10.3847/2041- 8213/aa813d)

    work page doi:10.3847/2041- 2017

  38. [43]

    2010 SDO/AIA response to coronal hole, quiet Sun, active region, and flare plasma.Astron

    O’Dwyer B, Del Zanna G, Mason HE, Weber MA, Tripathi D. 2010 SDO/AIA response to coronal hole, quiet Sun, active region, and flare plasma.Astron. Astrophys.521, A21. (10.1051/0004-6361/201014872)

    work page doi:10.1051/0004-6361/201014872 2010

  39. [44]

    1964 Smoothing and differentiation of data by simplified least squares procedures.Analytical Chemistry36, 1627–1639

    Savitzky A, Golay MJE. 1964 Smoothing and differentiation of data by simplified least squares procedures.Analytical Chemistry36, 1627–1639. (10.1021/ac60214a047)

    work page doi:10.1021/ac60214a047 1964

  40. [45]

    2013 Evolution of the Source of Quasi- Periodic Microwave Pulsations in a Single Flaring Loop.Publ

    Kupriyanova EG, Melnikov VF, Shibasaki K. 2013 Evolution of the Source of Quasi- Periodic Microwave Pulsations in a Single Flaring Loop.Publ. Astron. Soc. Jpn65, S3. (10.1093/pasj/65.sp1.S3)

    work page doi:10.1093/pasj/65.sp1.s3 2013

  41. [46]

    arXiv , author =:1911.05217 , journal =

    Yuan D, Feng S, Li D, Ning Z, Tan B. 2019 A Compact Source for Quasi-periodic Pulsation in an M-class Solar Flare.Astrophys. J. Lett.886, L25. (10.3847/2041-8213/ab5648)

    work page doi:10.3847/2041-8213/ab5648 2019

  42. [47]

    2012 Evidence for Widespread Cooling in an Active Region Observed with the SDO Atmospheric Imaging Assembly.Astrophys

    Viall NM, Klimchuk JA. 2012 Evidence for Widespread Cooling in an Active Region Observed with the SDO Atmospheric Imaging Assembly.Astrophys. J.753, 35. (10.1088/0004- 637X/753/1/35)

    work page doi:10.1088/0004- 2012

  43. [48]

    2019 Understanding Heating in Active Region Cores through Machine Learning

    Barnes WT, Bradshaw SJ, Viall NM. 2019 Understanding Heating in Active Region Cores through Machine Learning. I. Numerical Modeling and Predicted Observables.Astrophys. J. 880, 56. (10.3847/1538-4357/ab290c)

    work page doi:10.3847/1538-4357/ab290c 2019

  44. [49]

    1994 Some Implications of the Nanoflare Concept.Astrophys

    Cargill PJ. 1994 Some Implications of the Nanoflare Concept.Astrophys. J.422, 381. (10.1086/173733)

    work page doi:10.1086/173733 1994

  45. [50]

    2005Physics of the Solar Corona

    Aschwanden MJ. 2005Physics of the Solar Corona. An Introduction with Problems and Solutions (2nd edition). (10.1007/3-540-30766-4)

    work page doi:10.1007/3-540-30766-4

  46. [51]

    2011 SDO AIA and Hinode EIS observations of “warm” loops.Astron

    Del Zanna G, O’Dwyer B, Mason HE. 2011 SDO AIA and Hinode EIS observations of “warm” loops.Astron. Astrophys.535, A46. (10.1051/0004-6361/201117470)

    work page doi:10.1051/0004-6361/201117470 2011

  47. [52]

    2009 Relationship between wave processes in sunspots and quasi-periodic pulsations in active region flares.Astron

    Sych R, Nakariakov VM, Karlicky M, Anfinogentov S. 2009 Relationship between wave processes in sunspots and quasi-periodic pulsations in active region flares.Astron. Astrophys. 505, 791–799. (10.1051/0004-6361/200912132)

    work page doi:10.1051/0004-6361/200912132 2009

  48. [53]

    2014 Oscillations in a Sunspot with Light Bridges.Astrophys

    Yuan D, Nakariakov VM, Huang Z, Li B, Su J, Yan Y, Tan B. 2014 Oscillations in a Sunspot with Light Bridges.Astrophys. J.792, 41. (10.1088/0004-637X/792/1/41)

    work page doi:10.1088/0004-637x/792/1/41 2014

  49. [54]

    Frontiers in Astronomy and Space Sciences , keywords =

    Li D, Shi F, Zhao H, Xiong S, Song L, Peng W, Li X, Chen W, Ning Z. 2022 Flare quasi-periodic pulsation associated with recurrent jets.Frontiers in Astronomy and Space Sciences9, 1032099. (10.3389/fspas.2022.1032099)

    work page doi:10.3389/fspas.2022.1032099 2022

  50. [55]

    Vallisneriet al.(NANOGrav), (2020), 10.3847/1538- 4357/ab7b67, arXiv:2001.00595 [astro-ph.HE]

    Mishra SK, Sangal K, Kayshap P , Jelínek P , Srivastava AK, Rajaguru SP . 2023 Origin of Quasi- periodic Pulsation at the Base of a Kink-unstable Jet.Astrophys. J.945, 113. (10.3847/1538- 4357/acb058)

    work page doi:10.3847/1538- 2023

  51. [56]

    2026 Spatial variation of energy transport mechanisms within solar flare ribbons.Nature Astronomy10, 202–213

    Kerr GS, Krucker S, Allred JC, Rodríguez-Gómez JM, Inglis AR, Ryan DF, Hayes LA, Milligan RO, Kowalski AF, Plowman JE, Young PR, Kucera TA, Brosius JW. 2026 Spatial variation of energy transport mechanisms within solar flare ribbons.Nature Astronomy10, 202–213. (10.1038/s41550-025-02747-9)

    work page doi:10.1038/s41550-025-02747-9 2026

  52. [57]

    2016 Forward modelling of optically thin coronal plasma with the FoMo tool.Frontiers in Astronomy and Space Sciences3,

    Van Doorsselaere T, Antolin P , Yuan D, Reznikova V , Magyar N. 2016 Forward modelling of optically thin coronal plasma with the FoMo tool.Frontiers in Astronomy and Space Sciences3,

    2016

  53. [58]

    (10.3389/fspas.2016.00004)

    work page doi:10.3389/fspas.2016.00004 2016

  54. [59]

    arXiv , author =:2110.14257 , journal =

    Fyfe LE, Howson TA, De Moortel I. 2021 Forward modelling of heating within a coronal arcade.Astron. Astrophys.656, A120. (10.1051/0004-6361/202142028)

    work page doi:10.1051/0004-6361/202142028 2021

  55. [60]

    2019 Desaturating SDO/AIA Observations of Solar Flaring Storms.Astrophys

    Guastavino S, Piana M, Massone AM, Schwartz R, Benvenuto F. 2019 Desaturating SDO/AIA Observations of Solar Flaring Storms.Astrophys. J.882, 109. (10.3847/1538-4357/ab35d8) 13royalsocietypublishing.org/journal/rsta Phil. Trans. R. Soc. A 0000000

    work page doi:10.3847/1538-4357/ab35d8 2019

  56. [61]

    2021 Image Desaturation for SDO/AIA Using Deep Learning.Sol

    Yu X, Xu L, Yan Y. 2021 Image Desaturation for SDO/AIA Using Deep Learning.Sol. Phys. 296, 56. (10.1007/s11207-021-01808-2)

    work page doi:10.1007/s11207-021-01808-2 2021