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arxiv: 2605.12060 · v1 · submitted 2026-05-12 · 🌌 astro-ph.SR

Recognition: no theorem link

Effect of Solar Flares on Decayless Kink Oscillations in Nearby Coronal Loops

Zhiyi Li , Valery M. Nakariakov , Ding Yuan , Song Feng
Authors on Pith no claims yet

Pith reviewed 2026-05-13 04:50 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar flaresdecayless kink oscillationscoronal loopssolar coronaSDO/AIAmotion magnificationoscillation amplitude
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The pith

Decayless kink oscillations in coronal loops show little amplitude change in response to nearby solar flares of any class.

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

The study analyzes 130 solar flares from B to X class that lack quasi-periodic pulsations and checks for effects on decayless kink oscillations in nearby coronal loops observed in SDO/AIA 171 angstrom images. Low-amplitude oscillations with periods of 122 to 268 seconds were detected in every loop before, during, and after the flares using a motion magnification method. Average amplitudes remained essentially unchanged across all events, with only minor variations in some cases, such as slight increases more common in M-class flares. This indicates that flare-related mechanisms like blast waves or reconnection inflows do not substantially alter the energy maintaining the oscillations. A reader would care because the result points to a steady, flare-independent driver for these ubiquitous coronal motions.

Core claim

The amplitude of decayless kink oscillations does not undergo a major change in response to nearby flares, especially for less powerful classes, suggesting that flare-related processes such as blast waves and reconnection inflows have little effect on the energy supply to oscillating loops.

What carries the argument

Fractional Anisotropy-based Video Motion Magnification technique applied to SDO/AIA 171 angstrom images, used to detect and quantify low-amplitude decayless kink oscillations before, during, and after each flare.

Load-bearing premise

The motion magnification technique accurately measures the small oscillation amplitudes without systematic bias, and the chosen loops are representative and free from confounding influences.

What would settle it

Observation of statistically significant amplitude increases or decreases in a larger sample of X-class flares where blast-wave impact on the loops can be confirmed independently.

Figures

Figures reproduced from arXiv: 2605.12060 by Ding Yuan, Song Feng, Valery M. Nakariakov, Zhiyi Li.

Figure 1
Figure 1. Figure 1: C8.5-class flare event on January 28, 2014. (a) Target observation region [-1180, -880, -400, -100] (arcsec), with the location of a coronal loop of interest marked by the red dashed line, and the slice used in the construction of the time–distance map marked by the red solid line. The red solid dots mark the positions of the flare centre. (b) Raw coronal loop time–distance map. (c) Coronal loop time–dista… view at source ↗
Figure 2
Figure 2. Figure 2: M3.5-class flare event on February 24, 2011. Target observation region: [-1160, -860, 120, 420] (arcsec). Other symbols are the same as in Fig.1 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: M1.8-class flare event on September 21, 2011. Target observation region: [-1130, -830, 200, 500] (arcsec). Other symbols are the same as in Fig.1. 3.2. Parameters of Decayless Kink Oscillations [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: shows the statistical properties of the detected oscillations. The amplitudes range from 0.023 Mm to 0.111 Mm and exhibit an approximately normal distribution. The mean amplitude is 0.052 ± 0.014 Mm (with errors estimated as the standard deviation), and the median is 0.051 Mm. Approximately 68% of the events have amplitudes concentrated in the 0.03–0.07 Mm range. These amplitude values are lower than the t… view at source ↗
Figure 5
Figure 5. Figure 5: Amplitude distributions for pre-flare, during-flare, and post-flare phases [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Relative changes in the amplitudes of decayless kink oscillations during flares in comparison with the pre-flare value. B (N=52) C (N=44) M (N=28) X (N=6) Flare class 0% 20% 40% 60% 80% 100% Proportion (%) 76.9% 11.5% 11.5% 61.5% 25.0% 13.5% 59.1% 22.7% 18.2% 61.4% 27.3% 11.4% 64.3% 28.6% 7.1% 71.4% 21.4% 7.1% 33.3% 16.7% 50.0% 66.7% 16.7% 16.7% Constant Increase Decrease During-flare Post-flare [PITH_FUL… view at source ↗
Figure 7
Figure 7. Figure 7: Relative changes in the kink oscillation amplitude during and after a flare in comparison with the pre-flare value for the B, C, M, and X-class flares. The increase or decrease corresponds to the change by more than 10%. The number of analysed events, N, is shown in the bottom [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: shows the distribution of the events in which the amplitude changes by more than 20% with the distance between the centre of the oscillating loop and the flare site, separately for different flare classes. The events were divided into five groups based on projected distance: <60 Mm, 60—80 Mm, 80—100 Mm, 100—120 Mm, and >120 Mm. The numbers of events with modest amplitude changes (> 20%) in each group are 3… view at source ↗
read the original abstract

We present a statistical study of 130 solar flares (B to X class) that lack soft X-ray quasi-periodic pulsations and show no kink oscillations of nearby coronal loops visible in SDO/AIA 171~\AA~images. The aim is to investigate whether decayless kink oscillations of coronal loops respond to nearby flaring activity. Using the Fractional Anisotropy-based Video Motion Magnification technique, we detected low-amplitude decayless oscillations in all 130 loops before, during, and after each flare, confirming their ubiquitous nature. Oscillation periods are found to range from 122~s to 268~s, and the projected displacement amplitudes are 0.023--0.111~Mm. No amplitude--period correlation is found. For each event, we estimated the amplitude before, during, and after the flare. Across all flare classes, the average amplitude remains unchanged. However, in some specific cases, the oscillation amplitude may exhibit minor changes. For B-, C-, and M-class flares, the fraction of events with an amplitude change exceeding 10% is approximately 23%, 41%, and 36%, respectively. In M-class flares, such minor amplitude increases occur four times more often than decreases; in X-class flares (only six events), decreases dominate by a factor of three. The fraction of events that exhibit an increase in the amplitude of more than 20% appears to be highest when the loop centre is located at a distance of 100--120~Mm from the flare site, reaching 33% (6 out of 18 events). Overall, the amplitude of decayless kink oscillations does not undergo a major change in response to nearby flares, especially for less powerful classes, suggesting that flare-related processes such as blast waves and reconnection inflows have little effect on the energy supply to oscillating loops.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript presents a statistical study of 130 solar flares (B to X class) lacking soft X-ray QPPs and visible kink oscillations in SDO/AIA 171 Å images. Using the Fractional Anisotropy-based Video Motion Magnification technique, the authors detect low-amplitude decayless kink oscillations in all 130 nearby loops before, during, and after each flare. They report periods of 122–268 s and projected amplitudes of 0.023–0.111 Mm with no amplitude–period correlation, finding that average amplitudes remain unchanged across flare classes while only modest fractions of events show >10% or >20% changes, with some distance dependence; this leads to the conclusion that flare-related processes have little effect on the energy supply to the oscillating loops.

Significance. If the amplitude measurements are shown to be reliable, the large sample of 130 events provides statistically meaningful evidence that decayless kink oscillations are largely unaffected by nearby flares of B–M class, reinforcing their ubiquitous nature and independence from flare-driven energy inputs such as blast waves. This would be a useful observational constraint on coronal loop dynamics and wave excitation mechanisms. The small X-class subsample limits broader claims, but the overall dataset strengthens the case for minimal flare influence on these oscillations.

major comments (3)
  1. [Methods] The central claim that amplitudes 'do not undergo a major change' and that only modest fractions exceed 10% or 20% thresholds rests on amplitude measurements extracted via the Fractional Anisotropy-based Video Motion Magnification technique, yet the manuscript provides no error budget, synthetic-injection recovery tests, or calibration of the method's precision for sub-resolution displacements (0.023–0.111 Mm). Without this, the reported change fractions (e.g., 23% for B-class, 41% for C-class) and the 33% increase in the 100–120 Mm distance bin cannot be distinguished from measurement scatter or intrinsic variability.
  2. [Results] Only six X-class events are analyzed, yet the abstract states that 'decreases dominate by a factor of three' in this class; this sample size is too small for robust comparison with the larger B/C/M subsamples and undermines any class-dependent conclusions about amplitude response.
  3. [Results] No statistical tests, p-values, or uncertainty estimates are reported for the 'no amplitude–period correlation' statement or for the significance of the before/during/after amplitude comparisons, making it impossible to evaluate whether the observed minor changes are distinguishable from noise.
minor comments (2)
  1. [Abstract] The abstract mentions the period range and amplitude range but does not specify how periods and amplitudes were fitted or what functional form was assumed for the oscillations.
  2. Loop selection criteria and any checks that the chosen loops are unaffected by other variables (e.g., nearby non-flaring activity) are not described in sufficient detail to assess sample representativeness.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have identified important areas where the manuscript can be strengthened. We address each major comment below and will revise the paper to incorporate additional analysis and qualifications as appropriate.

read point-by-point responses

  1. Referee: [Methods] The central claim that amplitudes 'do not undergo a major change' and that only modest fractions exceed 10% or 20% thresholds rests on amplitude measurements extracted via the Fractional Anisotropy-based Video Motion Magnification technique, yet the manuscript provides no error budget, synthetic-injection recovery tests, or calibration of the method's precision for sub-resolution displacements (0.023–0.111 Mm). Without this, the reported change fractions (e.g., 23% for B-class, 41% for C-class) and the 33% increase in the 100–120 Mm distance bin cannot be distinguished from measurement scatter or intrinsic variability.

    Authors: We acknowledge that the manuscript does not present a formal error budget or synthetic recovery tests for the sub-resolution amplitude measurements. Although the Fractional Anisotropy-based Video Motion Magnification technique has been validated in earlier studies of decayless oscillations, we agree that demonstrating its precision specifically for the reported displacement range is necessary to support the change-fraction statistics. In the revised manuscript we will add an error analysis section that includes (i) per-event amplitude uncertainties derived from the AIA signal-to-noise ratio and (ii) synthetic displacement-injection tests performed on representative loop data to quantify recovery accuracy and scatter. These additions will allow direct comparison of observed amplitude variations against measurement uncertainties. revision: yes

  2. Referee: [Results] Only six X-class events are analyzed, yet the abstract states that 'decreases dominate by a factor of three' in this class; this sample size is too small for robust comparison with the larger B/C/M subsamples and undermines any class-dependent conclusions about amplitude response.

    Authors: We concur that the X-class subsample is limited to six events and that the descriptive statement in the abstract therefore cannot support robust class-dependent conclusions. The observation that decreases outnumber increases by a factor of three is simply a count within this small sample and was not presented as statistically significant. In the revision we will (i) qualify the abstract wording to read “in the limited sample of six X-class flares, amplitude decreases were observed more frequently than increases” and (ii) add an explicit discussion of the small-sample limitation in both the results and conclusions sections, thereby avoiding over-interpretation. revision: yes

  3. Referee: [Results] No statistical tests, p-values, or uncertainty estimates are reported for the 'no amplitude–period correlation' statement or for the significance of the before/during/after amplitude comparisons, making it impossible to evaluate whether the observed minor changes are distinguishable from noise.

    Authors: The original manuscript reported the absence of an amplitude–period correlation and the before/during/after amplitude comparisons without accompanying statistical tests or uncertainties. To rectify this, the revised version will include (i) Spearman rank correlation coefficients together with p-values for the amplitude–period relation across the full sample and per flare class, and (ii) mean (or median) amplitudes with standard errors (or interquartile ranges) for the before, during, and after intervals, accompanied by paired statistical tests (e.g., Wilcoxon signed-rank or paired t-tests) to assess the significance of any differences. These quantitative measures will be added to the results section and will enable readers to judge whether the reported minor changes exceed expected variability. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational statistical analysis with direct amplitude measurements

full rationale

The paper conducts a statistical study of 130 flare events, applying an established motion-magnification technique to measure projected displacement amplitudes (0.023–0.111 Mm) in coronal loops before, during, and after each flare. Periods and amplitude changes are computed directly from the processed image sequences; average amplitudes are compared across flare classes, and fractions exceeding 10% or 20% change are tallied from the same measurements. No equations, model derivations, fitted parameters presented as predictions, or self-referential steps appear in the reported chain. The central claim—that amplitudes show no major change—is an empirical summary of the observed values, not a reduction to inputs by construction. Any cited prior work on the magnification method or decayless oscillations supplies independent methodological context rather than a load-bearing premise that collapses the result.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on observational measurements and the assumption that the motion magnification technique faithfully captures true amplitudes; no free parameters, new entities, or ad hoc axioms are introduced in the abstract.

axioms (1)
  • domain assumption Detected oscillations are decayless kink oscillations identifiable by their periods and amplitudes in 171 Å images
    Invoked when applying the technique to all 130 loops and classifying them as decayless kink oscillations.

pith-pipeline@v0.9.0 · 5651 in / 1195 out tokens · 48238 ms · 2026-05-13T04:50:11.946407+00:00 · methodology

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Reference graph

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