Solar Physics最新文献

{"title":"The EUV Late-Phase: Statistical Results from 15 Years of Solar Dynamics Observatory Observations","authors":"Harry J. Greatorex,&nbsp;Aisling N. O’Hare,&nbsp;Susanna Bekker,&nbsp;Ryan J. Campbell,&nbsp;Daniel C. Keane,&nbsp;Ryan O. Milligan","doi":"10.1007/s11207-026-02673-7","DOIUrl":"10.1007/s11207-026-02673-7","url":null,"abstract":"<div><p>Since its launch in 2010, the Solar Dynamics Observatory (SDO) has provided continuous, high-cadence, multi-wavelength observations of the Sun, capturing thousands of solar flares and offering new insights into coronal dynamics. Among the discoveries enabled by SDO is the EUV late-phase (ELP), characterised by a secondary enhancement in warm coronal emission occurring tens of minutes after the main flare. While recent work has demonstrated the relevance of the ELP for space weather, the statistical behaviours and physical origins are not fully understood. Here, we present the most comprehensive statistical analysis of the ELP to date, based on 15-years of Fe <span>xvi</span> (335 Å) observations from the Atmospheric Imaging Assembly onboard SDO (SDO/AIA). From a sample of 5335 isolated flares between 2010 and 2025, we identify and validate 467 ELP events. The overall ELP occurrence rate was found to be 9%, with no significant dependence on the solar cycle and only a modest enhancement in the low-mid M-class range. The ELP typically exhibited an onset delay of 19 minutes, a peak-to-peak delay of 88 minutes, and a duration of 93 minutes. Strong correlations were found between ELP rise and decay rates (<span>(rho =0.76)</span>), and between flare and ELP impulsivity (<span>(rho =0.61)</span>). However, a comprehensive pairwise analysis revealed no significant correlation between the flare and ELP phases (<span>(|rho |&lt;0.3)</span>). A Principal Component Analysis of flare and ELP properties identified several semi-independent axes of variability, broadly associated with late-phase temporal scale, impulsive heating characteristics, and the relative prominence of flare and late-phase intensity measures. These results highlight the continuing importance of SDO’s long-term, high-resolution observations for uncovering new aspects of solar flare evolution and improving understanding of the Sun-Earth connection.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02673-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148061075","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Measurements on the Kinetic Origin of Streamer Dynamics","authors":"F. S. Mozer,&nbsp;K.-E. Choi,&nbsp;R. Sydora,&nbsp;A. Voshchepynets","doi":"10.1007/s11207-026-02675-5","DOIUrl":"10.1007/s11207-026-02675-5","url":null,"abstract":"<div><p>A major goal of solar physics is understanding the transition of the medium from the closed-loop magnetic configuration of the corona to the open structure of the heliospheric current sheet. The evolution of solar wind streamers, an essential component of this transition, has been observed in-situ for the first time by measuring a pass through a streamer stalk at 11.7 solar radii. A plasma rest frame DC electric field, reaching an amplitude of 400 mV/m, was observed as the magnetic field changed from +1100 nT to -1100 nT. This electric field violates the frozen in condition so it must be understood via the non-MHD Hall term of the Generalized Ohm’s Law. Two plasma regimes containing the large electric field were observed. In the first regime, the magnetic field was large, the ion beta was small (∼0.1), the ratio of the ion skin depth to ion gyroradius was large (&gt;10), and the current of ∼0.3 mA/m² was carried by electrons. In the second regime, the magnetic field was small, the ion beta was large (∼10), the ion skin depth was equal to the ion gyroradius, and the ∼10 mA/m² current was carried by the ions. Also, measurements during 15 such crossings showed that the plasma flow speed inside the current sheets exceeded that outside six times and the 326 km/s average speed inside the current sheets exceeded the 266 km/s outside. Such findings challenge the traditional consensus that streamers are the source of the “slow” solar wind.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02675-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148061074","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Solar Cycle Variation of Sustained Gamma Ray Emission from the Sun","authors":"Nat Gopalswamy,&nbsp;Pertti Mäkelä,&nbsp;Seiji Yashiro,&nbsp;Sachiko Akiyama,&nbsp;Hong Xie,&nbsp;G. Sindhuja","doi":"10.1007/s11207-026-02667-5","DOIUrl":"10.1007/s11207-026-02667-5","url":null,"abstract":"<div><p>We investigated the occurrence rate of the sustained gamma ray emission (SGRE) events from the Sun using data obtained by the Large Area Telescope (LAT) on board the Fermi satellite since its launch in 2008. The data cover the whole of solar cycle (SC) 24 and the rising and maximum phases of SC 25. One of the challenges was to estimate the number of SGRE events in SC 25 because of the malfunction of a solar array drive assembly starting in March 2018 that resulted in a large reduction in solar coverage (LAT gap). This is likely the reason for the small number (16) of SGRE events observed during the first 61 months of SC 25, whereas 27 events were observed during the weaker SC 24 over the corresponding epoch. Over the first 61 months, the average sunspot number (SSN) increased from 56.9 in SC 24 to 79.0 in SC 25. Other energetic events closely related to SGREs, viz., fast and wide (FW) coronal mass ejections (CMEs) and decameter-hectometric (DH) type II bursts also increased significantly in SC 25 by 29% and 33%, respectively when normalized to SSN. Therefore, the increase in solar activity should result in a higher number of SGREs in SC 25. We estimated the number of SGREs in SC 25 using three methods. (i) If the SGRE number varies commensurate with SSN, we should have 38 (27×1.39) SGRE events in SC 25 based on the 27 events in SC 24. However, FW CMEs and DH type II bursts in SC 25 were overabundant by 29% and 33%, so the number SGRE events should be accordingly higher: 48 (27×1.39×1.29 from FW CMEs) and 50 (27×1.39×1.33). (ii) In SC 24, ≈18% of FW CMEs and 27% of DH type II bursts were associated with SGRE events. If the same association rate prevails in SC 25, we should have 48 and 49 SGRE events in this cycle. (iii) Since SGRE events are invariably associated with &gt; 100 keV hard X-ray (HXR) bursts, we identified DH type II bursts associated with &gt; 100 keV HXR bursts from Fermi’s Gamma-ray Burst Monitor (GBM) during LAT data gaps. Based on our finding that SGRE events in SCs 24 and 25 were all associated with HXR bursts of duration ≳ 5 min, we found only 27 of the 79 LAT-gap type II bursts had &gt; 100 keV HXR bursts with duration ≳5 min. These DH type II bursts are likely to indicate SGRE events, bringing the total number to 43 (16 observed + 27 inferred). Thus, the three methods provide similar estimates of the number of SGRE events in SC 25. We, therefore, conclude that SC 25 is stronger than SC 24 based on the estimated number SGRE events. Other energetic phenomena such as halo CMEs, ground level enhancement (GLE) events, and intense geomagnetic storms are also consistent with a stronger SC 25.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02667-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148061065","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Large-Scale Solar Magnetic Fields Observed with Full-Disk Telescopes at the Sayan and Baikal Observatories: Similarities, Differences, and Application to the Space-Weather Issues","authors":"M. L. Demidov,&nbsp;R. V. Pavlova,&nbsp;V. S. Peshcherov","doi":"10.1007/s11207-026-02683-5","DOIUrl":"10.1007/s11207-026-02683-5","url":null,"abstract":"<div><p>Cross-comparison of solar magnetic fields measurements made with different telescopes, or with different spectral lines on the same instrument, is important and a traditional task of solar physics. This is crucial from the methodical point of view since allows to understand which device properties are responsible for the differences, if they have a place to be. In some studies this is also useful as a tool for diagnostics of the solar magnetic fields hidden spatial structure, the thin kG flux tubes. Most often the measurements at active regions are used for these purposes. But sometimes observations of the large-scale magnetic fields (LSMF) are involved for such analysis as well. The second case is especially important for some space-weather issues because the LSMF are responsible for the formation of the helio-magnetosphere and solar-wind properties.</p><p>Here we at the first time make a cross-calibration of LSMF observations made with two full-disk instruments, called Solar Telescopes for Operative Predictions (STOP), located at the <i>Sayan Solar</i> (SSO) and <i>Baikal Astrophysical</i> (BAO) observatories. These observatories are situated rather close to each other and sometimes it is possible to observe the Sun practically simultaneously. Despite the common name (caused by the main scientific goals) these telescopes have significant differences and it is interesting to examine how these differences affect on the measured magnetic-field strengths.</p><p>Data sets from both observatories are compared also with <i>Wilcox Solar Observatory</i> (WSO) measurements. As an additional scientific output of this study, SSO, BAO, and WSO measurements are used for calculations of solar-wind speed.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148061066","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigating Pre-Flare Signatures in Spectroscopic Observations of an X9-Class Solar Flare","authors":"Louis Seyfritz,&nbsp;Maria Kazachenko,&nbsp;Ryan French","doi":"10.1007/s11207-026-02674-6","DOIUrl":"10.1007/s11207-026-02674-6","url":null,"abstract":"<div><p>On October 3rd, 2024, the Sun emitted an X9.0-class flare from active region NOAA 13842. The event was recorded by multiple space-based instruments, beginning hours before the eruption, granting a unique opportunity to provide insight into the flare’s pre-flare phase. In this study, we employ analysis of Interface Region Imaging Spectrograph (IRIS) spectroscopic data to investigate pre-flaring phenomena associated with this flare. We present time-series and wavelet analysis of non-thermal velocity, Doppler velocity, and line intensity quantities of the IRIS Si IV 1403 Å line. We find two ranges of periodic oscillations during the pre-flare phase: ∼ 7 – 10 min and ∼ 18 – 21 min oscillations, with local enhancements occurring near the polarity inversion line. We also find a steady rise in Si IV line parameters beginning 3 hours before the flare in the same region, transitioning into strong non-thermal velocities and blueshifts <span>({sim},15)</span> minutes before onset. These findings are consistent with a slow destabilization of the coronal magnetic field, possibly driven by the gradual activation of a flux rope, followed by a rapid shift to intense reconnection activity leading to flare onset.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02674-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148173501","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Determination of 3He-Rich Periods Measured by the Suprathermal Ion Telescope on STEREO-A During Solar Cycle 24","authors":"Marlon Köberle,&nbsp;Lars Berger,&nbsp;Radoslav Bučík,&nbsp;Bernd Heber,&nbsp;Glenn M. Mason,&nbsp;Linghua Wang","doi":"10.1007/s11207-026-02668-4","DOIUrl":"10.1007/s11207-026-02668-4","url":null,"abstract":"<div><p>³He-rich solar energetic particles (SEP) events are characterized by a peculiar elemental composition with rare species like ³He or ultra-heavy ions tremendously enhanced over the solar system abundances. We report on ³He-rich SEP periods measured by the Suprathermal Ion Telescope (SIT) on board the Solar Terrestrial Relations Observatory Ahead (STEREO-A) beginning in 2007 until 2020, covering the whole Solar Cycle (SC) 24.</p><p>The mass resolution capabilities of the SIT do not allow to easily distinguish between ³He and ⁴He especially in cases of a low ³He to ⁴He ratio. Therefore, we developed a data-driven detection algorithm to find time periods during which a ³He enhancement can be statistically determined.</p><p>With this method we were able to identify a total of 144 periods, which likely include all periods in SC 24, that can be resolved by the SIT. We lay a special emphasis on the quantification of ³He and ⁴He. As a result, we present ³He and ⁴He fluences as well as ³He/⁴He fluence ratios for the 144 periods in 6 energy channels in the range from 160 to 1280 keV nucleon⁻¹.</p><p>The ³He fluence distributions show mean (and median) values decreasing with increasing energy, ranging from <span>(5.84cdot 10^{4})</span> to <span>(0.57cdot 10^{4})</span> (and <span>(1.77cdot 10^{4})</span> to <span>(0.22cdot 10^{4})</span>) particles/(cm² srMeV nucleon⁻¹).</p><p>The ³He/⁴He fluence ratios show a clear tendency to increase with increasing energies, with means ranging between 0.34 at 193 keV nucleon⁻¹ and 1.09 at the 772 keV nucleon⁻¹ channel, reaching an apparent plateau above 546 keV nucleon⁻¹.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02668-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148009703","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Development of TSI Composites Using Unified Uncertainty Estimation Validated by Bland-Altman Analysis","authors":"J. M. Aclin Merisha,&nbsp;A. Iren Sobia","doi":"10.1007/s11207-026-02669-3","DOIUrl":"10.1007/s11207-026-02669-3","url":null,"abstract":"<div><p>Assessment of long-term Total Solar Irradiance (TSI) variability is essential for understanding solar forcing of the Earth system. In this study, two new TSI composites are created from satellite observations of VIRGO/PMO6Va, ACRIM-II, SORCE/TIM, TSIS/TIM and TCTE/TIM by incorporating time-dependent and instrument-specific uncertainty estimates. The square root of sunspot number (SSN) and F10.7 index were individually used as time- dependent solar proxies for Composite-1 and Composite-2 respectively. The composites of selected individual TSI datasets were merged by the inverse-variance weighting method. The uncertainty values for both composites largely fall within the 2<span>(sigma )</span> range of approximately 0 – 0.5 <span>(mathrm{W} /mathrm{m}^{2})</span>. Their interchangeability with original satellite observations was confirmed by Bland-Altman analysis. When compared with VIRGO, 96.52% of the data points fall within the 95% limits of agreement, which is consistent with the expected coverage of mean ± 1.96<span>(sigma )</span>. The evidence of solar activity in TSI composites was validated by Magnitude Squared Coherence analysis for short periodicities less than 27d quasi-solar rotational periods and Power Spectrum Density analysis for long periodicities such as the Schwabe cycle, resulting in 7d, 9d, 27d and 11-year periodicities and annual periodicities related to orbital or instrumental effects.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148009498","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigating the Relationship Between Physical Properties and Spatial Irregularities at Coronal Hole Boundaries","authors":"Nawin Ngampoopun,&nbsp;David M. Long,&nbsp;Lucie M. Green,&nbsp;Stephanie L. Yardley,&nbsp;Alexander W. James,&nbsp;Emily I. Mason,&nbsp;Stephan G. Heinemann,&nbsp;Vadim M. Uritsky","doi":"10.1007/s11207-026-02672-8","DOIUrl":"10.1007/s11207-026-02672-8","url":null,"abstract":"<div><p>Coronal hole boundaries are the interfaces between closed and open magnetic field regions in the solar atmosphere. Many fundamental processes take place at these regions, including magnetic reconnection that is responsible for solar wind release and restructuring of the solar magnetic field. In this paper, we present a case study in which we investigate the physical properties of the boundary of a large low-latitude coronal hole. Differential Emission Measure analysis is used to derive the plasma properties of these regions. We also apply correlation dimension mapping analysis to measure the irregularities of the coronal hole boundary. We find that the leading boundary of this coronal hole has a slightly higher average plasma temperature, is associated with a stronger and more unipolar magnetic field, and has a smoother boundary line than the trailing counterpart. These differences are hypothesised to be direct consequences of the local magnetic field configurations of the coronal hole boundary: the leading boundary corresponds to large, well-organised coronal loops, and the trailing boundary corresponds to more dispersed, randomly orientated small magnetic bipoles. Hence, we suggest that the surrounding magnetic field structure and the nature of magnetic reconnection influence the properties of coronal hole boundaries.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02672-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148009525","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Deep Learning-Enabled Prediction of Geoeffective CMEs Using SOHO and SDO Observations","authors":"Zhaoxin Yan,&nbsp;Jason T. L. Wang,&nbsp;Haimin Wang,&nbsp;Harim Lee,&nbsp;Ju Jing,&nbsp;Yan Xu,&nbsp;Chunhui Xu,&nbsp;Vasyl Yurchyshyn","doi":"10.1007/s11207-026-02665-7","DOIUrl":"10.1007/s11207-026-02665-7","url":null,"abstract":"<div><p>Understanding and forecasting the geoeffectiveness of a coronal mass ejection (CME) is crucial for protecting infrastructure in the near-Earth space environment and on Earth. In this study, we present a novel fusion model to forecast the geoeffectiveness of CME events. Our model combines convolutional neural networks for feature learning and a prediction network for feature fusion and event classification. The model is trained by observations from instruments including the Large Angle Spectroscopic Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). The trained model is then used to predict whether an Earth-reaching CME will cause a geomagnetic storm and/or the probability that the CME will cause such a storm. Experimental results based on a five-fold cross validation scheme demonstrate the good performance of our fusion model, achieving a mean true skill statistic (TSS) score of 0.703 when the model is used as a deterministic prediction tool, and a mean Brier score of 0.095 when the model is used as a probabilistic forecasting tool, where a TSS score of 1 or a Brier score of 0 indicates perfect performance. This work contributes to forecasting the causal relationship between Earth-directed CMEs and geomagnetic storms in solar-terrestrial interactions.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02665-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148009273","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Quasi-Periodic Pulsations and Coronal Loops Oscillations in an M-Class Solar Flare","authors":"Yijie Han,&nbsp;Zongjun Ning,&nbsp;Dong Li,&nbsp;Yuzhi Yang,&nbsp;Xiaoyu Tang,&nbsp;Yuxiang Song,&nbsp;Guotianci Xu,&nbsp;Mingbao Gao,&nbsp;Kangyi Li,&nbsp;Yu Huang","doi":"10.1007/s11207-026-02663-9","DOIUrl":"10.1007/s11207-026-02663-9","url":null,"abstract":"<div><p>We explore the oscillations during an M2.3 class solar flare on 2023 December 14, including quasi-periodic pulsations (QPPs) in the light curves and displacement oscillations in the nearby coronal loops, which gives us a chance to investigate whether a physical connection exists between these two phenomena during solar flares. Using the Bayesian-based Markov Chain Monte Carlo (MCMC) and wavelet analysis methods, QPPs are identified in the soft X-ray (SXR), hard X-ray (HXR), and extreme ultraviolet (EUV) light curves. These have a period of around one minute (58 - 72 s). High correlations are found between SXR and HXR QPPs indicating that they could be associated with a periodical injection of non-thermal electrons. However, we do not find a time delay between SXR and HXR QPPs at the time resolution of 12 s of the data used. Meanwhile, after the flare maximum, two coronal loops rooted in the flare region display expansions and “decayless” oscillations with periods of 3.6 min and 8.2 min until the flare ending. Our observations suggest that the loop oscillations are most likely standing kink mode waves. The magnetic field strength in the loops is estimated to be 16 G using coronal seismology. We do not find observational evidences showing a physical relation between QPPs and loop oscillations in this event.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02663-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148009450","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}