Solar Physics最新文献

Sunspot Observations in 1684 – 1702: John Flamsteed and Philippe de La Hire 1684 - 1702年的太阳黑子观测：约翰·弗兰斯蒂德和菲利普·德·拉希尔

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-10-01 DOI: 10.1007/s11207-025-02544-7

Nadezhda Zolotova, Mikhail Vokhmyanin

引用次数: 0

Quantifying Chromosphere Response to Flare Energy Release Using AIA Observations in 1600 Å and 304 Å Passbands 利用AIA观测在1600 Å和304 Å波段量化耀斑能量释放的色球响应

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-30 DOI: 10.1007/s11207-025-02550-9

Jiong Qiu, Rhiannon Fleming

{"title":"Quantifying Chromosphere Response to Flare Energy Release Using AIA Observations in 1600 Å and 304 Å Passbands","authors":"Jiong Qiu, Rhiannon Fleming","doi":"10.1007/s11207-025-02550-9","DOIUrl":"10.1007/s11207-025-02550-9","url":null,"abstract":"<div><p>Imaging observations of the solar lower atmosphere by the Atmospheric Imaging Assembly (AIA) have been mostly used as the context, and their quantitative information has been much less explored. The chromosphere responds rapidly to energy release by magnetic reconnection during flares. Furthermore, a flare is a collection of multiple energy release events that can be identified in spatially resolved chromosphere observations. In this paper, we conduct a statistical and semi-quantitative study of the relative photometry in the UV 1600 Å and EUV 304 Å passbands for 18 flares observed by AIA. In each flare, we have identified thousands of flare ribbon pixels in the UV 1600 Å images, and measured their brightness (counts per second) and the rise and decay timescales, which are indicative of heating properties in flare loops. The analysis shows that bright flare pixels, characterized by peak brightness larger than ten times the quiescent brightness, exhibit sharplight curves with the half rise time below 2 min, followed by a two-phase decay with a rapid decay on timescales comparable to the rise time and then a more gradual decay. Flare ribbon pixels identified in both UV 1600 Å and EUV 304 Å images exhibit similar time profiles during the rise, and their peak brightness appear to be related by a power law. Our analysis shows that AIA observed flare brightness in UV 1600 Å relative to the quiescent brightness is a meaningful measurement of the flare chromosphere photometry. AIA observations for over a decade thus provide a unique and extensive database for systematic and semi-quantitative study of flaring chromosphere, either in the context of the Sun as a star, or in spatially resolved manner that helps to probe the nature of flare energy release on elementary scales.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 9","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-09-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02550-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145211011","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}

引用次数: 0

Observations of Switchback Chains in a Twin-CME Event 双cme事件中切换链的观测

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-29 DOI: 10.1007/s11207-025-02541-w

Emily McDougall, Bala Poduval, Matthew Argall

{"title":"Observations of Switchback Chains in a Twin-CME Event","authors":"Emily McDougall, Bala Poduval, Matthew Argall","doi":"10.1007/s11207-025-02541-w","DOIUrl":"10.1007/s11207-025-02541-w","url":null,"abstract":"<div><p>Magnetic switchbacks, the localized and abrupt reversals in the magnetic field direction, are prominent features in the solar wind. We present the results of a study of switchbacks and the solar energetic particle (SEP) events associated with a twin-CME scenario – described as sequential eruptions of two coronal mass ejections (CMEs) from the same active region occurring within a short time interval – observed by Parker Solar Probe during August 18 – 19, 2022. The two consecutive CMEs, originating from active region (AR) 13078, displayed overlapping trajectories, and the primary CME traversed the wake of the pre-CME within its predicted turbulence duration window, leading to the formation of a significant solar energetic particle (SEP) event. The interaction of these CMEs was further complicated by their embedding within a high-speed stream emanating from a nearby coronal hole which led to increased solar wind density, plasma temperature, and intensified magnetic field strength. The interaction between the twin-CME event and the high-speed stream results in a compression and subsequent process which forced magnetic reconnection. This reconnection produced a distinct chain of magnetic switchbacks downstream of the CME wake, characterized by sharp directional changes in the magnetic field, enhanced transverse ion current, and suprathermal alpha particle flux. The orientation of the magnetic field of the high-speed stream as it surrounded the twin-CME suggests that interchange reconnection facilitated the emergence of switchback structures in the turbulent CME sheath, aligning with predictions from the model by Zank et al. (2020). In addition to the supportive evidences of interchange reconnection as a plausible explanation for switchbacks, our findings are expected to provide deeper insights into CME evolution in high-speed stream environments and have implications for understanding turbulent plasma processes that contribute to solar wind structuring.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 9","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-09-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145210655","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}

引用次数: 0

Short and Intermediate Periodicities in Ca ii K Plage Areas as Seen in Kodaikanal Images for Individual Cycles from 14 to 22 在Kodaikanal图像中从14到22的单个周期中看到Ca ii K斑块区域的短周期和中间周期

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-29 DOI: 10.1007/s11207-025-02545-6

Partha Chowdhury, V. Muthu Priyal, Jagdev Singh, Belur Ravindra

{"title":"Short and Intermediate Periodicities in Ca ii K Plage Areas as Seen in Kodaikanal Images for Individual Cycles from 14 to 22","authors":"Partha Chowdhury, V. Muthu Priyal, Jagdev Singh, Belur Ravindra","doi":"10.1007/s11207-025-02545-6","DOIUrl":"10.1007/s11207-025-02545-6","url":null,"abstract":"<div><p>We analyze historical Ca <span>ii</span> K images from the Kodaikanal Observatory (KO) spanning 1907 to 1996, encompassing Solar Cycles 14 through 22. These digitized images were processed using the Equal Contrast Technique (ECT) to ensure uniform data quality for studying long and short-term variations. From these standardized images, we identify and compute the areas of both plages and network regions in both solar hemispheres in every image. We then utilizy this revised, uniform Ca <span>ii</span> K plage area time series for Solar Cycles 14 to 22. Our primary objective is to investigate the presence of short, Rieger-type periods and quasi-biennial oscillations (QBOs), specifically those near ≈ 1.3 years. To achieve this, we employ both Lomb-Scargle periodograms and Morlet wavelet maps. Our power spectrum analysis consistently shows that Rieger-type periods are significant across all solar cycles, in both the northern and southern hemispheres and in the whole disk data. However, the wavelet analysis reveals that both Rieger-type and QBO periodicities are intermittent, exhibiting varying periods in different cycles and hemispheres. This indicates that plages and network areas demonstrate asymmetric behavior between the two hemispheres. We have also discussed the potential reasons behind these observed periodicities.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 9","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-09-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145210652","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}

引用次数: 0

Application of a Neural Network for Identifying Erroneous Solar Images 神经网络在错误太阳图像识别中的应用

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-26 DOI: 10.1007/s11207-025-02554-5

Kiran Jain, Mitchell Creelman

引用次数: 0

Role of CME Clusters and CME-CME Interactions in Producing Sustained (gamma )-Ray Emission Events CME星团和CME-CME相互作用在产生持续(gamma )射线发射事件中的作用

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-25 DOI: 10.1007/s11207-025-02535-8

Atul Mohan, Pertti Mäkelä, Natchimuthuk Gopalswamy, Sachicko Akiyama, Seiji Yashiro

{"title":"Role of CME Clusters and CME-CME Interactions in Producing Sustained (gamma )-Ray Emission Events","authors":"Atul Mohan, Pertti Mäkelä, Natchimuthuk Gopalswamy, Sachicko Akiyama, Seiji Yashiro","doi":"10.1007/s11207-025-02535-8","DOIUrl":"10.1007/s11207-025-02535-8","url":null,"abstract":"<div><p>Fast (<span>(mathrm{V}_{mathrm{CME}} > 1000text{ km},text{s}^{-1})</span>) coronal mass ejections (CMEs) capable of accelerating protons beyond 300 MeV are thought to trigger hours-long sustained <span>(gamma )</span>-ray emission (SGRE) after the impulsive flare phase. Meanwhile, CME-CME interactions can cause enhanced proton acceleration, increasing the fluxes of solar energetic particles. This study explores the role of fast CME interactions in SGRE production during CME clusters, which we define as a series of CMEs linked to > C-class flares with waiting times < 1 day from the same active region (AR). We focus on clusters in major CME-productive ARs (major ARs), by defining a major AR as one that produced > 1 CME associated to a major (> M-class) flare. The study identified 76 major ARs between 2011 and 2019, of which 12 produced all SGRE events. SGRE-producing ARs exhibit higher median values for the speed of their fastest CMEs (2013 vs. 775 km s<sup>−1</sup>) and the class of their strongest flares (X1.8 vs. M5.8), compared to SGRE-lacking ARs. They also produced relatively faster CMEs (median speed: 1418 vs. 1206.5 km s<sup>−1</sup>), with the SGRE-associated CMEs occurring during periods of higher CME rates than typical fast CME epochs. Twelve of 22 (54.5%) SGRE events and 5 of 7 (71.4%) long-duration (> 10 h) SGRE events occurred during CME clusters, with high chances of CME-CME interactions. A case study on very active major ARs showed that all SGRE-associated CMEs with <span>(mathrm{V}_{mathrm{CME}} lesssim 2000text{ km},text{s}^{-1})</span> underwent CME-CME interactions within ≲ 10 <span>({mathrm{R_{odot }}})</span>, while SGRE-associated CMEs faster than 3000 km s<sup>−1</sup> did not undergo interactions.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 9","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-09-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02535-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145145199","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}

引用次数: 0

Flare Energetics, CME Launch and Heliospheric Propagation for the May 2024 Events, as Derived from Ensemble MHD Modelling 基于Ensemble MHD模型的2024年5月事件的耀斑能量学、日冕物质抛射和日球层传播

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-25 DOI: 10.1007/s11207-025-02553-6

Brigitte Schmieder, Jinhan Guo, Guillaume Aulanier, Anwesha Maharana, Stefaan Poedts

{"title":"Flare Energetics, CME Launch and Heliospheric Propagation for the May 2024 Events, as Derived from Ensemble MHD Modelling","authors":"Brigitte Schmieder, Jinhan Guo, Guillaume Aulanier, Anwesha Maharana, Stefaan Poedts","doi":"10.1007/s11207-025-02553-6","DOIUrl":"10.1007/s11207-025-02553-6","url":null,"abstract":"<div><p>Many questions must be answered before understanding the relationship between the emerging magnetic flux through the solar surface and the extreme geoeffective events. The main ingredients for getting X-ray class flares and large interplanetary Coronal Mass Ejections (CMEs) are the buildup of electric current in the corona, the existence of magnetic free energy, magnetic energy/helicity ratio, twist, and magnetic stress in active regions (ARs). The upper limit of solar energy in the space research era, as well as the potential for experiencing superflares and extreme solar events, can be predicted using MHD simulations of CMEs.</p><p>To address this problem, we consider the recent events of May 2024 and use three MHD models:</p><p>1) OHM (“Observationally driven High order scheme Magnetohydrodynamic code”) for investigating the magnetic evolutions at a synthetic dipole structure.</p><p>2) TMF (time-dependent magneto-friction) for setting up an initial non-potential magnetic field in the active region. A zero-beta MHD model for tracing the magnetic evolution of active regions.</p><p>3) EUHFORIA (“European heliospheric forecasting information asset”) for interplanetary CME propagations.</p><p>For the eruptive flares with CMEs, magnetic solar energy is computed along with data-constrained MHD simulations for the May 2024 events. We show the consistency between the data-initiated, realistic simulation of the May 2024 big event and energy scalings from an idealised simulation of a bipolar eruption using OHM. The estimated free magnetic energy did not surpass <span>(5.2 times 10^{32}text{ erg})</span>. Good arrival time predictions (<span>(<3)</span> hours) are achieved with the EUHFORIA simulation with the cone model. We note the interest in coupling all the chains of codes from the Sun to the Earth and developing different approaches to test the results.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 9","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-09-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145145200","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}

引用次数: 0

Observations of Flare Induced Doppler Shifts in the Si iii 1206 Å Line Si ii1206 Å线耀斑诱导多普勒频移的观测

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-23 DOI: 10.1007/s11207-025-02548-3

Luke H. Majury, Ryan O. Milligan

{"title":"Observations of Flare Induced Doppler Shifts in the Si iii 1206 Å Line","authors":"Luke H. Majury, Ryan O. Milligan","doi":"10.1007/s11207-025-02548-3","DOIUrl":"10.1007/s11207-025-02548-3","url":null,"abstract":"<div><p>Doppler shifts in chromospheric and transition-region lines during solar flares are often interpreted as chromospheric condensation or evaporation. However, alternative sources of Doppler-shifted emission have been suggested, such as filament eruptions, jets or chromospheric bubbles. We analyse high-cadence scans from SORCE/SOLSTICE, which provide one-minute resolution profiles of the transition-region Si <span>iii</span> (1206 Å, <span>(textrm{T} = 10^{4.6},textrm{K})</span>) line. 11 X-, M-, and C-class events observed during these scans with clear impulsive phase Si <span>iii</span> enhancements were identified. By subtracting a quiet-Sun profile and fitting Gaussian profiles to the Si <span>iii</span> line, measurements of flare-induced Doppler shifts were made. After correcting for a systematic trend in these shifts with solar longitude, two of the 11 events were found to exhibit a significant Doppler shift, one with a <span>(201.36pm 21.94;textrm{km,s}^{-1})</span> redshift and the other with a <span>(-39.75pm 11.00;textrm{km,s}^{-1})</span> blueshift. Intriguingly, SDO/AIA 304 Å and 1600 Å imaging revealed a bright eruption coincident with the event that exhibited a blueshift, suggesting the shift may have resulted from the eruption rather than evaporation alone. Our results highlight Si <span>iii</span> as a useful diagnostic of flaring dynamics at a temperature that has received limited attention to date. Future comparisons of these observations with radiative hydrodynamic simulations, along with new observations from state-of-the-art spectrometers such as SOLAR-C/EUVST and MUSE, should clarify the mechanisms behind the observed shifts in this study.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 9","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-09-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02548-3.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145110510","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}

引用次数: 0

Activity-Cycle Variations of Convection Scales in Subsurface Layers of the Sun 太阳亚表层对流尺度的活动周期变化

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-18 DOI: 10.1007/s11207-025-02546-5

Alexander V. Getling, Alexander G. Kosovichev

引用次数: 0

MHD Simulations of CME with Associated Prominence Eruption 日珥喷发伴随日冕物质抛射的MHD模拟

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2025-09-17 DOI: 10.1007/s11207-025-02547-4

Yuhong Fan

引用次数: 0