Solar Physics最新文献

The Sun as a Rosetta Stone for Understanding Star–Planet Interactions 太阳是理解恒星-行星相互作用的罗塞塔石碑

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-05-08 DOI: 10.1007/s11207-026-02654-w

Maria Pia Di Mauro, Camilla Pezzotti, Raffaele Reda, Nuno Moedas, Luca Giovannelli

{"title":"The Sun as a Rosetta Stone for Understanding Star–Planet Interactions","authors":"Maria Pia Di Mauro, Camilla Pezzotti, Raffaele Reda, Nuno Moedas, Luca Giovannelli","doi":"10.1007/s11207-026-02654-w","DOIUrl":"10.1007/s11207-026-02654-w","url":null,"abstract":"<div><p>The Sun serves as a unique and invaluable reference point, or “Rosetta Stone”, for the study of other planetary systems. As the only star that can be observed with high spatial and temporal resolution, the Sun provides critical insight into stellar structure and activity, exoplanet formation, and star–planet interactions.</p><p>We demonstrate the efficiency of a multi-disciplinary approach to interpret phenomena observed in distant exoplanetary systems by analogy with the Sun-Earth system. By applying the Star-Planet Interaction (SPI) code to a highly accurate model of the host star constrained by asteroseismic observations and empirical stellar wind proxies, we show that it is possible to quantify the impact of the star’s rotation and gravitational-tidal interaction on the long-term evolution of exoplanets including the resulting atmospheric loss and its implications for habitability.</p><p>Here we show results obtained for the case of the Sun and provide a powerful framework for interpreting the habitability potential of exoplanetary systems across the Galaxy.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02654-w.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147830066","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

Magnetic Reconnection at a Hyperbolic Flux Tube Associated with a Confined Flare in NOAA Active Region 12268 美国国家海洋和大气管理局活跃区12268中与受限耀斑相关的双曲通量管的磁重联

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-05-07 DOI: 10.1007/s11207-026-02658-6

Pawan Kumar, Sadashiv, Sanjay Kumar, Sushree S. Nayak, Simrat Kaur, Ramit Bhattacharya

{"title":"Magnetic Reconnection at a Hyperbolic Flux Tube Associated with a Confined Flare in NOAA Active Region 12268","authors":"Pawan Kumar,  Sadashiv, Sanjay Kumar, Sushree S. Nayak, Simrat Kaur, Ramit Bhattacharya","doi":"10.1007/s11207-026-02658-6","DOIUrl":"10.1007/s11207-026-02658-6","url":null,"abstract":"<div><p>In this article, we identify the magnetic reconnections at the hyperbolic flux tube (HFT), aided by slipping reconnection at quasi-separatrix layers (QSLs), which are pivotal to the occurrence of a confined M2.1 class flare in NOAA active region 12268. The magnetic field topology before the flare onset is obtained through a non-force-free field extrapolation scheme that accommodates a non-zero Lorentz force. A key aspect is the presence of an HFT in the computational domain above the flaring region, along with two QSLs at the lower boundary. To simulate the dynamics of the active region, we conduct a data-constrained magnetohydrodynamic (MHD) simulation initiated by the extrapolated field. The dynamics captured in the simulation document the formation of a current sheet within the HFT configuration, leading to magnetic reconnection at the HFT. Additionally, we observe the slipping motion of the footpoints of the magnetic field lines in the QSLs at the bottom boundary, which indicates the occurrence of slipping reconnection in the QSLs. Importantly, the magnetic reconnection at the HFT is suggested to be the primary driver in the development of the intricate flare brightenings and the flare ribbons.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147829667","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

How the Solar Dynamics Observatory Advanced Our Physical Understanding of the Sun 太阳动力学观测站如何促进了我们对太阳的物理认识

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-05-07 DOI: 10.1007/s11207-026-02657-7

Markus J. Aschwanden

引用次数: 0

Comparing Magnetic Field Distribution of Active Regions: Part 1 Methods of Mode Analysis 磁场分布比较：第一部分模态分析方法

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-05-04 DOI: 10.1007/s11207-026-02659-5

P. Bhowmik, C. B. Prior

{"title":"Comparing Magnetic Field Distribution of Active Regions: Part 1 Methods of Mode Analysis","authors":"P. Bhowmik, C. B. Prior","doi":"10.1007/s11207-026-02659-5","DOIUrl":"10.1007/s11207-026-02659-5","url":null,"abstract":"<div><p>We develop methods for comparing solar active region magnetic fields using two forms of mode analysis. These methods are designed to directly compare all three field components of the magnetic field and characterise their differences in a manner that is both meaningful and interpretable. The first mode decomposition is a Zernike polynomial analysis, the planar counterpart of a spherical polar decomposition, used to compare the spectral properties of the fields at both small and large scales, as well as to assess the dominance of particular modes (bipolar/quadrupolar). The second method is a multi-resolution (wavelet) analysis, which allows one to precisely quantify the spatial variation between the fields. In this study, we use these decompositions to compare and contrast magnetogram data derived from convective flux emergence experiments with observed active-region data, in order to assess their viability as models of active-region formation. We show that both elements: a significant contribution from the rise through the convective zone in the model, and the choice of initial condition, play a key role in simulations accurately recreating the spectral properties of active region fields.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 5","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-05-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147807616","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

Medium-Term Forecasting of Solar F10.7 Using VMD-SOBI-DLinear Hybrid Model 基于VMD-SOBI-DLinear混合模型的太阳能F10.7中期预报

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-04-27 DOI: 10.1007/s11207-026-02656-8

Yang Guo, Boyang Wang, Xueshu Shi, Jian Sun, Jiaxing He

{"title":"Medium-Term Forecasting of Solar F10.7 Using VMD-SOBI-DLinear Hybrid Model","authors":"Yang Guo, Boyang Wang, Xueshu Shi, Jian Sun, Jiaxing He","doi":"10.1007/s11207-026-02656-8","DOIUrl":"10.1007/s11207-026-02656-8","url":null,"abstract":"<div><p>The F10.7 index serves as a key indicator of solar activity, and its accurate prediction is essential for mitigating adverse effects on radio communications, navigation systems, and satellite operations. This paper proposes a hybrid model integrating Variational Mode Decomposition (VMD), Second-Order Blind Identification (SOBI), and Deep Linear Network (DLinear) for medium-term prediction of the F10.7 index. The proposed approach begins by applying VMD to decompose the F10.7 time series into multiple modal components with distinct frequency characteristics, thereby reducing the inherent non-linearity and complexity of the data. Subsequently, SOBI is employed to extract independent source signals from these modal components, enhancing feature interpretability and discriminability. Finally, the DLinear model is utilized to model and predict the F10.7 index based on the refined features. Experimental results demonstrate that the VMD–SOBI–DLinear model achieves significant performance improvements in medium-term F10.7 forecasting. Compared to Informer, the proposed model exhibits enhanced prediction accuracy across the 1 – 27 day horizon, with MAE and RMSE reduced by 42.0% and 35.5%, respectively, at the 27-day prediction window. Moreover, the model maintains robust performance during both solar maximum and minimum periods, indicating its strong potential as a core tool for operational medium-term space weather forecasting.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 4","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-04-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147796556","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

Revealing Flare Energetics and Dynamics with SDO EVE Solar Extreme Ultraviolet Spectral Irradiance Observations 利用SDO EVE观测太阳极紫外光谱辐照度揭示耀斑能量和动力学

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-04-21 DOI: 10.1007/s11207-026-02650-0

Thomas N. Woods, Phillip C. Chamberlin, Andrew Jones, James P. Mason, Liying Qian, Harry P. Warren, Don Woodraska, Rita Borelli, Francis G. Eparvier, Gabi Gonzalez

{"title":"Revealing Flare Energetics and Dynamics with SDO EVE Solar Extreme Ultraviolet Spectral Irradiance Observations","authors":"Thomas N. Woods, Phillip C. Chamberlin, Andrew Jones, James P. Mason, Liying Qian, Harry P. Warren, Don Woodraska, Rita Borelli, Francis G. Eparvier, Gabi Gonzalez","doi":"10.1007/s11207-026-02650-0","DOIUrl":"10.1007/s11207-026-02650-0","url":null,"abstract":"<div><p>NASA’s Solar Dynamics Observatory (SDO) Extreme-ultraviolet Variability Experiment (EVE) has been making solar full-disk extreme ultraviolet (EUV) spectral measurements since 2010 over the spectral range of 6 nm to 106 nm with 0.1 nm spectral resolution and with 10 – 60 sec cadence. A primary motivation for EVE’s solar EUV irradiance observations is to provide the important energy input for various studies of Earth’s upper atmosphere. For example, the solar EUV radiation creates the ionosphere, heats the thermosphere, and drives photochemistry in Earth’s upper atmosphere. In addition, EVE’s observations have been a treasure trove for solar EUV flare spectra. While EVE measures the full-disk spectra, the flare spectrum is easily determined as the EVE spectrum minus the pre-flare spectrum, as long as only one flare event is happening at a time. These EVE flare observations provide EUV variability with 0.1 nm spectral resolution and have been used to study flare phases (including the discovery of the EUV Late Phase flare class), flare energetics (plasma temperature variations), corona heating (plasma abundance changes that support nano-flare heating mechanism), flare dynamics (downwelling and upwelling plasma flows during flares from Doppler-related wavelength shifts), and coronal mass ejections (CME) energetics (CME mass and velocity derived from coronal dimming in some EUV lines). A brief review of each of these flare research topics using EVE data are presented. With over 10,000 flares detected in the EVE observations, there is still much to study and to learn about solar flare physics using EVE solar EUV spectra.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 4","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02650-0.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147738099","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

Machine Learning–Based Characterization of Solar p-Mode Frequency Shifts During Solar Cycle 25 基于机器学习的第25太阳周期p模频移表征

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-04-21 DOI: 10.1007/s11207-026-02660-y

Rekha Jain, Akash Kumar, Sushanta C. Tripathy

{"title":"Machine Learning–Based Characterization of Solar p-Mode Frequency Shifts During Solar Cycle 25","authors":"Rekha Jain, Akash Kumar, Sushanta C. Tripathy","doi":"10.1007/s11207-026-02660-y","DOIUrl":"10.1007/s11207-026-02660-y","url":null,"abstract":"<div><p>The solar interior is probed by the properties of the Sun’s acoustic oscillations (<span>(p)</span>-modes) observed on the solar surface. The frequencies of these <span>(p)</span>-modes measured in the last three decades show long term variation similar to the ∼ 11 year cyclic behaviour exhibited by 10.7 cm radio flux, sunspot numbers, and other solar activity indices. It is also now established that the cyclic behavior of some of the solar proxies is connected with geomagnetic activities and has implications for space weather. Hence, in recent years efforts have been made using machine-learning methods to forecast these solar proxies with a view to improve our understanding of space weather. Developing a comparable method for forecasting <span>(p)</span>-mode frequency shifts is therefore of interest for two reasons. Firstly, it will facilitate future investigations into its potential role in tracing energy drivers from the Sun’s interior to the geospace response by improving models of solar interior dynamics to coronal and heliospheric plasma conditions. In other words, it will help establish a more robust and quantitative link between the Sun’s interior and its exterior. Secondly, it may provide us with an independent indicator or an early indicator of ascending and descending phase of solar activity which might be useful for space weather forecasting.</p><p>In this article, we develop and apply the standard time-series analysis and machine-learning based methods to characterise <span>(p)</span>-mode frequency shifts for the remaining Solar Cycle 25.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 4","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02660-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147738080","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

Oscillatory Dynamics and Energy Transport in Twisted Magnetic Flux Tubes of the Solar Photosphere 太阳光球扭曲磁通管的振荡动力学和能量输运

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-04-20 DOI: 10.1007/s11207-026-02652-y

Adel S. Alanezy, Suzana S. A. Silva, Istvan Ballai, Gary Verth, Viktor Fedun

{"title":"Oscillatory Dynamics and Energy Transport in Twisted Magnetic Flux Tubes of the Solar Photosphere","authors":"Adel S. Alanezy, Suzana S. A. Silva, Istvan Ballai, Gary Verth, Viktor Fedun","doi":"10.1007/s11207-026-02652-y","DOIUrl":"10.1007/s11207-026-02652-y","url":null,"abstract":"<div><p>We investigate the oscillatory behaviour of the footpoints of twisted magnetic flux tubes in the solar photosphere. We identify the dominant magnetohydrodynamic (MHD) wave modes present in these waveguides and assess their role in energy transport. Using vector magnetograms from the Solar Dynamics Observatory/Helioseismic and Magnetic Imager Space-weather HMI Active Region Patches (SDO/HMI SHARP) series of active region 11158, the footpoints of twisted flux tubes are identified as convex local maxima of the Integrated Average Current Deviation (IACD) field, which highlights regions of enhanced magnetic twist and current concentration. To study the waves propagating in these structures, we apply the Spectral Proper Orthogonal Decomposition (SPOD) method, which separates complex spatio-temporal data into oscillatory patterns and their characteristic frequencies. Our analysis shows that the footpoints of the twisted flux tubes support both kink and sausage MHD modes, with oscillations detected across multiple diagnostics, including IACD, the vertical magnetic field, and the vertical Poynting flux. The coexistence of these modes suggests nonlinear interactions or mode coupling within the twisted magnetic structures. These twisted flux tubes act as magnetic waveguides that modulate the vertical transport of energy between the photosphere and higher atmospheric layers. The inferred upward Poynting fluxes (<span>(10^{5})</span> – <span>(10^{6}~mathrm{W,m^{-2}})</span>) indicate that such twisted magnetic features may contribute to localised chromospheric heating.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 4","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02652-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147738332","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

Hybrid ANN+PSO Technique for Accurate Short-Term F10.7 Index Forecasting 基于神经网络+粒子群算法的F10.7指数短期准确预测

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-04-15 DOI: 10.1007/s11207-026-02655-9

J. A. Lazzús, I. Salfate

引用次数: 0

Comparative Analysis of the Halloween 2003 and May 2024 Storms: From the State of the Sun to Geomagnetic Fluctuations 2003年万圣节和2024年5月风暴的比较分析：从太阳状态到地磁波动

IF 2.4 3区物理与天体物理

Solar Physics Pub Date : 2026-04-15 DOI: 10.1007/s11207-026-02642-0

Anna Wawrzaszek, Agnieszka Gil, Renata Modzelewska, Fabian Zgiet

{"title":"Comparative Analysis of the Halloween 2003 and May 2024 Storms: From the State of the Sun to Geomagnetic Fluctuations","authors":"Anna Wawrzaszek, Agnieszka Gil, Renata Modzelewska, Fabian Zgiet","doi":"10.1007/s11207-026-02642-0","DOIUrl":"10.1007/s11207-026-02642-0","url":null,"abstract":"<div><p>As the Sun approaches the peak of its activity cycle, it creates the opportunity for more frequent and intense geomagnetic storms to affect Earth. This was clearly observed in early spring of 2023 when the Sun released several eruptive events. A recent geomagnetic storm in May 2024 served as another powerful reminder that the Sun’s state directly influences conditions on Earth, leading to increased fluctuations in our planet’s magnetic field. Consequently, auroras and other manifestations of solar activity were seen even at mid-latitudes.</p><p>In this work, we focus on the Halloween storm of 2003 and the May storm of 2024, the two strongest geomagnetic events in the last three Solar Cycles. We perform a systematic comparison of the state of the Sun prior to the storms, focusing on solar flares and Halo coronal mass ejections. A comparative analysis of solar wind parameters and geomagnetic field responses is conducted to describe the strength of individual events and to reveal similarities and differences between the two storms. To characterize geoeffectiveness during the considered periods thoroughly, the geomagnetically induced currents indices are discussed based on data for latitudes between <span>(58^{circ })</span> and <span>(70^{circ })</span> in the European region.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"301 4","pages":""},"PeriodicalIF":2.4,"publicationDate":"2026-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-026-02642-0.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147737540","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