Solar Physics最新文献

{"title":"Spectral Cross-Calibrations of ASO-S/HXI with Other X-ray Missions","authors":"Zhentong Li,&nbsp;Yang Su,&nbsp;Wei Liu,&nbsp;Wei Chen,&nbsp;Fu Yu,&nbsp;Weiqun Gan","doi":"10.1007/s11207-025-02465-5","DOIUrl":"10.1007/s11207-025-02465-5","url":null,"abstract":"<div><p>Cross-calibration of X-ray instruments is crucial for stereoscopic studies of solar hard X-ray directivity and three-dimensional morphology, where spectral and imaging differences observed from multiple perspectives provide critical constraints. We present the preliminary results of the spectral calibrations of ASO-S/HXI through internal consistency checks of its three total flux detectors and cross-calibrations with Solar Orbiter/STIX, Fermi/GBM, and Konus-Wind data. Both calibration tests suggest that the response matrix of one of the HXI total flux monitors, D94 (with a thin aluminum window), needs to be modified. The new response matrix is determined by testing the series of response matrices with changing effective aluminum thickness through simulations. Post-correction analysis reveals <span>(sim 88%)</span> of co-observed events demonstrate electron spectral index consistency within <span>(pm 0.5)</span>, while comparisons of the total counts above 30 keV show &lt; 10% differences for STIX-HXI flares with separation angles &lt; 20° and Fermi-observed moderate flares. Though challenges persist regarding detector response uncertainties, the pile-up effect, and other nonideal factors, the achieved inter-instrument consistency enables quantitative electron anisotropy investigations through joint spectral analysis.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02465-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143875473","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":"Effect of Nonlinear Surface Inflows into Activity Belts on Solar Cycle Modulation","authors":"Mohammed H. Talafha,&nbsp;Kristóf Petrovay,&nbsp;Andrea Opitz","doi":"10.1007/s11207-025-02466-4","DOIUrl":"10.1007/s11207-025-02466-4","url":null,"abstract":"<div><p>Converging flows are visible around bipolar magnetic regions (BMRs) on the solar surface, according to observations. Average flows are created by these inflows combined, and the strength of these flows depends on the amount of flux present during the solar cycle. In models of the solar cycle, this average flow can be depicted as perturbations to the meridional flow. In this article, we study the effects of introducing surface inflow to the surface flux transport models (SFT) as a possible nonlinear mechanism in the presence of latitude quenching for an inflow profile whose amplitude varies within a cycle depending on the magnetic activity. Using a grid based on one-dimensional SFT models, we methodically investigate the extent of the nonlinearity caused by inflows, latitude quenching (LQ), and their combinations. The results show that including surface inflows in the model in the presence of both LQ and tilt quenching (TQ) produced a polar field within a <span>(pm 1sigma )</span> of an average cycle polar field (<span>(sigma )</span> is the standard deviation) with a correlation coefficient of 0.85. We confirm that including inflows produces a lower net contribution to the dipole moment (10 – 25%). Furthermore, the relative importance of LQ vs. inflows is inversely correlated with the dynamo effectivity range (<span>(lambda _{R})</span>). With no decay term, introducing inflows into the model results in a less significant net contribution to the dipole moment. Including inflows in the SFT model shows a possible nonlinear relationship between the surface inflows and the solar dipole moment, suggesting a potential nonlinear mechanism contributing to the saturation of the global dynamo. For lower <span>(lambda _{R})</span> (<span>(lessapprox 10^{circ })</span>), TQ always dominates LQ, and for higher <span>(lambda _{R})</span>, LQ dominates. However, including inflows makes the domination earlier in case of having a decay term in the model.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02466-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143875262","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":"Analysis of the Vertical Current Evolution for the X9.3 Flare on 6 September 2017","authors":"Haili Li,&nbsp;Xiaofeng Deng,&nbsp;Hongfei Liang,&nbsp;Xinping Zhou,&nbsp;Yu Liu,&nbsp;Zhongquan Qu","doi":"10.1007/s11207-025-02467-3","DOIUrl":"10.1007/s11207-025-02467-3","url":null,"abstract":"<div><p>In this article, we examine the morphological evolution and current distribution of the X9.3-class flare on 6 September 2017 that occurred in the active region (AR) 12673. We combine the high-resolution observations of the Atmospheric Imaging Assembly (AIA) and Helioseismic Magnetic Imager (HMI) instruments on board the Solar Dynamics Observatory. The vertical current intensity and the soft X-ray flux within the active region showed two peaks, corresponding, respectively, to the X2.2 and X9.3 flares on that day, while the latter constituted a more significant increase. A pair of conjugate current ribbons appeared at the same locations consistent with the two ribbons of the flare. These current ribbons underwent sustained and significant changes during the X9.3 flare eruption. In the early period of the flare, there was a substantial decrease in the area of the current ribbons, resulting in the emergence of a series of high-density small current islands. During the later phase, not only did the area of the currents rapidly increase, but also the flare kernels evolved into two flare bands along the sheared magnetic neutral line in the photosphere. The AIA 1600 Å and 304 Å images revealed that the two ribbons of the X9.3 flare formed from small bright kernels. It was also observed that the positions of the flare kernels closely matched those of the current islands. Based on the vertical current distribution and evolution near the highly sheared core field region during the X9.3 flare, we conclude that this flare eruption should be attributed to tether-cutting magnetic reconnection.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143871417","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":"A Multi-Viewpoint CME Catalog Based on SoloHI Observed Events","authors":"Cecilia Mac Cormack,&nbsp;Shaheda B. Shaik,&nbsp;Phillip Hess,&nbsp;Robin Colaninno,&nbsp;Teresa Nieves-Chinchilla","doi":"10.1007/s11207-025-02463-7","DOIUrl":"10.1007/s11207-025-02463-7","url":null,"abstract":"<div><p>Coronal mass ejections (CMEs) are significant drivers of geomagnetic activity, and understanding these structures is critical to developing and improving forecasting tools for space weather. The Solar Orbiter (SolO) mission, with its comprehensive set of remote sensing and in-situ instruments, along with its unique orbit, is significantly advancing the study of the CMEs and other structures in the heliosphere. A critical contribution to the study of CMEs by SolO is the observations from the Solar Orbiter Heliospheric Imager (SoloHI). SoloHI observes photospheric visible light, which is scattered by electrons in the solar wind, and provides high-resolution observations of the corona and heliosphere. The resolution and vantage point offered by SoloHI make it uniquely well-suited to study CME evolution in the heliosphere. To contribute to the science goals of SolO, we present the initial release of a living CME catalog based on SoloHI observations during its initial years of observations, with a multi-viewpoint focus. We catalog 140 events detected by SoloHI during the period of January 2022 until April 2023. For each event detected by SoloHI, we present available in-situ data and remote sensing observations detected by other missions. With the available observations, we identify the source region of the CME and describe its main characteristics, track the CME through the coronagraphs and heliospheric imagers, and provide in-situ detection when possible. We also provide a morphological classification and observations quality parameter based on the SoloHI observations. Additionally, we cross-check with other available CME catalogs and link to the event description provided by the Space Weather Database Of Notifications, Knowledge, Information (DONKI) catalog, developed at the Community Coordinated Modeling Center (CCMC). In this article, we describe the features of the SoloHI CME catalog and the methods used to generate the entries. We also present a statistical study of the morphological classification of the cataloged CMEs in the SoloHI observations, building up on the previous studies that classify the events observed by LASCO coronagraphs. We provide various observing scenarios with SoloHI observations to demonstrate the contribution that this catalog offers to the scientific community to explore the new observing viewpoint of CMEs with the SolO mission.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02463-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143840288","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":"Magnitude Prediction of Solar Cycle 26 Using a New Precursor Approach","authors":"Mohammed Akram Zermane,&nbsp;Nadia Oulebsir,&nbsp;Mohamed Reda Bekli,&nbsp;Zahir Belhadi,&nbsp;Katia Becheker,&nbsp;Abdeldjalil Zaidi,&nbsp;Abdelghani Hadj Hammou","doi":"10.1007/s11207-025-02459-3","DOIUrl":"10.1007/s11207-025-02459-3","url":null,"abstract":"<div><p>A long-term prediction approach for solar cycles is proposed by including the century-scale modulation in the SODA (Solar Dynamo Amplitude) and XSODA (Extended Solar Dynamo Amplitude) indices of Schatten and Pesnell, MSODA and MXSODA. Additionally, we also introduce a new technique, the minimal fluctuation method, to reduce temporal fluctuations. By combining this method with MSODA, we predict that Solar Cycle 26 will reach a maximum sunspot number of <span>(109.14pm 32.92)</span> in the year <span>(2035.3 pm 2.3)</span>. Using MXSODA, the most reliable indicator, the peak is expected to reach a maximum amplitude of <span>(160.70pm 47.83)</span> on the same date.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793173","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":"14C-Based Sunspot Numbers for the Last Millennium Encompass the Full Range of Variability: Extreme Value Theory","authors":"F. J. Acero,&nbsp;V. M. S. Carrasco,&nbsp;M. C. Gallego,&nbsp;I. G. Usoskin,&nbsp;J. M. Vaquero","doi":"10.1007/s11207-025-02464-6","DOIUrl":"10.1007/s11207-025-02464-6","url":null,"abstract":"<div><p>We examine the statistical properties of extreme solar activity levels through the application of the extreme value theory to the annual sunspot number series reconstructed from ¹⁴C data spanning the last millennium. We have used the extreme value theory to study long-term solar variability by applying the peaks-over-threshold technique to an annual sunspot number series reconstructed from ¹⁴C data for the last millennium. We have obtained a negative value of the shape parameter of the generalized Pareto distribution implying that an upper bound has been reached by the extreme sunspot number value distribution during the past millennium. The results obtained from the same analysis applied to two subperiods of the series, are consistent with that considering the whole series. We have also estimated return levels and periods for the extreme sunspot numbers. The maximum annual sunspot number (273.6) observed during the past millennium is slightly higher (lower) than that considering a 1000-year (10,000-year) return level, but they are within the 95% confidence interval in both cases. It approximately corresponds to a 3500-year return period. Our result implies that solar activity has reached its upper limit, and it would be unlikely to observe, in the near future, sunspot numbers significantly higher than those already observed during the past millennium.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02464-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793072","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":"New Index Characterizing Magnetic Field Turbulence in Relation to the Galactic Cosmic Ray Intensity Variation in the Period 1968 – 2023","authors":"M. Siluszyk,&nbsp;K. Iskra","doi":"10.1007/s11207-025-02453-9","DOIUrl":"10.1007/s11207-025-02453-9","url":null,"abstract":"<div><p>Data on the <span>(B_{y})</span> and <span>(B_{z})</span> components of the heliospheric magnetic field (HMF) were used to study the relationships between the Power Spectral Density (PSD) (<span>(PSDpropto f^{-nu } )</span>, <span>(f)</span> is the frequency) of HMF turbulence and the rigidity spectrum variation (RSV) of the galactic cosmic ray (GCR) intensity (<span>(delta D(R)/D(R) propto R^{- gamma } )</span>). A new common exponent <span>(nu _{yz})</span> was constructed to account for the contributions of both the <span>(B_{y})</span> and <span>(B_{z})</span> components of the HMF. The period from 1969 to 2022 was considered, divided into five subperiods based on the global solar magnetic field (GSMF) polarities: i) 1969 – 1979 (<span>(A&gt;0)</span>) (positive polarity—magnetic field lines directed away from the Sun’s northern hemisphere), ii) 1980 – 1990 (<span>(A&lt;0)</span>) (negative polarity—magnetic field lines directed towards the Sun’s northern hemisphere), iii) 1991 – 2002 (<span>(A&gt;0)</span>), iv) 2003 – 2013 (<span>(A&lt;0)</span>), and v) 2014 – 2022 (<span>(A&gt;0)</span>). The analysis of these five subperiods confirmed a close relationship between the PSD and the RSV, determined by the exponents <span>(nu _{yz})</span> and <span>(gamma )</span>, respectively. These exponents, calculated from independent sources, may be important parameters in the study of long-term GCR variations in the heliosphere.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793113","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":"The Properties of Non-Potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares","authors":"S. Liu,&nbsp;Shahid Idrees,&nbsp;D. Liu,&nbsp;S. G. Zeng","doi":"10.1007/s11207-025-02456-6","DOIUrl":"10.1007/s11207-025-02456-6","url":null,"abstract":"<div><p>Solar active regions (ARs), characterized by intense magnetic fields, are prime locations for solar flares. Understanding the properties of these magnetic fields is crucial for predicting and mitigating space weather events. In this study, the non-potential magnetic field parameters of active region (AR) NOAA 9077 are investigated; this AR experienced a super-strong X5.7 solar flare. Using advanced extrapolation techniques, the 3D magnetic field structure from vector magnetograms is obtained using the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station (HSOS). Then, various non-potential parameters are calculated, including current density, shear angle, quasi-separatrix layers (QSLs), twist, and field line helicity. By analyzing the spatial and temporal distributions of these parameters, we aim to shed light on the relationship between magnetic field properties and solar flare occurrence. Our findings reveal that high twist and complex magnetic field configurations are prevalent before flares, while these features tend to weaken after the eruption. Additionally, we observe decreases in helicity and free energy after the flare, while the free energy peaks approximately 1.5 days prior to the onset of the flare. Furthermore, we investigate the distribution of quasi-separatrix layers and twist, finding high degrees of complexity before flares. Multiple patterns of high current density regions suggest unstable magnetic structures prone to flaring, coinciding with the shear angle distribution. Relative field line helicity patterns exhibit distinct characteristics compared to current density, concentrating before flares and diverging afterward. Overall, our results highlight the contrasting nature of current density and relative field line helicity patterns in relation to solar flares, in addition to the aforementioned features in the set of commonly derived non-potential parameters for this particular event.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793101","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":"Direct Measurement of the Longitudinal Magnetic Field in the Solar Photosphere with the Zeeman Effect","authors":"Jie Chen,&nbsp;Jiangtao Su,&nbsp;Wenbin Xie,&nbsp;Yuanyong Deng,&nbsp;Xianyong Bai,&nbsp;Ziyao Hu,&nbsp;Haiqing Xu,&nbsp;Suo Liu,&nbsp;Yin Zhang,&nbsp;Yingzi Sun,&nbsp;Yongliang Song,&nbsp;Xiaofan Wang","doi":"10.1007/s11207-025-02455-7","DOIUrl":"10.1007/s11207-025-02455-7","url":null,"abstract":"<div><p>The primary objective of our research is to validate direct measurements of the solar magnetic field through calculating the splitting of polarized spectral lines. The data are collected by the Solar Magnetism and Activity Telescope (SMAT) located at the Huairou Solar Observing Station (HSOS). The number of sampling points of the spectral line profile was varied from 5 to 31. By fitting the profiles of left- and right-circularly polarized light intensities, we determined the spectral line splitting, and the error between the magnetic-field strength determined from this and the true value was less than 2%. We found that the correlation between the magnetic-field strength measured in the active regions by SMAT and that observed by Helioseismic and Magmetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) reached about 80%, but in the quiet region, this correlation was very low.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143778065","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":"On Field Line Slippage Rates in the Solar Corona","authors":"David MacTaggart","doi":"10.1007/s11207-025-02462-8","DOIUrl":"10.1007/s11207-025-02462-8","url":null,"abstract":"<div><p>Magnetic reconnection is one of the fundamental dynamical processes in the solar corona. The method of studying reconnection in active region-scale magnetic fields generally depends on <i>non-local</i> methods (i.e. requiring information across the magnetic field under study) of magnetic topology, such as separatrix skeletons and quasi-separatrix layers. The theory of General Magnetic Reconnection is also non-local, in that its measure of the reconnection rate depends on determining the maxima of integrals along field lines. In this work, we complement the above approaches by introducing a <i>local</i> description of magnetic reconnection, that is one in which information about reconnection at a particular location depends only on quantities at that location. This description connects the concept of the <i>field line slippage rate</i>, relative to ideal motion, to the underlying local geometry of the magnetic field characterized in terms of the Lorentz force and field-aligned current density. It is argued that the dominant non-ideal term for the solar corona, discussed in relation to this new description, is mathematically equivalent to the anomalous resistivity employed by many magnetohydrodynamic simulations. However, the general application of this new approach is adaptable to the inclusion of other non-ideal terms, which may arise from turbulence modelling or the inclusion of a generalized Ohm’s law. The approach is illustrated with two examples of coronal magnetic fields related to flux ropes: an analytical model and a nonlinear force-free extrapolation. In terms of the latter, the slippage rate corresponds to the reconnection that would happen if the given (static) force-free equilibrium were the instantaneous form of the magnetic field governed by an Ohm’s law with non-ideal terms.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02462-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143778066","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}