Solar Physics最新文献_第3页

14C-Based Sunspot Numbers for the Last Millennium Encompass the Full Range of Variability: Extreme Value Theory 过去一千年基于 14C 的太阳黑子数涵盖了全部变异范围：极值理论

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-07 DOI: 10.1007/s11207-025-02464-6

F. J. Acero, V. M. S. Carrasco, M. C. Gallego, I. G. Usoskin, J. M. Vaquero

{"title":"14C-Based Sunspot Numbers for the Last Millennium Encompass the Full Range of Variability: Extreme Value Theory","authors":"F. J. Acero, V. M. S. Carrasco, M. C. Gallego, I. G. Usoskin, 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 <sup>14</sup>C 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 <sup>14</sup>C 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}

引用次数: 0

New Index Characterizing Magnetic Field Turbulence in Relation to the Galactic Cosmic Ray Intensity Variation in the Period 1968 – 2023 描述 1968-2023 年间磁场湍流与银河宇宙射线强度变化关系的新指数

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-07 DOI: 10.1007/s11207-025-02453-9

M. Siluszyk, K. Iskra

{"title":"New Index Characterizing Magnetic Field Turbulence in Relation to the Galactic Cosmic Ray Intensity Variation in the Period 1968 – 2023","authors":"M. Siluszyk, 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>0)</span>) (positive polarity—magnetic field lines directed away from the Sun’s northern hemisphere), ii) 1980 – 1990 (<span>(A<0)</span>) (negative polarity—magnetic field lines directed towards the Sun’s northern hemisphere), iii) 1991 – 2002 (<span>(A>0)</span>), iv) 2003 – 2013 (<span>(A<0)</span>), and v) 2014 – 2022 (<span>(A>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}

引用次数: 0

The Properties of Non-Potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares 具有复杂结构和强太阳耀斑的超活跃区非势磁场参数的性质

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-07 DOI: 10.1007/s11207-025-02456-6

S. Liu, Shahid Idrees, D. Liu, S. G. Zeng

{"title":"The Properties of Non-Potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares","authors":"S. Liu, Shahid Idrees, D. Liu, 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}

引用次数: 0

Direct Measurement of the Longitudinal Magnetic Field in the Solar Photosphere with the Zeeman Effect 利用泽曼效应直接测量太阳光层的纵向磁场

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-04 DOI: 10.1007/s11207-025-02455-7

Jie Chen, Jiangtao Su, Wenbin Xie, Yuanyong Deng, Xianyong Bai, Ziyao Hu, Haiqing Xu, Suo Liu, Yin Zhang, Yingzi Sun, Yongliang Song, Xiaofan Wang

引用次数: 0

On Field Line Slippage Rates in the Solar Corona 日冕中的现场线路滑移率

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-04 DOI: 10.1007/s11207-025-02462-8

David MacTaggart

{"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}

引用次数: 0

Turbulence Evolution Between 0.5 and 1 AU for the Solar Wind of Various Origins 不同来源太阳风在0.5 - 1au间的湍流演化

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-03 DOI: 10.1007/s11207-025-02458-4

Liudmila Rakhmanova, Maria Riazantseva, Yuri Yermolaev, Alexander Khokhlachev, Georgy Zastenker

引用次数: 0

Improved Tomographic Reconstruction of 3D Global Coronal Density from STEREO/COR1 Observations 基于STEREO/COR1观测的三维全球日冕密度改进层析重建

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-03 DOI: 10.1007/s11207-025-02454-8

Tongjiang Wang, C. Nick Arge, Shaela I. Jones

{"title":"Improved Tomographic Reconstruction of 3D Global Coronal Density from STEREO/COR1 Observations","authors":"Tongjiang Wang, C. Nick Arge, Shaela I. Jones","doi":"10.1007/s11207-025-02454-8","DOIUrl":"10.1007/s11207-025-02454-8","url":null,"abstract":"<div><p>Tomography is a powerful technique for recovering the three-dimensional (3D) density structure of the global solar corona. In this work, we present an improved tomography method by introducing radial weighting in the regularization term. Radial weighting provides balanced smoothing of density values across different heights, helping to recover finer structures at lower heights while also stabilizing the solution and preventing oscillatory artifacts at higher altitudes. We apply this technique to reconstruct the 3D electron density of Carrington Rotation (CR) 2098 using two weeks of polarized brightness (pB) observations from the inner coronagraph (COR1) on board spacecraft-B of the twin Solar Terrestrial Relations Observatory (STEREO), where the radial weighting function is taken as the inverse intensity background, calculated by averaging all the pB images used. Comparisons between density distributions at various heights from the tomography and magnetohydrodynamics (MHD) simulations show good agreement. We find that radial weighting not only effectively corrects the oversmoothing effect near the inner boundary in reconstructions using second-order smoothing but also significantly improves reconstruction quality when using zero-order smoothing. Additionally, comparing reconstructions for CR 2091 from single-satellite data with that from multiviewpoint data suggests that coronal evolution and dynamics may significantly impact on the reconstructed density structures. This improved tomography method has been used to create a database of 3D densities for CRs 2052 to 2154, based on STEREO/COR1-B data, covering the period from 08 January 2007 to 17 September 2014.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143761772","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

A Study on the Transition-Range Spectral Index of the Solar Wind Turbulence in the Inner Heliosphere 内日光层太阳风湍流的过渡范围光谱指数研究

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-03 DOI: 10.1007/s11207-025-02439-7

Haifeng Yang, Guoqing Zhao, Hengqiang Feng, Liang Xiang

{"title":"A Study on the Transition-Range Spectral Index of the Solar Wind Turbulence in the Inner Heliosphere","authors":"Haifeng Yang, Guoqing Zhao, Hengqiang Feng, Liang Xiang","doi":"10.1007/s11207-025-02439-7","DOIUrl":"10.1007/s11207-025-02439-7","url":null,"abstract":"<div><p>Based on observations from Parker Solar Probe, this paper studies the dependence of the correlations between the transition-range spectral index of the magnetic energy spectrum and four parameters (inertial-range cross-helicity and magnetic energy density, transition-range magnetic helicity, and bulk proton temperature) on solar wind speed and heliocentric distance. Results show significant correlations between the spectral index and both cross-helicity and magnetic energy density. Notably, at lower speeds or closer distances, the correlation coefficient (CC) between the cross-helicity and spectral index is smaller than that between the magnetic energy density and spectral index. Conversely, at higher speeds or greater distances, the correlation with cross-helicity becomes comparable to or even exceeds that with magnetic energy density. Additionally, as the speed increases or the heliocentric distance decreases, cross-helicity, magnetic energy density, proton temperature, and the absolute values of the spectral index show a mostly upward trend. Moreover, cross-helicity, absolute values of the spectral index, and CC between the magnetic energy density and spectral index exhibit a similar trend with the speed, initially rising and then declining at the highest speed bin. We discuss the results using the recently proposed “helicity barrier” effect.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143761709","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

Coronal Electric Currents and Kink Instability of Magnetic Flux Rope 磁通绳的日冕电流与扭结不稳定性

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-03 DOI: 10.1007/s11207-025-02461-9

Yuriy T. Tsap, Alexander V. Stepanov, Yulia G. Kopylova

{"title":"Coronal Electric Currents and Kink Instability of Magnetic Flux Rope","authors":"Yuriy T. Tsap, Alexander V. Stepanov, Yulia G. Kopylova","doi":"10.1007/s11207-025-02461-9","DOIUrl":"10.1007/s11207-025-02461-9","url":null,"abstract":"<div><p>Using the energy method and the thin magnetic flux tube approximation, we find the wave dispersion relation for magnetohydrodynamic kink oscillations of a force-free magnetic flux rope with uncompensated longitudinal electric current under solar coronal conditions. The eigenvectors are shown to impose restrictions on the conditions of the kink instability of a flux rope. The observed weak twist of coronal loops with a small (<span>(lesssim 1)</span>) number of turns of the magnetic field lines around the axis indicates the dominance of unshielded magnetic flux ropes in the corona of the Sun, in which the longitudinal electric currents do not exceed <span>(10^{11})</span> – <span>(10^{12})</span> A. These restrictions can be associated with the absence of solar superflares. The period of kink oscillations of twisted coronal loops should decrease with decreasing longitudinal electric current, which can be used to study its dynamics in solar flares. No dependence of compact and eruptive solar flares on the twist of flux ropes can be explained by the coexistence of both shielded and unshielded electric currents in the corona.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143761706","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

Turbulent Power: A Discriminator Between Sheaths and CMEs 湍流功率：鞘层和日冕物质抛射的鉴别器

IF 2.7 3区物理与天体物理

Solar Physics Pub Date : 2025-04-03 DOI: 10.1007/s11207-025-02457-5

Deep Ghuge, Debesh Bhattacharjee, Prasad Subramanian

引用次数: 0