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太阳辐射/对流区域边界处的碳、氮、氧元素的电子碰撞电离研究 认领 引用
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作者 侯永 罗青波 +2 位作者 梁欣 曾交龙 袁建民 《物理学报》 SCIE EI CAS CSCD 北大核心 2026年第1期220-230,共11页
太阳辐射层与对流层边界区域T≈180eV,ne≈9×1022cm-3,是太阳内部能量传输方式从辐射主导向对流主导转变的关键界面,也是研究高温稠密等离子体物理的天然实验室.这一区域的物理特性决定了恒星演化模型的可靠性与能量传输机... 太阳辐射层与对流层边界区域T≈180eV,ne≈9×1022cm-3,是太阳内部能量传输方式从辐射主导向对流主导转变的关键界面,也是研究高温稠密等离子体物理的天然实验室.这一区域的物理特性决定了恒星演化模型的可靠性与能量传输机制的稳定性,特别是高温稠密等离子体中强烈的碰撞电离会改变电子数密度分布,进而影响能量的输运过程.本文发展了一种耦合等离子体环境效应来计算原子结构的新方法:通过将计算原子结构的Flexible Atomic Code (FAC)与超网链(hypernetted-chain, HNC)近似相结合,在原子波函数计算中引入电子-电子、电子-离子关联函数来考虑等离子体中屏蔽效应,系统研究了极端条件下电子碰撞电离的物理机制.基于扭曲波近似的计算表明,考虑等离子体环境效应时,碳、氮和氧元素的电子碰撞电离截面较自由原子模型显著增强,同时电离阈值出现明显下降的现象.研究发现这种增强效应主要源于离子间强耦合导致的原子势场重叠和自由电子屏蔽引起的束缚态能级移动.本研究直接将离子结构引入电子结构计算的哈密顿量中,所获得的电离参数可直接用于改进太阳内部辐射输运模型,为惯性约束聚变等极端条件等离子体研究提供了理论支持. 展开更多
关键词 辐射/对流区域边界 环境效应 电子碰撞电离 超网链近似
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Half-year Evolution of a Decaying Solar Active Region and Peripheral Dimming Regions 认领 引用
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作者 Jiasheng Wang Yu Xu Zhenyong Hou 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第7期181-191,共11页
Using multi-wavelength observations from the Solar Dynamics Observatory,we investigated the six-month decay process of the solar active region(AR)NOAA AR 12738 from 2019 April to October.We systematically analyzed the... Using multi-wavelength observations from the Solar Dynamics Observatory,we investigated the six-month decay process of the solar active region(AR)NOAA AR 12738 from 2019 April to October.We systematically analyzed the region’s evolution by examining extreme ultraviolet intensity variations,quantifying magnetic flux diffusion,and investigating thermodynamic changes via Differential Emission Measure(DEM)analysis.This study presents the first long-term tracking of a peripheral dimming region(dark moat),revealing its continuous areal decrease over time.DEM results reveal cooling plasma signatures and thermal restructuring,with the dimming region exhibiting a distinct temperature deficit in the range 105.5–105.9 K.Potential field extrapolation identifies two dominant magnetic configurations:low-lying loops with cool plasma(105.8 K),consequently lacking plasma at the typical 105.8 K formation temperature.The thermal deficit,not just the absence of material,is the key driver of the reduced emission.Our results demonstrate that long-duration dimming provides a valuable diagnostic for understanding AR decay,thermal evolution,and coronal magnetic restructuring. 展开更多
关键词 Sun:corona Sun:evolution Sun:magnetic fields Sun:filaments,prominences
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Erratum:“Data-driven Simulations of Magnetic Field Evolution in Active Region 11429:Magneto-frictional Method Using PENCIL CODE”(2024,RAA,24,025007) 认领 引用
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作者 P.Vemareddy Jön Warnecke Ph.A.Bourdin 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第3期293-293,共1页
On page 6,Figure 3 is a duplicate of Figure 4.We publish below the correct figure,sincerely apologizing to the authors.
关键词 magnetic field evolution magneto frictional method pencil code erratum figure duplication apology active region
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基于SDO/AIA紫外图像的太阳较差自转研究 认领 引用
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作者 曾曙光 金汉乐 +5 位作者 邓林华 吴前锐 曾祥云 郑胜 黄瑶 刘德剑 《天文学报》 CAS CSCD 北大核心 2026年第1期43-52,共10页
太阳的较差自转是将极向磁场转化为环向磁场的关键机制.采用通量调制法对太阳动力学观测台(Solar Dynamics Observatory,SDO)上大气成像仪(Atmospheric Imaging Assembly,AIA)的1600Å等波段的太阳全日面紫外图像进行了较差自转研究... 太阳的较差自转是将极向磁场转化为环向磁场的关键机制.采用通量调制法对太阳动力学观测台(Solar Dynamics Observatory,SDO)上大气成像仪(Atmospheric Imaging Assembly,AIA)的1600Å等波段的太阳全日面紫外图像进行了较差自转研究.首先,对全日面图像进行了预处理并将其划分为不同的纬度区域.然后,经过数据处理得到各纬度区域的通量时间序列.最后,对各纬度区域通量时间序列进行自相关分析以得到各纬度的自转周期和自转角速度.研究结果表明:在80°S到80°N的纬度范围内,太阳的自转角速度是关于纬度变化的函数;在AIA不同波长下,随着高度增加太阳赤道自转角速度变大,而较差自转程度减弱;赤道附近平均自转角速度及较差自转程度与太阳活动周无明显关系. 展开更多
关键词 太阳 自转 太阳 活动 太阳 紫外辐射 方法 数据分析 自相关
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Magnetic Field Measurements in the Solar Chromosphere Using the Hβ4861A Line.I.Forward Modeling Based on 1D Models 认领 引用
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作者 Jiasheng Wang Wenxian Li +3 位作者 Xianyong Bai Yingzi Sun Yuanyong Deng Jiaben Lin 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第7期59-70,共12页
The chromosphere is a complex solar atmosphere that hosts a variety of transients and transports significant free energy to heat the corona.However,due to the limited sensitivity of polarization measurement and the in... The chromosphere is a complex solar atmosphere that hosts a variety of transients and transports significant free energy to heat the corona.However,due to the limited sensitivity of polarization measurement and the influence of spectral line broadening,the basic magnetic field configuration in the chromosphere has not yet been fully revealed to correspond to the observed phenomena.In this work,we investigated the validity and application of the magnetic field inversion method for the Hβ4861A spectral line with non-local thermodynamic equilibrium(non-LTE)approximations.The formation height of the Hβline center in the chromosphere is 1100–1300 km(log τ_(500 nm)=[−4.86,−5.00])in quiet Sun(QS)and 300—410 km(log τ_(500 nm)=[−2.41,−4.57])in sunspots.We generated synthetic spectra by incorporating magnetic fields into semi-empirical Fontenla-Avrett-Loeser(FAL)models for QS and sunspots,and then performed inversions to obtain the magnetic fields,which were then compared with the magnetic fields in the models.In addition,we evaluated the accuracy of the magnetic fields obtained using the weak-field approximation(WFA)and the impact of using these WFA results as the initial guess model for non-LTE inversion on the final results.Our work validates the effectiveness of the inversion method for the measurement of line-of-sight(LOS)magnetic field components,which significantly improved the accuracy in both weak field(0—500 G)and strong field(>2000 G)regions,while maintaining accuracy in the intermediate field range of 500—2000 G.This demonstrates that the inversion techniques we employed are capable of resolving Zeeman-sensitive spectral lines in the chromosphere,which can be applied to the Hβobservational data from the new generation Solar Full-disk Multi-layer Magnetograph at GanYu Solar Station to provide full disk chromospheric magnetic field information. 展开更多
关键词 Sun:chromosphere Sun:magnetic fields (Sun:)sunspots polarization techniques:polarimetric
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First Time Observed M-shaped Coronal Mass Ejection Associated with a Blowout Jet and an Extreme Ultraviolet Wave 认领 引用
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作者 Yu-Hu Miao Lin-Hua Deng +8 位作者 Chao-Wei Jiang Abouazza Elmhamdi Jiang-Tao Su Ming-Xiang Guan Hai-Xin Zou Jiao-Man Li Xue-Mei Cao Jun-Tao Wang Yun-Zhi Hua 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第3期63-72,共10页
The coronal blowout jet,extreme ultraviolet(EUV)wave and coronal mass ejection(CME)are common phenomena in the solar atmosphere.In this paper,we report the occurrence of an M-shaped CME event associated with a blowout... The coronal blowout jet,extreme ultraviolet(EUV)wave and coronal mass ejection(CME)are common phenomena in the solar atmosphere.In this paper,we report the occurrence of an M-shaped CME event associated with a blowout jet and an EUV wave using high-resolution,multi-angle and multi-wavelength observations taken from Solar Dynamics Observatory,and Solar TErrestrial RElations Observatory.Interestingly,and for the first time,it is found that two bubble-like CMEs and a jet-like CME were simultaneously triggered by the same eruptive event.Our observational analyses and findings indicate the following:(1)the eruption of a blowout jet led to a large-scale EUV wave;(2)the eruption of the EUV wave swept a small filament(prominence)and a long filament;(3)eventually the EUV wave split-up into two parts,leading to the two bubble-like CMEs,while the blowout jet induced a jet-like CME.The combined events appear to form an M-shape like structure CME,that we sketch throughout a proposed cartoon tentatively explaining the observed complex configuration.Based on observational diagnosis,we argue that the jet,the EUV wave and the multi-CME are highly interlinked.A suggested eruption-model,from the solar atmosphere to the space,is outlined and discussed,providing a possibly new way to probe the relationship between the solar eruptions and the surrounding space.The investigation of such a rare phenomenon can be a key point for better understanding of the physical associated triggering mechanisms and energy transport in the solar atmosphere,crucial for MHD simulations and modeling. 展开更多
关键词 magnetohydrodynamics(MHD)-(Sun) solar-terrestrial relations-shock waves-Sun coronal mass ejections(CMEs)
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Observations of Weak Magnetic Fields in the Solar Chromosphere with Two He I Lines 认领 引用
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作者 Deqing Ren David Faulkner Katzíguez Damian J.Christian 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第1期70-85,共16页
Solar magnetic fields are responsible for solar coronal mass ejections and other eruptive phenomena that govern space weather.Today,most of our knowledge about the solar magnetic field topologies was derived from the ... Solar magnetic fields are responsible for solar coronal mass ejections and other eruptive phenomena that govern space weather.Today,most of our knowledge about the solar magnetic field topologies was derived from the measurements of the magnetic field of the solar photosphere.The solar chromosphere is dilute,and associated magnetic fields are weak,which makes them difficult to measure.To address this challenging issue,we propose the use of the He I D35876?line,together with the He I 10830?line,to measure the off-limb weak and moderate chromospheric magnetic fields in the Hanle effect regime.We show that the current approach of using the polarization amplitude or degree cannot reliably retrieve the magnetic fields.We demonstrated that by using the Stokes linear polarization profiles simultaneously with the 5876 and 10830?lines,without the use of the circular polarization,chromospheric magnetic fields as low as and down to a few gauss can be measured easily and reliably with today's instruments.We further demonstrate the potential to measure the weak chromospheric magnetic fields with the Stokes linear polarization profiles by using the He 5876?line alone,which has not been fully investigated yet.This work will provide a new technique for future daily synoptic observations for the weak magnetic fields in the solar chromosphere for both the active and quiescent regions,which are still difficult to measure. 展开更多
关键词 Sun magnetic fields-Sun chromosphere-methods observational
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莱曼阿尔法太阳耀斑事件标准数据集 认领 引用
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作者 卢磊 封莉 黎辉 《空间科学学报》 CAS CSCD 北大核心 2026年第1期247-253,共7页
太阳耀斑是太阳大气中最强烈的爆发现象,能够释放大量能量并产生各种波长的电磁辐射.研究太阳耀斑对于理解太阳活动、空间天气预报以及保护地球空间环境至关重要.本数据集基于夸父一号(ASO-S)卫星搭载的全日面成像仪(Solar Disk Imager,... 太阳耀斑是太阳大气中最强烈的爆发现象,能够释放大量能量并产生各种波长的电磁辐射.研究太阳耀斑对于理解太阳活动、空间天气预报以及保护地球空间环境至关重要.本数据集基于夸父一号(ASO-S)卫星搭载的全日面成像仪(Solar Disk Imager, SDI)在莱曼阿尔法波段(121.6±7.5) nm采集的全日面图像数据,通过一套自主研发的太阳耀斑自动识别与关键参数提取算法,系统记录了2024年莱曼阿尔法太阳耀斑事件.该算法可有效避免宇宙线、粒子暴等事件的干扰,能够对不同强度级别的耀斑进行识别,并能对日面上同时发生的多个耀斑进行分别识别与追踪.本数据集收录了耀斑的起止时间、持续时间、发生位置、显著性等关键参数,包含耀斑识别过程记录文档、耀斑事件列表、耀斑峰值时刻快视图像和耀斑区域电影动画等数据.该数据集可为太阳物理学研究、空间天气预报以及相关领域提供重要的科学数据支持. 展开更多
关键词 太阳耀斑 莱曼阿尔法 空间天气 自动识别
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Statistical study of ICMEs and their geoeffectiveness during the rising phases of Solar Cycles 23,24,and 25 认领 引用
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作者 XinYue Chen ChengLong Shen +5 位作者 YuTian Chi DongWei Mao ZhiYong Zhang JunYan Liu ChenXi Zhai YuMing Wang 《Earth and Planetary Physics》 EI CSCD 2026年第4期592-604,共13页
As Solar Cycle 25 appears to approach the declining phase,to objectively evaluate the activity intensity during its rising phase and conduct a comparative analysis,we extend the catalog of Interplanetary Coronal Mass ... As Solar Cycle 25 appears to approach the declining phase,to objectively evaluate the activity intensity during its rising phase and conduct a comparative analysis,we extend the catalog of Interplanetary Coronal Mass Ejections(ICMEs)from 2016 to 2025.Subsequently,we systematically compare and analyze the parameter characteristics and geoeffectiveness of ICMEs during the rising phase of Solar Cycle 25 with those of the previous two solar cycles.Overall,from 1995 to 2025,we identify 657 ICME events,which are classified into 530 groups and are associated with a total of 325 geomagnetic storms,including 103 intense geomagnetic storms.The annual occurrence frequencies of ICMEs,the number of ICME groups and their associated geomagnetic storms are largely synchronized with the variations in sunspot numbers.The sunspot numbers during the rising phase of Solar Cycle 25 are comparable to those of Solar Cycle 23 and clearly higher than those of Solar Cycle 24.Compared with the previous two solar cycles,Solar Cycle 25 exhibits the smallest number of ICMEs during its rising phase.The numbers of geomagnetic storms and intense geomagnetic storms during this period fall between those of the two preceding cycles,consistent with the overall variation in solar activity.Although the number of intense geomagnetic storms during the rising phase of Solar Cycle 25 is relatively small,their intensities are remarkably high,with several extremely intense storm events observed.During the rising phase of Solar Cycle 25,the average values of the magnetic field strength,southward magnetic field component,and dawn–dusk electric field of ICMEs are the highest among the three periods.They are key parameters influencing the geoeffectiveness of ICMEs.Overall,the geoeffectiveness of ICMEs during the rising phase of Solar Cycle 25 is intermediate between those of the previous two cycles. 展开更多
关键词 Interplanetary Coronal Mass Ejections geomagnetic storms geoeffectiveness
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The Split Janus-faced Sun:Magnetic Rhythm and Duality in the Solar Cycle 认领 引用
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作者 Weiqi Chen Kejun Li Jingchen Xu 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第6期165-173,共9页
The solar cycle—most notably characterized by its sunspot activity patterns—serves as a cornerstone of heliospheric physics.This research uncovers a fundamental magnetic dichotomy in the Sun's full-disk field,id... The solar cycle—most notably characterized by its sunspot activity patterns—serves as a cornerstone of heliospheric physics.This research uncovers a fundamental magnetic dichotomy in the Sun's full-disk field,identifying two functionally separate populations:the strong magnetic field group(SG)and weak magnetic field group(WG).The solar cycle exhibits a dual nature,much like Janus,with the SG and WG operating in opposing phases regardless of low or high latitudes.The SG-dominated cycle represents one facet of this duality and is visually prominent at the solar surface.It is well-established that this component synchronizes with the sunspot cycle at low latitudes but operates in anti-phase at high latitudes.In contrast,the WG-driven cycle acts as its hidden counterpart,functioning in opposition to the SG at both high and low latitudes—a behavior that had not been identified until now.Influenced by these magnetic field groups,this dual nature permeates the entire solar atmosphere,revealing that the full-disk solar activity is globally modulated by the Janus cycle. 展开更多
关键词 Sun:magnetic fields Sun:activity Sun:atmosphere
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中国空间探日的新征程与新使命 认领 引用
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作者 汪景琇 《人民论坛·学术前沿》 CSSCI 北大核心 2026年第8期56-63,共8页
太阳是迄今唯一一颗能够被人类详细观测的恒星,太阳活动是影响人类生存环境的空间天气的源头。太阳影响地球气候和环境长期变化的程度与应对之策,是意义重大且至今争议未决的重要科学问题。因而,太阳物理学研究具有显著的科学价值和紧... 太阳是迄今唯一一颗能够被人类详细观测的恒星,太阳活动是影响人类生存环境的空间天气的源头。太阳影响地球气候和环境长期变化的程度与应对之策,是意义重大且至今争议未决的重要科学问题。因而,太阳物理学研究具有显著的科学价值和紧迫性。近年来,在太阳空间立体探测方面,我国学者提出一系列具有高度前瞻性和战略性的设想和计划。实践中,我国的空间太阳探测开始的时间较晚,“羲和号”与“夸父一号”的成功发射,标志着中国在太阳探测领域迈出重要步伐。完成“羲和二号”和“夸父二号”空间探日项目,是“十五五”期间的重要工作任务。未来,应确立清晰的发展思路,仰望星空、脚踏实地,一步一个脚印开启星际探测新征程。 展开更多
关键词 太阳物理 空间探测 探日工程 “十五五”规划
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相邻暗条之间磁重联触发的重复双向喷流 认领 引用
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作者 孟妮 梁红飞 周新平 《天文学报》 CAS CSCD 北大核心 2026年第4期111-117,共7页
利用太阳动力学天文台(Solar Dynamics Observatory,SDO)的高时间分辨率和高空间分辨率观测数据,对一组在同一源区内重复发生的双向喷流事件进行了详细分析.研究结果表明,该喷流的产生与两个小尺度、相邻暗条之间的相互作用以及喷流源... 利用太阳动力学天文台(Solar Dynamics Observatory,SDO)的高时间分辨率和高空间分辨率观测数据,对一组在同一源区内重复发生的双向喷流事件进行了详细分析.研究结果表明,该喷流的产生与两个小尺度、相邻暗条之间的相互作用以及喷流源区的磁重联过程密切相关.观测显示,这两个暗条的相邻末端分别扎根于源区内相反的磁极中.当暗条逐渐靠近时,其交互区域出现明显的增亮斑块.随后,一对高温等离子体喷流沿着两条丝状结构向相反方向运动,呈现典型的双向喷流特征.综合分析结果表明,观测到的这些双向喷流事件具有明显的重复发生特征,其形成机制与近期提出的相邻暗条之间磁重联模型一致.该机制区别于传统认为双向喷流主要由新浮现双极磁场与上覆水平磁场磁重联所触发的情形. 展开更多
关键词 太阳 喷流 太阳 暗条 太阳 日冕 磁重联 等离子体
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The Relationship between Characteristics of Gradual Solar Energetic Particle Events and their Event-integrated Fe/O Ratios 认领 引用
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作者 Zhuo-Rui Wang Liu-Guan Ding +1 位作者 Bin Gu Huan-Zhi Yuan 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第5期116-126,共11页
Based on multiple-spacecraft observations, we select 157 gradual solar energetic particle (SEP) events spanningfrom 2007 January to 2017 October. These SEP events are classified into Fe-rich and Fe-poor events inaccor... Based on multiple-spacecraft observations, we select 157 gradual solar energetic particle (SEP) events spanningfrom 2007 January to 2017 October. These SEP events are classified into Fe-rich and Fe-poor events inaccordance with their event-integrated Fe/O ratio (relative to the coronal reference value of 0.131). A comparative analysis is performed to investigate the correlationship between SEP properties and the associatedsolar eruptions for these two classes of events, aiming to reveal the impacts of different seed populations on SEPevents. The main conclusions are as follows: (1) Fe-rich events are generally associated with coronal massejections (CMEs) that have lower speed, mass, kinetic energy, and lower-class flares, along with lower peakfluxes, in comparison to Fe-poor events. Moreover, there is no significant correlation between the peak intensitiesof Fe-rich events and CME speeds. In contrast, the peak intensities of Fe-poor events exhibit a strong positivecorrelation with CME speeds, and they encompass nearly all (96%) extremely large SEP events. (2) The pre-CMEs (preceding CMEs occurring within 24 hr prior to the primary CME associated with SEP event) associatedwith both Fe-rich and Fe-poor events show no significant difference. However, the occurrence rate of Fe-richevents slightly increases with more frequent pre-CME eruptions. The occurrence rates of the two classes of SEPevents associated with different type-Ⅱ radio bursts exhibit distinct differences: the occurrence rate of Fe-richevents decreases progressively from the metric (m), to the decameter-hectometric (DH), and then to the kilometric(km) wavebands. This may imply that the dominant seed particles accelerated by the shock have undergonechanges at different altitudes, for instance, from flare materials with a high Fe/O ratio to coronal/solar windmaterials with a low Fe/O ratio. (3) The two classes of SEP events display distinct longitudinal distributions andeast-west asymmetries. The occurrence rate of Fe-rich events reaches their maxima within the relativelongitudinal range of 30°–90° indicating the degrees of the source westward of the magnetic footpoint, which isparticularly pronounced in the case of medium- or low-speed CMEs. At various relative longitudes, the peakintensities of the two classes of SEP events also show statistically significant differences, with the Fe-poor eventtypically exhibiting a notably higher intensity compared to the Fe-rich event. 展开更多
关键词 Sun particle emission-Sun abundances-Sun activity
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Are spicules driven by oscillations? 认领 引用
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作者 ChuXin Chen 《Earth and Planetary Physics》 EI CSCD 2026年第3期438-446,共9页
The formation of spicules on the solar surface is poorly understood.In the present investigation,we propose a mechanism that provides an explanation for this phenomenon.The squeeze of the enhanced downflow region in t... The formation of spicules on the solar surface is poorly understood.In the present investigation,we propose a mechanism that provides an explanation for this phenomenon.The squeeze of the enhanced downflow region in the intergranular lanes by oscillation results in an initial narrow,high-speed upward flow with a velocity on the order of several kilometers per second and a width on the order of 10 km.The underlying physics principle is the same as in the design of an anti-tank weapon,called a“shaped charge”.The life of a spicule is divided into two stages.The first stage is mechanical driving by the pressure gradient at its base;the second stage is electromagnetic driving.Dynamo action in the early lifetime of a spicule plays an important role in the transfer of mechanical energy to magnetic energy.The subsequent Fermi acceleration is responsible for the energy transfer from magnetic energy to thermal energy and kinetic energy.Depending on the strength of the ambient magnetic field,the formation of type I spicules(strong case)and typeⅡspicules(weak case)can be naturally explained in this frame setting,which is one of the merits of our proposed mechanism.The variation in temperature along the height is consistent with prior observation-based models. 展开更多
关键词 spicule formation shaped charge initial narrow,high-speed upward flow Fermi acceleration of charged particles
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Periodicities in Solar Microwave Emission During Solar Cycles 20-24 认领 引用
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作者 Mahender Aroori Vivek Reddy Pininti 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第7期85-99,共15页
We present a detailed time-series analysis of solar radio flux at five discrete frequencies 1.0,2.0,3.75,9.4,and 17 GHz and daily sunspot numbers(SSNs)spanning Solar Cycles 20 to 24,using the Fast Fourier Transform,L... We present a detailed time-series analysis of solar radio flux at five discrete frequencies 1.0,2.0,3.75,9.4,and 17 GHz and daily sunspot numbers(SSNs)spanning Solar Cycles 20 to 24,using the Fast Fourier Transform,Lomb–Scargle periodogram,and Wavelet techniques.These complementary methods identify persistent and transient periodicities by integrating global spectral estimation,reliable detection in unevenly sampled data,and time–frequency localization,enabling a comprehensive characterization of solar activity across different atmospheric layers.Our results reveal that radio fluxes at 2.0 GHz and 2.8 GHz exhibit the strongest correlation with SSN,indicating their close association with active-region dynamics and magnetic field concentrations.In contrast,emissions at 17 GHz show minimal correlation with SSN,suggesting an origin in distinct,possibly nonthermal,coronal processes.Prominent rotational periodicities in the range of 26–31 days are consistently detected in the SSN and lower-frequency fluxes,but are largely absent in the 17 GHz band.Cycle-wise analysis highlights Solar Cycle 21 as the most active,with the highest number of statistically significant periodic components.These findings underscore the utility of multi-frequency radio observations combined with advanced spectral techniques in revealing the complex,cycle-dependent nature of solar magnetic activity. 展开更多
关键词 Sun:atmosphere Sun:radio radiation The Sun Sun:corona
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太阳爆发与空间天气研究进展 认领 引用
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作者 申远灯 谭宋 欧雨迪 《四川师范大学学报（自然科学版）》 CAS 2026年第3期388-412,共25页
太阳爆发活动(主要包括耀斑与日冕物质抛射)是太阳系内规模最大的瞬态能量释放过程,也是驱动灾害性空间天气的物理源头.以“太阳源区触发-行星际传输演化-近地空间响应”这一完整的因果链条为主线,系统评述该领域的研究现状与范式演进.... 太阳爆发活动(主要包括耀斑与日冕物质抛射)是太阳系内规模最大的瞬态能量释放过程,也是驱动灾害性空间天气的物理源头.以“太阳源区触发-行星际传输演化-近地空间响应”这一完整的因果链条为主线,系统评述该领域的研究现状与范式演进.在源区触发阶段,重点综述磁重联作为终极引擎的确立过程,以及磁通量绳从理论争议到多波段成像确证的跨越,并剖析理想磁流体不稳定性与非理想磁重联在灾变起始中的动力学博弈.在行星际传输阶段,阐述日冕物质抛射与动态、磁化太阳风环境的复杂相互作用,分析背景太阳风的动力学阻曳效应以及最新发现的磁场折返等微观结构对行星际媒介认知的重塑,并详述激波驱动的高能粒子加速机制与扩散路径模型.在近地响应阶段,系统论述爆发能量在地球磁层、热层及电离层中的层级耗散与耦合机制,解析南向磁场触发的能量注入路径,以及由此引发的热层径向膨胀、电离层不均匀体闪烁和地磁感应电流等物理过程.结合近年典型灾害空间天气案例,揭示现代技术文明在空间环境演变面前的系统性脆弱.针对预报瓶颈,梳理从经验统计到物理驱动数值模型,再到人工智能全链条数字孪生的范式更迭,并展望通过立体探测网构建日地全景数字孪生预报体系的科学蓝图. 展开更多
关键词 太阳爆发 空间天气 日冕物质抛射 磁重联 数字孪生
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Forecasting solar cycles using the time-series dense encoder deep learning model 认领 引用
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作者 Cui Zhao Shangbin Yang +1 位作者 Jianguo Liu Shiyuan Liu 《Astronomical Techniques and Instruments》 CSCD 2026年第1期43-54,共12页
The solar cycle(SC),a phenomenon caused by the quasi-periodic regular activities in the Sun,occurs approximately every 11 years.Intense solar activity can disrupt the Earth’s ionosphere,affecting communication and na... The solar cycle(SC),a phenomenon caused by the quasi-periodic regular activities in the Sun,occurs approximately every 11 years.Intense solar activity can disrupt the Earth’s ionosphere,affecting communication and navigation systems.Consequently,accurately predicting the intensity of the SC holds great significance,but predicting the SC involves a long-term time series,and many existing time series forecasting methods have fallen short in terms of accuracy and efficiency.The Time-series Dense Encoder model is a deep learning solution tailored for long time series prediction.Based on a multi-layer perceptron structure,it outperforms the best previously existing models in accuracy,while being efficiently trainable on general datasets.We propose a method based on this model for SC forecasting.Using a trained model,we predict the test set from SC 19 to SC 25 with an average mean absolute percentage error of 32.02,root mean square error of 30.3,mean absolute error of 23.32,and R2(coefficient of determination)of 0.76,outperforming other deep learning models in terms of accuracy and training efficiency on sunspot number datasets.Subsequently,we use it to predict the peaks of SC 25 and SC 26.For SC 25,the peak time has ended,but a stronger peak is predicted for SC 26,of 199.3,within a range of 170.8-221.9,projected to occur during April 2034. 展开更多
关键词 Solar cycle Forecasting TiDE Deep learning
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Optical Continuum Light Curves and Bolometric Energy Estimates of Solar White-light Flares 认领 引用
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作者 Yingjie Cai Yijun Hou +2 位作者 Hengkai Ding Ting Li Jifeng Liu 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2026年第4期9-17,共9页
Solar white-light flares(WLFs)are solar flares exhibiting enhanced emission in the optical continuum.They are critical for understanding energy release and transport mechanisms in solar flares and for conducting compa... Solar white-light flares(WLFs)are solar flares exhibiting enhanced emission in the optical continuum.They are critical for understanding energy release and transport mechanisms in solar flares and for conducting comparative studies with stellar WLFs.However,the scarcity of accurately and reliably measured optical continuum light curves for solar WLFs significantly hampers related studies.Based on the optimized solar WLF identification method,we construct a dataset of optical continuum light curves for 70 solar WLFs using 6173 A continuum intensity images from the Solar Dynamics Observatory.Moreover,for each solar WLF event,we also provide the location of the white-light emission enhancement signals and key parameters including bolometric energies and durations derived from both the traditional fixed-temperature blackbody model and the refined variabletemperature blackbody model.This dataset will serve as a valuable resource for future statistical investigations of solar WLFs and for comparative studies between solar and stellar flares. 展开更多
关键词 Sun flares-Sun activity-Sun atmosphere-methods data analysis
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基于相位编组与多级阈值的太阳射电Ⅲ型暴自动检测算法 认领 引用
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作者 张洪瑞 董亮 +6 位作者 何乐生 黄文耿 王晶 ZAINAL ABIDIN Zamri Bin 杨凤辉 RAZAK Dalilah Nur Fathiah Bintin Hanim 高冠男 《空间科学学报》 CAS CSCD 北大核心 2026年第3期592-603,共12页
太阳射电Ⅲ型暴是太阳活动中最为常见的射电爆发类型之一,其具有快速频率漂移等特征,是耀斑爆发和日冕物质抛射等太阳活动事件的示踪器.现有的识别方法面临连续爆发检测能力弱、小样本学习不足等问题,导致误检率高和召回率低.针对这些缺... 太阳射电Ⅲ型暴是太阳活动中最为常见的射电爆发类型之一,其具有快速频率漂移等特征,是耀斑爆发和日冕物质抛射等太阳活动事件的示踪器.现有的识别方法面临连续爆发检测能力弱、小样本学习不足等问题,导致误检率高和召回率低.针对这些缺陷,提出一种基于相位编组法的自适应轮廓检测算法,该方法融合灰度梯度相位信息与多级阈值过滤,通过形态学操作拟合太阳射电Ⅲ型暴频谱轮廓,实现对太阳射电Ⅲ型暴频谱的自动识别,通过计算对应的爆发起止时间、爆发起止频率、频率漂移率等有效信息,对海量频谱观测数据进行快速批量识别与分析.基于云南天文台澄江米波太阳射电望远镜的观测数据集开展应用,经检验,该方法在识别太阳射电Ⅲ型暴上实现了93.5%的召回率. 展开更多
关键词 太阳射电Ⅲ型暴 相位编组法 多级阈值 形态学 自动识别
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基于改进YOLOv8的太阳黑子自动识别 认领 引用
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作者 南旭东 王瑞 +4 位作者 牛思博 赵志军 班梦威 陈小改 刘钟燕 《应用光学》 CAS 北大核心 2026年第4期794-800,共7页
随着众多地面和空间太阳望远镜的投入使用,产生了大量的太阳图像数据。基于光球图像的太阳活动区实测研究是一个重要话题,例如,太阳黑子的形成与演化问题、黑子旋转以及动力传输问题等,这些都需要对太阳黑子进行大量的统计分析。因此,... 随着众多地面和空间太阳望远镜的投入使用,产生了大量的太阳图像数据。基于光球图像的太阳活动区实测研究是一个重要话题,例如,太阳黑子的形成与演化问题、黑子旋转以及动力传输问题等,这些都需要对太阳黑子进行大量的统计分析。因此,黑子的自动识别是开展研究的关键步骤。本文依据太阳黑子形态特征及其在日面上的位置,将其分为规则黑子、不规则黑子、小黑子、黑子群、边缘黑子以及边缘黑子群6大类,并提出一种太阳黑子识别模型——VanillaNet-MBConv-YOLOv8,实现对全日面光球图像中这6类黑子的自动识别。所提网络以VanillaNet替换YOLOv8的原有主干网络Darknet53,以MBConv模块优化原C2f模块,从而增强模型对太阳黑子特征提取的能力,改善网络模型错减、漏检现象,提升检测精度。在SDO/HMI(solar dynamics observatory/helioseismic and magnetic imager)的全日面太阳光球图像上的实验结果表明,所提网络模型相较于原YOLOv8模型以及其他主流网络模型,在网络性能、识别准确率以及漏检现象上均有显著提升。平均识别准确率达到91.0%,召回率达到71.5%,F1-score达到0.80。 展开更多
关键词 太阳黑子 目标检测 YOLOv8 卷积神经网络 VanillaNet MBConv
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