摘要
2024年5月10—11日,太阳活动区(AR)13664爆发了自卡林顿事件(1859年)以来最强的太阳风暴事件之一,引发了G5级地磁暴(地磁扰动指数达-412 nT)和全球范围的极光现象。AR13664呈现致密复杂的磁场分布,伴随快速磁场演化与高活动性,如丰富的磁场浮现、拓扑重构与产生多个耀斑和日冕物质抛射(CME)等。由此AR 13664是否代表强烈太阳爆发的能量积累和释放的典型过程,使其成为研究磁场复杂度、能量存储与释放机制、强烈太阳爆发成因的理想对象。综述了目前相关研究成果,聚焦基于多波段观测、磁流体力学建模和非线性无力场外推,揭示AR 13664从磁通量浮现到近地空间响应的全链条物理过程。围绕AR 13664的研究结果表明:(1)该活动区表现出极高的磁通量浮现速率,峰值可达2.2×10^(22)Mx/d,迅速形成复杂的βγδ型磁结构,总无符号磁通量高达1.35×10^(23)Mx,为能量的高效存储奠定了磁拓扑基础;(2)磁拓扑分析结果表明,磁能释放过程与准分割面(QSL)及多重电流片的演化高度相关,揭示了局部非势能区的能量释放机制;(3)多阶段磁剪切过程被清晰观测到,表明磁绳结构的逐步形成与不稳定性增强,与随后爆发的12次X级耀斑和多个晕状CME密切相关;(4)相关CME具有跨赤道日面源区大尺度结构,在日地空间快速传播,最快投影速度超过2000 km/s,其行星际结构在1 AU处表现为强烈的南向磁场(行星际磁场z轴分量Bz最小达到-50 nT),对地球磁层造成剧烈冲击,诱发强磁暴和电离层扰动过程。这些研究系统描绘了极端空间天气事件从太阳源头到近地空间的全链条演化过程,为太阳爆发的触发、能量积累释放,以及传播机制提供了创新性理解,为建立更加准确和可预报的空间天气模型提供了重要的研究基础。
During May 10-11,2024,Solar Active Region(AR)13664 experienced one of the most intense solar storm events since the Carrington Event of 1859,triggering a G5-level geomagnetic storm(Dst index reaching-412 nT)and global auroral displays.AR 13664 exhibited a dense and complex magnetic field distribution,accompanied by rapid magnetic field evolution and high activity such as abundant magnetic emergence,topological restructuring,and the generation of multiple flares and coronal mass ejections(CMEs).AR 13664 may represent a typical process of energy accumulation and release in intense solar eruptions,making it an ideal subject for studying magnetic complexity,energy storage and release mechanisms,and the causes of strong solar eruptions.This paper reviews current relevant research findings,focusing on multi-band observations,magnetohydrodynamic modeling,and nonlinear force-free field extrapolations,to reveal the full chain physical processes from magnetic flux emergence to near-Earth space responses of AR 13664.The research results around AR 13664 indicate:(1)the region exhibited an extremely high rate of magnetic flux emergence,peaking at 2.2×10^(22)Mx/day,rapidly forming a complexβγδ-type magnetic structure,with a total unsigned magnetic flux of up to 1.35×10^(23)Mx,laying the magnetic topological foundation for efficient energy storage;(2)magnetic topology analysis indicates that the energy release process is closely related to the evolution of quasi-separatrix layers(QSLs)and the development of multiple current sheets,revealing the energy release mechanism in local non-potential energy regions;(3)multi-stage magnetic shearing processes were clearly observed,showing the gradual formation of magnetic rope structures and enhanced instability,closely associated with subsequent eruptions of 12 X-class flares and multiple halo CMEs;(4)the associated CMEs exhibit large-scale trans-equatorial source structures and propagate swiftly through solar-terrestrial space.Some of these CMEs reach projected speeds surpassing 2000 km/s and showcase pronounced southward magnetic fields(with the North-south magnetic field Bz dropping to a minimum of-50 nT)at 1 AU.These characteristics lead to significant impacts on Earth's magnetosphere,instigating intense magnetic storms and disturbances in the ionosphere.These studies systematically depict the full chain evolution process of extreme space weather events from the solar source to near-Earth space,providing innovative insights into the triggering,energy accumulation,release,and propagation mechanisms of solar eruptions,and offering an important research foundation for establishing more accurate and predictable space weather models.
作者
周桂萍
周振军
张小凡
林伟
万庆涛
ZHOU Guiping;ZHOU Zhenjun;ZHANG Xiaofan;LIN Wei;WAN Qingtao(Department of Solar Physics Research,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China;University of Chinese Academy of Sciences,Beijing 101499,China;School of Atmospheric Sciences,Sun Yat-sen University,Zhuhai 519080,China)
出处
《科技导报》
北大核心
2025年第16期93-104,共12页
Science & Technology Review
基金
中国科学院基础与交叉前沿科研先导专项(B类)(XDB0560102)
国家重点研发计划项目(2022YFF0503800)
国家自然科学基金委员会项目(12533010,12350004,12473095,12373111,12403067)。
关键词
极端太阳风暴
活动区
日冕物质抛射
磁重联
地磁暴
extreme solar storms
active region
coronal mass ejections
magnetic reconnection
geomagnetic storms
