YNAO OpenIR  > 抚仙湖太阳观测和研究基地
Growth of a filament channel by intermittent small-scale magnetic reconnection
Li, H. T.1,3; Cheng, X.1,2,3; Guo, J. H.1,3; Yan XL(闫晓理)4; Wang, L. F.1,3; Zhong, Z.1,3; Li, C.1,3; Ding, M. D.1,3
发表期刊ASTRONOMY & ASTROPHYSICS
2022-07-21
卷号663
DOI10.1051/0004-6361/202243115
产权排序第4完成单位
收录类别SCI ; EI
关键词Sun: activity Sun: filaments, prominences Sun: magnetic fields
摘要

Context. A filament channel (FC), a plasma volume where the magnetic field is primarily aligned with the polarity inversion line, is believed to be the pre-eruptive configuration of coronal mass ejections. Nevertheless, evidence for how the FC is formed is still elusive. Aims. In this paper, we present a detailed study of the build-up of a FC in order to understand its formation mechanism. Methods. The New Vacuum Solar Telescope (NVST) of the Yunnan Observatory and the Optical and Near-infrared Solar Eruption Tracer (ONSET) of Nanjing University, as well as the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO), are used to study the growth process of the FC. Furthermore, we reconstruct the nonlinear force-free field (NLFFF) of the active region using the regularized Biot-Savart laws (RBSL) and the magnetofrictional method to reveal the three-dimensional (3D) magnetic field properties of the FC. Results. We find that partial filament materials are quickly transferred to longer magnetic field lines formed by small-scale magnetic reconnection, as evidenced by dot-like H alpha and extreme ultraviolet (EUV) brightenings and subsequent bidirectional outflow jets, as well as untwisting motions. The H alpha and EUV bursts appear repeatedly at the same location and are closely associated with flux cancelation, which occurs between two small-scale opposite polarities and is driven by shearing and converging motions. The 3D NLFFF model reveals that the reconnection takes place in a hyperbolic flux tube that is located above the flux-cancelation site and below the FC. Conclusions. The FC is gradually built up toward a twisted flux rope via a series of small-scale reconnection events that occur intermittently prior to the eruption.

资助项目NSFC[11722325] ; NSFC[11733003] ; NSFC[11790303] ; NSFC[11873087] ; Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; National Key R&D Program of China[2021YFA1600504] ; Alexander von Humboldt foundation
项目资助者NSFC[11722325, 11733003, 11790303, 11873087] ; Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; National Key R&D Program of China[2021YFA1600504] ; Alexander von Humboldt foundation
语种英语
学科领域天文学 ; 太阳与太阳系 ; 太阳物理学
学科门类理学 ; 理学::天文学
文章类型Article
出版者EDP SCIENCES S A
出版地17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN0004-6361
URL查看原文
WOS记录号WOS:000828286700005
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CORONAL MASS EJECTION ; FLUX ROPE ; SOLAR TELESCOPE ; ERUPTION ; REGION ; FIELD ; EVOLUTION ; TOPOLOGY ; DYNAMICS ; FLARE
EI入藏号20223112453783
EI主题词Observatories
EI分类号701.2 Magnetism: Basic Concepts and Phenomena - 932.3 Plasma Physics
引用统计
被引频次:2[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
版本出版稿
条目标识符http://ir.ynao.ac.cn/handle/114a53/25379
专题抚仙湖太阳观测和研究基地
通讯作者Cheng, X.
作者单位1.School of Astronomy and Space Science, Nanjing University, Nanjing 210023, PR China;
2.Max Planck Institute for Solar System Research, Gottingen 37077, Germany;
3.Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, 210023, PR China;
4.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, PR China
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GB/T 7714
Li, H. T.,Cheng, X.,Guo, J. H.,et al. Growth of a filament channel by intermittent small-scale magnetic reconnection[J]. ASTRONOMY & ASTROPHYSICS,2022,663.
APA Li, H. T..,Cheng, X..,Guo, J. H..,Yan XL.,Wang, L. F..,...&Ding, M. D..(2022).Growth of a filament channel by intermittent small-scale magnetic reconnection.ASTRONOMY & ASTROPHYSICS,663.
MLA Li, H. T.,et al."Growth of a filament channel by intermittent small-scale magnetic reconnection".ASTRONOMY & ASTROPHYSICS 663(2022).
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