YNAO OpenIR  > 抚仙湖太阳观测和研究基地
A solar filament disconnected by magnetic reconnection
Xue ZK(薛志科)1,2,3; Yan XL(闫晓理)1,2; Yang LH(杨丽恒)1,2; Wang JC(王金成)1,2; Li QL(李巧玲)1,2,4; Zhao L(赵丽)1,2
发表期刊ASTRONOMY & ASTROPHYSICS
2020-01-21
卷号633页码:8
DOI10.1051/0004-6361/201936969
产权排序第1完成单位
收录类别SCI ; EI
关键词Sun: filaments, prominences magnetic reconnection Sun: activity Sun: magnetic fields
摘要

Aims. We aim to study a high-resolution observation of an asymmetric inflow magnetic reconnection between a filament and its surrounding magnetic loops in active region NOAA 12436 on 2015 October 23.

Methods. We analyzed the multiband observations of the magnetic reconnection obtained by the New Vacuum Solar Telescope (NVST) and the Solar Dynamic Observatory. We calculated the NVST H alpha Dopplergrams to determine the Doppler properties of the magnetic reconnection region and the rotation of a jet.

Results. The filament firstly becomes active and then approaches its southwestern surrounding magnetic loops (L1) with a velocity of 9.0 km s(-1). During this period, the threads of the filament become loose in the reconnection region and then reconnect with L1 in turn. L1 is pressed backward by the filament with a velocity of 5.5 km s(-1), and then the magnetic reconnection occurs between them. A set of newly formed loops are separated from the reconnection site with a mean velocity of 127.3 km s(-1). In the middle stage, some threads of the filament return back first with a velocity of 20.1 km s(-1), and others return with a velocity of 4.1 km s(-1) after about 07:46 UT. Then, L1 also begins to return with a velocity of 3.5 km s(-1) at about 07:47 UT. At the same time, magnetic reconnection continues to occur between them until 07:51 UT. During the reconnection, a linear typical current sheet forms with a length of 5.5 Mm and a width of 1.0 Mm, and a lot of hot plasma blobs are observed propagating from the typical current sheet. During the reconnection, the plasma in the reconnection region and the typical current sheet always shows redshifted feature. Furthermore, the material and twist of the filament are injected into the newly longer-formed magnetic loops by the magnetic reconnection, which leads to the formation of a jet, and its rotation.

Conclusions. The observational evidence for the asymmetric inflow magnetic reconnection is investigated. We conclude that the magnetic reconnection does occur in this event and results in the disconnection of the filament. The looseness of the filament may be due to the pressure imbalance between the inside and outside of the filament. The redshifted feature in the reconnection site can be explained by the expansion of the right flank of the filament to the lower atmosphere because of the complex magnetic configuration in this active region.

资助项目National Science Foundation of China (NSFC)[11973084] ; National Science Foundation of China (NSFC)[11873087] ; National Science Foundation of China (NSFC)[11803085] ; National Science Foundation of China (NSFC)[11803086] ; National Science Foundation of China (NSFC)[11633008] ; Yunnan Science Foundation of China[2018FB007] ; Yunnan Science Foundation of China[2018FA001] ; Youth Innovation Promotion Association, CAS[2019061] ; Youth Innovation Promotion Association, CAS[2011056] ; CAS 'Light of West China' Program ; Project of the Group for Innovation of Yunnan Province ; CAS Key Laboratory of Solar Activity, National Astronomical Observatories[KLSA201910]
项目资助者National Science Foundation of China (NSFC)[11973084, 11873087, 11803085, 11803086, 11633008] ; Yunnan Science Foundation of China[2018FB007, 2018FA001] ; Youth Innovation Promotion Association, CAS[2019061, 2011056] ; CAS 'Light of West China' Program ; Project of the Group for Innovation of Yunnan Province ; CAS Key Laboratory of Solar Activity, National Astronomical Observatories[KLSA201910]
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::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:000508936600003
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]MOTIONS ; FLARE ; MODEL
EI入藏号20202908954978
EI主题词Magnetism
EI分类号701.2 Magnetism: Basic Concepts and Phenomena
引用统计
被引频次:13[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/22112
专题抚仙湖太阳观测和研究基地
通讯作者Xue ZK(薛志科)
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, Kunming Yunnan 650216, PR China
2.Center for Astronomical Mega-Science, Chinese Academy of Sciences, Beijing 100012, PR China
3.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Beijing 100012, PR China
4.University of Chinese Academy of Sciences, Beijing 100049, PR China
第一作者单位中国科学院云南天文台
通讯作者单位中国科学院云南天文台
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GB/T 7714
Xue ZK,Yan XL,Yang LH,et al. A solar filament disconnected by magnetic reconnection[J]. ASTRONOMY & ASTROPHYSICS,2020,633:8.
APA Xue ZK,Yan XL,Yang LH,Wang JC,Li QL,&Zhao L.(2020).A solar filament disconnected by magnetic reconnection.ASTRONOMY & ASTROPHYSICS,633,8.
MLA Xue ZK,et al."A solar filament disconnected by magnetic reconnection".ASTRONOMY & ASTROPHYSICS 633(2020):8.
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