中国科学院机构知识库网格
Chinese Academy of Sciences Institutional Repositories Grid
A solar filament disconnected by magnetic reconnection

文献类型:期刊论文

AuthorXue 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
SourceASTRONOMY & ASTROPHYSICS
Issued Date2020-01-21
Volume633Pages:8
KeywordSun: filaments, prominences magnetic reconnection Sun: activity Sun: magnetic fields
ISSN0004-6361
DOI10.1051/0004-6361/201936969
Rank第1完成单位
SubtypeArticle
English Abstract

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.

Subject天文学 ; 太阳与太阳系 ; 太阳物理学
URL查看原文
Publish Place17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
Funding ProjectNational 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]
WOS KeywordMOTIONS ; FLARE ; MODEL
WOS Research AreaAstronomy & Astrophysics
Language英语
PublisherEDP SCIENCES S A
WOS IDWOS:000508936600003
Funding OrganizationNational 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]
源URL[http://ir.ynao.ac.cn/handle/114a53/22111]  
Collection云南天文台_抚仙湖太阳观测站
Corresponding AuthorXue ZK(薛志科)
Affiliation1.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
Recommended Citation
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.

入库方式: OAI收割

来源:云南天文台

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