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Formation of a Solar Filament by Magnetic Reconnection, Associated Chromospheric Evaporation, and Subsequent Coronal Condensation
Yang B(杨波)1,2,3; Yang JY(杨家艳)1,2; Bi Y(毕以)1,2; Hong JC(洪俊超)1,2; Xu, Zhe4
Source PublicationASTROPHYSICAL JOURNAL LETTERS
2021-11
Volume921Issue:2
DOI10.3847/2041-8213/ac31b6
Contribution Rank第1完成单位
Indexed BySCI
Abstract

We present the first observation of a solar filament formed by magnetic reconnection, associated chromospheric evaporation, and subsequent coronal condensation. Driven by shearing motion during flux emergence, a sequential tether-cutting reconnection process occurred and resulted in an M1.3 confined flare accompanied by the formation of a sigmoid structure. It is found that the flare had conjugate compact footpoint brightenings, which correspond to the footpoints of the sigmoid. Furthermore, observational evidence of explosive evaporation is well diagnosed at the conjugate footpoint brightenings in the impulsive phase of the flare. After the flare, continuous cool condensations formed at about the middle section of the sigmoid and then moved in opposite directions along the sigmoid, eventually leading to the formation of the filament. These observations suggest that magnetic reconnection can not only form the magnetic field structure of the filament but also heat the chromospheric footpoints during their formation and drive chromospheric evaporation. As a result, the heated chromospheric plasma may be evaporated into the magnetic field structure of the filament, where the accumulated hot plasma might suffer from thermal instability or nonequilibrium, causing catastrophic cooling and coronal condensation to form the cool, dense material of the filament. This observation lends strong support to the evaporation-condensation model and highlights the crucial role of magnetic reconnection in forming both the magnetic field structure and the cool, dense material of the filaments.

Funding ProjectNational Key R&D Program of China[2019YFA0405000] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[12073072] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[11633008] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[11933009] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[12173084] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[11873088] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[11703084] ; CAS Light of West China Program ; Open Research Program of the Key Laboratory of Solar Activity of the Chinese Academy of Sciences[KLSA202018] ; CASChinese Academy of Sciences[QYZDJ-SSW-SLH012] ; Yunnan Natural Science FoundationNatural Science Foundation of Yunnan Province[202001AU070052] ; Yunnan Natural Science FoundationNatural Science Foundation of Yunnan Province[202101AV070004] ; China Postdoctoral Science FoundationChina Postdoctoral Science Foundation[2020M671639]
Funding OrganizationNational Key R&D Program of China[2019YFA0405000] ; Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[12073072, 11633008, 11933009, 12173084, 11873088, 11703084] ; CAS Light of West China Program ; Open Research Program of the Key Laboratory of Solar Activity of the Chinese Academy of Sciences[KLSA202018] ; CASChinese Academy of Sciences[QYZDJ-SSW-SLH012] ; Yunnan Natural Science FoundationNatural Science Foundation of Yunnan Province[202001AU070052, 202101AV070004] ; China Postdoctoral Science FoundationChina Postdoctoral Science Foundation[2020M671639]
Language英语
Subject Area天文学 ; 太阳与太阳系 ; 太阳物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP Publishing Ltd
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN2041-8205
URL查看原文
WOS IDWOS:000715533600001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordHELICAL FLUX ; PROMINENCE ; ERUPTION ; EMERGENCE ; TELESCOPE ; FLARES ; MODEL ; ONSET
Citation statistics
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24656
Collection抚仙湖太阳观测和研究基地
太阳物理研究组
Corresponding AuthorYang B(杨波)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People's Republic of China; boyang@ynao.ac.cn;
2.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China;
3.Key Laboratory of Solar Activity, National Astronomical Observatories of Chinese Academy of Science, Beijing, 100012, People's Republic of China;
4.Purple Mountain Observatory, Chinese Academy of Sciences, No. 8 Yuanhua Road, Qixia District, Nanjing 210034, People's Republic of China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Yang B,Yang JY,Bi Y,et al. Formation of a Solar Filament by Magnetic Reconnection, Associated Chromospheric Evaporation, and Subsequent Coronal Condensation[J]. ASTROPHYSICAL JOURNAL LETTERS,2021,921(2).
APA Yang B,Yang JY,Bi Y,Hong JC,&Xu, Zhe.(2021).Formation of a Solar Filament by Magnetic Reconnection, Associated Chromospheric Evaporation, and Subsequent Coronal Condensation.ASTROPHYSICAL JOURNAL LETTERS,921(2).
MLA Yang B,et al."Formation of a Solar Filament by Magnetic Reconnection, Associated Chromospheric Evaporation, and Subsequent Coronal Condensation".ASTROPHYSICAL JOURNAL LETTERS 921.2(2021).
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