YNAO OpenIR  > 抚仙湖太阳观测和研究基地
The Formation Process of the First Halo Coronal Mass Ejection in Solar Cycle 25: Magnetic Cancellation, Bidirectional Jet, and Hot Channel
Yan XL(闫晓理)1,2; Wang JC(王金成)1; Guo, Qiaoling3; Xue ZK(薛志科)1; Yang LH(杨丽恒)1; Tan, Baolin2
Source PublicationASTROPHYSICAL JOURNAL
2021-09-01
Volume919Issue:1Pages:8
DOI10.3847/1538-4357/ac116d
Contribution Rank第1完成单位
Indexed BySCI
Abstract

To better understand the trigger mechanism of a coronal mass ejection (CME), we present the evolution of a CME source region (active region NOAA 12790) and the formation of a hot channel before the occurrence of the first halo CME in solar cycle 25. Through analyzing the evolution of Solar Dynamics Observatory/Helioseismic and Magnetic Imager line-of-sight magnetograms, it is found that continuous magnetic cancellation occurs at the polarity inversion line (PIL) in this active region. With ongoing magnetic cancellation, several bidirectional jets and unidirectional jets occur along the large-scale arched magnetic loops. A hot channel forms during the first bidirectional jet. After the occurrence of the fourth bidirectional jet, the hot channel immediately erupts and produces a C-class flare, a cusp structure, and a halo CME. It is worth pointing out that the cusp structure only appears in the 131 angstrom and 94 angstrom observations (temperature about 10 MK). The obvious contraction of the newly formed loops is observed at the top of the cusp structure. The observations reveal a clear physics process: magnetic cancellation of a bipolar magnetic field at the PIL results in the occurrence of the bidirectional/unidirectional jets and the formation of the hot channel. The axial magnetic flux feeding for the hot channel through the continued magnetic cancellation leads to the hot channel eruption, which results in the formation of the hot cusp structure and the occurrence of the C-class flare and the halo CME.

Funding ProjectNational Science Foundation of China (NSFC)[11873087] ; National Science Foundation of China (NSFC)[11973084] ; National Science Foundation of China (NSFC)[11803085] ; National Science Foundation of China (NSFC)[2019FD085] ; National Science Foundation of China (NSFC)[12003064] ; National Science Foundation of China (NSFC)[11633008] ; National Science Foundation of China (NSFC)[11763004] ; National Science Foundation of China (NSFC)[U1831210] ; National Science Foundation of China (NSFC)[11803002] ; Yunnan Key Science Foundation of China[2018FA001] ; Yunnan Key Science Foundation of China[2018FB007] ; Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; Key Laboratory of Solar Activity of CAS[KLSA202008] ; Key Research and Development Project of Yunnan Province[202003AD150019]
Funding OrganizationNational Science Foundation of China (NSFC)[11873087, 11973084, 11803085, 2019FD085, 12003064, 11633008, 11763004, U1831210, 11803002] ; Yunnan Key Science Foundation of China[2018FA001, 2018FB007] ; Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; Key Laboratory of Solar Activity of CAS[KLSA202008] ; Key Research and Development Project of Yunnan Province[202003AD150019]
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
ISSN0004-637X
URL查看原文
WOS IDWOS:000697834600001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordRECONNECTION ; FLARE ; FILAMENT ; PROMINENCE ; ERUPTIONS ; MODEL ; LOOPS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24634
Collection抚仙湖太阳观测和研究基地
Corresponding AuthorYan XL(闫晓理)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
2.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Beijing 100012, People's Republic of China
3.College of Mathematics Physics and Information Engineering, Jiaxing University, Jiaxing 314001, 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
Yan XL,Wang JC,Guo, Qiaoling,et al. The Formation Process of the First Halo Coronal Mass Ejection in Solar Cycle 25: Magnetic Cancellation, Bidirectional Jet, and Hot Channel[J]. ASTROPHYSICAL JOURNAL,2021,919(1):8.
APA Yan XL,Wang JC,Guo, Qiaoling,Xue ZK,Yang LH,&Tan, Baolin.(2021).The Formation Process of the First Halo Coronal Mass Ejection in Solar Cycle 25: Magnetic Cancellation, Bidirectional Jet, and Hot Channel.ASTROPHYSICAL JOURNAL,919(1),8.
MLA Yan XL,et al."The Formation Process of the First Halo Coronal Mass Ejection in Solar Cycle 25: Magnetic Cancellation, Bidirectional Jet, and Hot Channel".ASTROPHYSICAL JOURNAL 919.1(2021):8.
Files in This Item:
File Name/Size DocType Version Access License
The Formation Proces(1719KB)期刊论文出版稿开放获取CC BY-NC-SAView Application Full Text
Related Services
Recommend this item
Bookmark
Usage statistics
Export to Endnote
Google Scholar
Similar articles in Google Scholar
[Yan XL(闫晓理)]'s Articles
[Wang JC(王金成)]'s Articles
[Guo, Qiaoling]'s Articles
Baidu academic
Similar articles in Baidu academic
[Yan XL(闫晓理)]'s Articles
[Wang JC(王金成)]'s Articles
[Guo, Qiaoling]'s Articles
Bing Scholar
Similar articles in Bing Scholar
[Yan XL(闫晓理)]'s Articles
[Wang JC(王金成)]'s Articles
[Guo, Qiaoling]'s Articles
Terms of Use
No data!
Social Bookmark/Share
File name: The Formation Process of the First Halo Coronal Mass Ejection in Solar Cycle 25_ Magnetic Cancellation, Bidirectional Jet, and Hot Channel.pdf
Format: Adobe PDF
All comments (0)
No comment.
 

Items in the repository are protected by copyright, with all rights reserved, unless otherwise indicated.