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Decay of Solar Pores Driven by Small-scale Magnetic Reconnection Episodes
Xue ZK(薛志科)1,2,3; Yan XL(闫晓理)1,3; Yang LH(杨丽恒)1,2,3; Chen, Jie2; Wang JC(王金成)1,3; Li, Qiaoling4; Zhao L(赵丽)1,3
Source PublicationASTROPHYSICAL JOURNAL LETTERS
2021-10
Volume919Issue:2
DOI10.3847/2041-8213/ac2733
Contribution Rank第1完成单位
Indexed BySCI
Abstract

We present the relationships between the disappearances of two small pores, magnetic cancellations, and magnetic reconnection episodes in the NOAA AR 12778 on 2020 October 26 with high-resolution observations of the New Vacuum Solar Telescope and the Solar Dynamics Observatory. Two emerging positive polarities (P1 and P2) approach a negative polarity (N1) with velocities of 0.26 and 0.42 km s(-1), respectively. Then, two small-scale magnetic reconnection episodes occur between a series of magnetic loops that are rooted in these polarities. The reconnection inflow velocities are around 4.0 km s(-1) which is faster than the movements of P1 and P2. Compared with the first magnetic reconnection episode, more magnetic free energy is released in the second reconnection episode due to the greater magnetic strength of P2. Subsequently, magnetic cancellation occurs first between P1 and N1, and then between P2 and N1. At the same time, the pores S1 (N1) and S2 (P2) decay and disappear. The area decay rate of the small pore S2 is estimated to be 7.3 Mm(2) hr(-1), which is larger than previously reported cases. And the flux decay rate of S2 is 5.1 x 10(19) Mx hr(-1), similar to the results obtained in the larger sunspots. We conclude that the magnetic reconnection episodes may be caused by both the movement of the magnetic polarities and the plasma dynamics themselves. The decay and disappearance of the small pores and the polarities are driven by magnetic reconnection episodes and then flux submergence. We suggest that a magnetic reconnection episode is a more efficient mechanism for the disappearance of solar pores.

Funding ProjectNational Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11873087] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11803085] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11803086] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11633008] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[U1831210] ; Youth Innovation Promotion Association, CAS[2019061] ; CAS Light of West China Program, Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; Key Research and Development Project of Yunnan Province[202003AD150019] ; National Key R&D Program of China[2019YFA0405000] ; CAS Key Laboratory of Solar Activity, National Astronomical Observatories[KLSA202104] ; CAS Key Laboratory of Solar Activity, National Astronomical Observatories[KLSA202101]
Funding OrganizationNational Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11873087, 11803085, 11803086, 11633008, U1831210] ; Youth Innovation Promotion Association, CAS[2019061] ; CAS Light of West China Program, Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; Key Research and Development Project of Yunnan Province[202003AD150019] ; National Key R&D Program of China[2019YFA0405000] ; CAS Key Laboratory of Solar Activity, National Astronomical Observatories[KLSA202104, KLSA202101]
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:000703260200001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordFIELD ; EVOLUTION ; JETS ; FLUX
Citation statistics
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24582
Collection抚仙湖太阳观测和研究基地
选址与日冕观测组
Corresponding AuthorXue ZK(薛志科)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan 650216, People's Republic of China; zkxue@ynao.ac.cn;
2.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Beijing 100012, People's Republic of China;
3.Center for Astronomical Mega-Science, Chinese Academy of Sciences, Beijing 100012, People's Republic of China;
4.Department of Physics, Yunnan University, Kunming, Yunnan 650091, 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
Xue ZK,Yan XL,Yang LH,et al. Decay of Solar Pores Driven by Small-scale Magnetic Reconnection Episodes[J]. ASTROPHYSICAL JOURNAL LETTERS,2021,919(2).
APA Xue ZK.,Yan XL.,Yang LH.,Chen, Jie.,Wang JC.,...&Zhao L.(2021).Decay of Solar Pores Driven by Small-scale Magnetic Reconnection Episodes.ASTROPHYSICAL JOURNAL LETTERS,919(2).
MLA Xue ZK,et al."Decay of Solar Pores Driven by Small-scale Magnetic Reconnection Episodes".ASTROPHYSICAL JOURNAL LETTERS 919.2(2021).
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