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Two Types of Confined Solar Flares
Li,Ting1,2; Liu,Lijuan3,4; Hou,Yijun1,2; Zhang,Jun1,2
2019-08-22
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume881Issue:2
AbstractAbstract With the aim of understanding the physical mechanisms of confined flares, we selected 18 confined flares during 2011–2017, and first classified them into two types based on their different dynamic properties and magnetic configurations. “Type I” confined flares are characterized by slipping reconnection, strong shear, and a stable filament. “Type II” flares have almost no slipping reconnection, and have a configuration in potential state after the flare. A filament erupts but is confined by a strong strapping field. “Type II” flares could be explained by 2D MHD models, while “type I” flares need 3D MHD models. Seven of 18 confined flares (~39%) belong to “type I” and 11 (~61%) are “type II.” The post-flare loops (PFLs) of “type I” flares have a stronger non-potentiality, but the PFLs in “type II” flares are weakly sheared. All the “type I” flares exhibit ribbon elongations parallel to the polarity inversion line (PIL) at speeds of several tens of km s?1. Only a small proportion of “type II” flares show ribbon elongations along the PIL. We suggest that different magnetic topologies and reconnection scenarios dictate the distinct properties for the two types of flares. Slipping magnetic reconnections between multiple magnetic systems result in “type I” flares. For “type II” flares, magnetic reconnections occur in antiparallel magnetic fields underlying the erupting filament. Our study shows that “type I” flares account for more than one third of all the large confined flares, and should not be neglected in further studies.
Keywordmagnetic reconnection Sun: activity Sun: flares Sun: magnetic fields
DOI10.3847/1538-4357/ab3121
Language英语
WOS IDIOP:0004-637X-881-2-ab3121
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/27771
Collection中国科学院国家天文台
Affiliation1.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China liting@nao.cas.cn
2.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
3.School of Atmospheric Sciences, Sun Yat-sen University, Zhuhai, Guangdong, 519082, People’s Republic of China; liulj8@mail.sysu.edu.cn
4.CAS Center for Excellence in Comparative Planetology, People’s Republic of China
First Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Li,Ting,Liu,Lijuan,Hou,Yijun,et al. Two Types of Confined Solar Flares[J]. The Astrophysical Journal,2019,881(2).
APA Li,Ting,Liu,Lijuan,Hou,Yijun,&Zhang,Jun.(2019).Two Types of Confined Solar Flares.The Astrophysical Journal,881(2).
MLA Li,Ting,et al."Two Types of Confined Solar Flares".The Astrophysical Journal 881.2(2019).
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