Magnetic Flux of Active Regions Determining the Eruptive Character of Large Solar Flares
Li,Ting1,2; Hou,Yijun1,2; Yang,Shuhong1,2; Zhang,Jun1,3; Liu,Lijuan4,5; Veronig,Astrid M.6
Source PublicationThe Astrophysical Journal
AbstractAbstract We establish the largest eruptive/confined flare database to date and analyze 322 flares of Geostationary Operational Environmental Satellite class M1.0 and larger that occurred during 2010–2019, i.e., almost spanning all of solar cycle 24. We find that the total unsigned magnetic flux ( ) of active regions (ARs) is a key parameter governing the eruptive character of large flares, with the proportion of eruptive flares exhibiting a strong anticorrelation with . This means that an AR containing a large magnetic flux has a lower probability that the large flares it produces will be associated with a coronal mass ejection (CME). This finding is supported by the high positive correlation we obtained between the critical decay index height and , implying that ARs with a larger have a stronger magnetic confinement. Moreover, the confined flares originating from ARs larger than Mx have several characteristics in common: stable filament, slipping magnetic reconnection, and strongly sheared post-flare loops. Our findings reveal new relations between the magnetic flux of ARs and the occurrence of CMEs in association with large flares. The relations obtained here provide quantitative criteria for forecasting CMEs and adverse space weather, and have important implications for “superflares” on solar-type stars and stellar CMEs.
KeywordSolar flares Solar activity Solar coronal mass ejections Stellar flares Solar magnetic fields Stellar coronal mass ejections
WOS IDIOP:0004-637X-900-2-aba6ef
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China;
2.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
3.School of Physics and Materials Science, Anhui University, Hefei 230601, People’s Republic of China
4.School of Atmospheric Sciences, Sun Yat-sen University, Zhuhai, Guangdong, 519082, People’s Republic of China
5.CAS Center for Excellence in Comparative Planetology, People’s Republic of China
6.Institute of Physics & Kanzelh?he Observatory for Solar and Environmental Research, University of Graz, A-8010 Graz, Austria
First Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
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GB/T 7714
Li,Ting,Hou,Yijun,Yang,Shuhong,et al. Magnetic Flux of Active Regions Determining the Eruptive Character of Large Solar Flares[J]. The Astrophysical Journal,2020,900(2).
APA Li,Ting,Hou,Yijun,Yang,Shuhong,Zhang,Jun,Liu,Lijuan,&Veronig,Astrid M..(2020).Magnetic Flux of Active Regions Determining the Eruptive Character of Large Solar Flares.The Astrophysical Journal,900(2).
MLA Li,Ting,et al."Magnetic Flux of Active Regions Determining the Eruptive Character of Large Solar Flares".The Astrophysical Journal 900.2(2020).
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