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Magnetic Flux of Active Regions Determining the Eruptive Character of Large Solar Flares View all abstracts by submitter

Ting Li   Submitted: 2020-07-16 21:38

We establish the largest eruptive/confined flare database to date and analyze 322 flares of GOES class M1.0 and larger that occurred during 2010-2019, i.e., almost spanning the entire solar cycle 24. We find that the total unsigned magnetic flux (ΦAR) of active regions (ARs) is a key parameter in governing the eruptive character of large flares, with the proportion of eruptive flares exhibiting a strong anti-correlation with ΦAR. This means that an AR containing a large magnetic flux has a lower probability for the large flares it produces to 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 ΦAR, implying that ARs with a larger ΦAR have a stronger magnetic confinement. Moreover, the confined flares originating from ARs larger than 1.01023 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. These relations obtained here provide quantitative criteria for forecasting CMEs and adverse space weather, and have also important implications for "superflares" on solar-type stars and stellar CMEs.

Authors: Ting Li, Yijun Hou, Shuhong Yang, Jun Zhang, Lijuan Liu, Astrid M. Veronig
Projects: SDO-HMI

Publication Status: accepted for publication in ApJ
Last Modified: 2020-07-18 21:49
Go to main E-Print page  Statistical Analysis of the Relation between Coronal Mass Ejections and Solar Energetic Particles  Case study of multi-temperature coronal jets for emerging flux MHD models  Edit Entry  Download Preprint  Delete Entry 

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