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Dynamic Property and Magnetic Nonpotentiality of Two Types of Confined Solar Flares View all abstracts by submitter

Ting Li   Submitted: 2022-07-14 09:53

We analyze 152 large confined flares (GOES class ≥M1.0 and ≤45° from disk center) during 2010-2019, and classify them into two types according to the criterion taken from the work of Li et al. (2019). ``Type I" flares are characterized by slipping motions of flare loops and ribbons and a stable filament underlying the flare loops. ``Type II" flares are associated with the failed eruptions of the filaments, which can be explained by the classical 2D flare model. A total of 59 flares are ``Type I" flares (about 40%) and 93 events are ``Type II" flares (about 60%). There are significant differences in distributions of the total unsigned magnetic flux (Φ_AR) of active regions (ARs) producing the two types of confined flares, with ``Type I" confined flares from ARs with a larger ΦAR than ``Type II". We calculate the mean shear angle Ψ_HFED within the core of an AR prior to the flare onset, and find that it is slightly smaller for ``Type I" flares than that for ``Type II" events. The relative non-potentiality parameter Ψ_HFED/Φ_AR has the best performance in distinguishing the two types of flares. About 73% of ``Type I" confined flares have Ψ_HFED/Φ_AR<1.0x10-21 degree Mx-1, and about 66% of ``Type II" confined events have Ψ_HFED/Φ_AR≥1.0x10-21 degree Mx-1. We suggest that ``Type I" confined flares cannot be explained by the standard flare model in 2D/3D, and the occurrence of multiple slipping magnetic reconnections within the complex magnetic systems probably leads to the observed flare.

Authors: Xuchun Duan, Ting Li and Qihang Jing
Projects: SDO-HMI

Publication Status: ApJ, 933 (2), 191, 2022
Last Modified: 2022-07-15 09:51
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