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Properties and Energetics of Magnetic Reconnection: I. Evolution of Flare Ribbons View all abstracts by submitter

Jiong Qiu   Submitted: 2022-05-13 19:56

In this article, we measure the mean magnetic shear from the morphological evolution of flare ribbons, and examine the evolution of flare thermal and nonthermal X-ray emissions during the progress of flare reconnection. We analyze three eruptive flares and three confined flares ranging from GOES class C8.0 to M7.0. They exhibit well-defined two ribbons along the magnetic polarity inversion line (PIL), and have been observed by the Atmospheric Imaging Assembly and the Ramaty High Energy Solar Spectroscopic Imager from the onset of the flare throughout the impulsive phase. The analysis confirms the strong-to-weak shear evolution in the core region of the flare, and the flare hard X-ray emission rises as the shear decreases. In eruptive flares in this sample, significant nonthermal hard X-ray emission lags the ultraviolet emission from flare ribbons, and rises rapidly when the shear is modest. In all flares, we observe that the plasma temperature rises in the early phase when the flare ribbons rapidly spread along the PIL and the shear is high. We compare these results with prior studies, and discuss their implications, as well as complications, related to physical mechanisms governing energy partition during flare reconnection.

Authors: J. Qiu & J. Cheng
Projects: RHESSI,SDO-AIA,SDO-HMI

Publication Status: Solar Physics, accepted
Last Modified: 2022-05-16 08:37
Go to main E-Print page  Data-driven modeling of solar coronal magnetic field evolution and eruptions  A new look at the frequency-dependent damping of slow-mode waves in the solar corona  Edit Entry  Download Preprint  Delete Entry 

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