Imaging and Spectroscopic Observations of the Dynamic Processes in Limb Solar Flares

TL;DR

This study combines imaging and spectroscopic data from IRIS and AIA to analyze dynamic processes like magnetic reconnection, chromospheric evaporation, and coronal rain in limb solar flares, revealing detailed plasma motions and energy release mechanisms.

Contribution

It provides new observational evidence of multiple dynamic processes in solar flares using combined imaging and spectroscopic data, enhancing understanding of flare energy release.

Findings

Detection of magnetic reconnection downflows as redshifts and blueshifts.

Observation of chromospheric evaporation during the impulsive phase.

Identification of warm rain as downward moving plasma in the gradual phase.

Abstract

We investigate various dynamic processes including magnetic reconnection, chromospheric evaporation, and coronal rain draining in two limb solar flares through imaging and spectroscopic observations from the Interface Region Imaging Spectrograph (IRIS) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. In the early phase of the flares, a bright and dense loop-top structure with a cusp-like shape can be seen in multi-wavelength images, which is co-spatial with the hard X-ray 25--50 keV emission. In particular, intermittent magnetic reconnection downflows are detected in the time-space maps of AIA 304 {\AA}. The reconnection downflows are manifested as redshifts on one half of the loops and blueshifts on the other half in the IRIS Si {\sc iv} 1393.76 {\AA} line due to a projection effect. The Si {\sc iv} profiles exhibit complex features (say, multi-peak) with a relatively larger width at the loop-top region. During the impulsive phase, chromospheric evaporation is observed in both AIA images and the IRIS Fe {\sc xxi} 1354.08 {\AA} line. Upward motions can be seen from AIA 131 {\AA} images. The Fe {\sc xxi} line is significantly enhanced and shows a good Gaussian shape. In the gradual phase, warm rains are observed as downward moving plasmas in AIA 304 {\AA} images. Both the Si {\sc iv} and Fe {\sc xxi} lines show a relatively symmetric shape with a larger width around the loop top. These results provide observational evidence for various dynamic processes involved in and are crucial to understand the energy release process of solar flares.