2016/09/20 by Yijun Hou, Jun Zhang, Ting Li +3 · 1 citation
Engineering · Physics and Astronomy · #Amplitude #Flare #Fluid dynamics and aerodynamics studies #Light curve #Light field #Magnetic field #Magnetic reconnection #Oscillation (cell signaling) #Scientific Research and Discoveries #Solar and Space Plasma Dynamics #Solar flare #Sunspot #astro-ph.SR
paper · pdf · doi:10.3847/2041-8205/829/2/l29
6 pages, 4 figures, Accepted for publication in ApJL
arxiv created 2016/09/20 · openalex publication_date 2016/09/28 · openalex created_date 2016/09/30 · arxiv updated 2016/10/05 · openalex updated_date 2026/08/05
ABSTRACT With the high-resolution data from the Interface Region Imaging Spectrograph , we detect a light wall above a sunspot light bridge in the NOAA active region (AR) 12403. In the 1330 Å slit-jaw images, the light wall is brighter than the ambient areas while the wall top and base are much brighter than the wall body, and it keeps oscillating above the light bridge. A C8.0 flare caused by a filament activation occurred in this AR with the peak at 02:52 UT on 2015 August 28, and the flare’s one ribbon overlapped the light bridge, which was the observational base of the light wall. Consequently, the oscillation of the light wall was evidently disturbed. The mean projective oscillation amplitude of the light wall increased from 0.5 to 1.6 Mm before the flare and decreased to 0.6 Mm after the flare. We suggest that the light wall shares a group of magnetic field lines with the flare loops, which undergo a magnetic reconnection process, and they constitute a coupled system. When the magnetic field lines are pushed upward at the pre-flare stage, the light wall turns to the vertical direction, resulting in the increase of the light wall’s projective oscillation amplitude. After the magnetic reconnection takes place, a group of new field lines with smaller scales are formed underneath the reconnection site, and the light wall inclines. Thus, the projective amplitude notably decrease at the post-flare stage.