2016/03/23 by Chunming Zhu, Rui Liu, David Alexander +1 · 36 citations
Earth and Planetary Sciences · Physics and Astronomy · #Coronal loop #Coronal mass ejection #Current sheet #Earthquake Detection and Analysis #Event (particle physics) #Flare #Ionosphere and magnetosphere dynamics #Magnetic reconnection #Nanoflares #Solar and Space Plasma Dynamics #Solar flare #Solar physics #astro-ph.SR
paper · pdf · doi:10.3847/2041-8205/821/2/l29
published in The Astrophysical Journal Letters 821(2), L29 (IOP Publishing) · 7 pages, 5 figures
arxiv created 2016/03/23 · openalex publication_date 2016/04/19 · arxiv updated 2016/04/27 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
ABSTRACT We report multi-wavelength and multi-viewpoint observations of a solar eruptive event that involves loop–loop interactions. During a C2.0 flare, motions associated with inflowing and outflowing plasma provide evidence for ongoing magnetic reconnection. The flare loop top and a rising “concave-up” feature are connected by a current-sheet-like structure (CSLS). The physical properties (thickness, length, temperature, and density) of the CSLS are evaluated. In regions adjacent to the CSLS, the EUV emission (characteristic temperature at 1.6 MK) begins to increase more than 10 minutes prior to the onset of the flare, and steeply decreases during the decay phase. The reduction of the emission resembles that expected from coronal dimming. The dynamics of this event imply a magnetic reconnection rate in the range 0.01–0.05.