2016/01/07 by V. Aparna, Durgesh Tripathi
Physics and Astronomy · #Astrophysics #Coronal mass ejection #Extreme ultraviolet #Extreme ultraviolet lithography #Flux (metallurgy) #Ionosphere and magnetosphere dynamics #Materials science #Nuclear physics #Optics #Phase (matter) #Physics #Plasma #Protein filament #Rope #Solar and Space Plasma Dynamics #Solar wind #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.3847/0004-637x/819/1/71
published as ApJ, 819 (2016), 71 · 16 pages, 6 figures
arxiv created 2016/01/07 · openalex publication_date 2016/02/29 · arxiv updated 2016/04/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
ABSTRACT A filament eruption was observed on 2010 October 31 in the images recorded by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory ( SDO ) in its Extreme Ultra-Violet (EUV) channels. The filament showed a slow-rise phase followed by a fast rise and was classified to be an asymmetric eruption. In addition, multiple localized brightenings which were spatially and temporally associated with the slow-rise phase were identified, leading us to believe that the tether-cutting mechanism initiated the eruption. An associated flux rope was detected in high-temperature channels of AIA, namely 94 and 131 Å, corresponding to 7 and 11 MK plasma respectively. In addition, these channels are also sensitive to cooler plasma corresponding to 1–2 MK. In this study, we have applied the algorithm devised by Warren et al. to remove cooler emission from the 94 Å channel to deduce only the high-temperature structure of the flux rope and to study its temporal evolution. We found that the flux rope was very clearly seen in the clean 94 Å channel image corresponding to Fe xviii emission, which corresponds to a plasma at a temperature of 7 MK. This temperature matched well with that obtained using Differential Emission Measure analysis. This study provides important constrains in the modeling of the thermodynamic structure of the flux ropes in coronal mass ejections.