2016/11/11 by Bhuwan Joshi, Upendra Kushwaha, Astrid Veronig +2
Computer Science · Physics and Astronomy · #Astronomy #Astrophysics #Corona (planetary geology) #Coronal mass ejection #Current sheet #Extreme ultraviolet #Flare #Flux (metallurgy) #Ionosphere and magnetosphere dynamics #Jet (fluid) #Laser #Magnetic field #Magnetic reconnection #Magnetohydrodynamics #Mechanics #Physics #Plasmoid #Solar Radiation and Photovoltaics #Solar and Space Plasma Dynamics #Solar flare #Solar wind #astro-ph.SR
paper · pdf · doi:10.3847/0004-637x/832/2/130
17 pages, 10 figures, The Astrophysical Journal
arxiv created 2016/11/11 · openalex publication_date 2016/11/23 · openalex created_date 2016/11/30 · arxiv updated 2016/12/07 · openalex updated_date 2026/08/05
ABSTRACT We investigate the triggering, activation, and ejection of a solar eruptive prominence that occurred in a multi-polar flux system of active region NOAA 11548 on 2012 August 18 by analyzing data from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory , the Reuven Ramaty High Energy Solar Spectroscopic Imager , and the Extreme Ultraviolet Imager/Sun Earth Connection Coronal and Heliospheric Investigation on board the Solar Terrestrial Relation Observatory . Prior to the prominence activation, we observed striking coronal activities in the form of a blowout jet, which is associated with the rapid eruption of a cool flux rope. Furthermore, the jet-associated flux rope eruption underwent splitting and rotation during its outward expansion. These coronal activities are followed by the prominence activation during which it slowly rises with a speed of ∼12 km s −1 while the region below the prominence emits gradually varying EUV and thermal X-ray emissions. From these observations, we propose that the prominence eruption is a complex, multi-step phenomenon in which a combination of internal (tether-cutting reconnection) and external (i.e., pre-eruption coronal activities) processes are involved. The prominence underwent catastrophic loss of equilibrium with the onset of the impulsive phase of an M1.8 flare, suggesting large-scale energy release by coronal magnetic reconnection. We obtained signatures of particle acceleration in the form of power-law spectra with hard electron spectral index ( δ ∼ 3) and strong HXR footpoint sources. During the impulsive phase, a hot EUV plasmoid was observed below the apex of the erupting prominence that ejected in the direction of the prominence with a speed of ∼177 km s −1 . The temporal, spatial, and kinematic correlations between the erupting prominence and the plasmoid imply that the magnetic reconnection supported the fast ejection of prominence in the lower corona.