The Prominence Driven Forced Reconnection in the Solar Corona and Associated Plasma Dynamics

Abstract

Using the multitemperature observations from SDO/AIA on 2019 December 30, we provide a signature of prominence driven forced magnetic reconnection in the corona and associated plasma dynamics from 09:20 UT to 10:38 UT. A hot prominence segment erupts with a speed of ≈21 km s-1 and destabilizes the entire prominence system. Thereafter, it rises upward in the north from 09:28 UT to 09:48 UT with a speed of 24 km s-1 . The eruptive prominence stretches overlying field lines upward with the speed of 27-28 km s-1, which further undergo the forced reconnection. The coronal plasma also flows southward with a speed of 7 km s-1, and both of these inflows trigger the reconnection at ≈09:48 UT. Thereafter, the eastward and westward magnetic channels are developed and separated. The east-west reorganization of the magnetic fields starts creating bidirectional plasma outflows toward the limb with their respective speeds of 28 and 37 km s-1. Their upper ends are diffused in the overlying corona, transporting another set of upflows with the speeds of ≈22 km and 19 km s-1. The multitemperature plasma (log T e = 6.0-7.2 K) evolves and elongates to a length of ≈105 km on the reorganized fields. The hot plasma and remaining prominence threads move from the reconnection region toward another segment of a prominence in the eastward direction. The prominence-prominence/loop interaction and associated reconnection generate jet-like eruptions with a speed of 178-183 km s-1. After the formation of the jet, the overlying magnetic channel disappears in the corona. © 2021. The American Astronomical Society. All rights reserved..