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 Te = 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.