The prominence driven forced reconnection in the solar corona and associated plasma dynamics

TL;DR

This study presents multi-temperature observations of prominence-driven forced magnetic reconnection in the solar corona, revealing plasma dynamics, magnetic reorganization, and jet-like eruptions during a specific solar event on December 30, 2019.

Contribution

It provides detailed observational evidence of prominence-driven forced magnetic reconnection and associated plasma flows in the solar corona, highlighting new insights into the dynamics of prominence eruptions.

Findings

Prominence erupts at 21 km/s, destabilizing the system.

Bi-directional plasma outflows reach speeds of 28-37 km/s.

Jet-like eruptions occur at speeds of 178-183 km/s.

Abstract

Using the multi-temperature observations from SDO/AIA on 30th December 2019, we provide a signature of prominence driven forced magnetic reconnection in the corona and associated plasma dynamics during 09:20 UT to 10:38 UT. A hot prominence segment erupts with a speed of 21 km/s and destabilises the entire prominence system. Thereafter, it rose upward in the north during 09:28 UT to 09:48 UT with a speed of 24 km/s. The eruptive prominence stretches overlying field lines upward with the speed of 27-28 km/s , which further undergo into the forced reconnection. The coronal plasma also flows in southward direction with the speed of 7 km/s, and both these inflows trigger the reconnection at 09:48 UT. Thereafter, the east and westward magnetic channels are developed and separated. The east-west reorganization of the magnetic fields starts creating bi-directional plasma outflows towards the limb with their respective speed of 28 km/s and 37 km/s. Their upper ends are diffused in the overlying corona, transporting another set of upflows with the speed of 22 km/s and 19 km/s. The multi-temperature plasma (Te=6.0-7.2) evolves and elongated upto a length of ~10^5 km on the reorganized fields. The hot plasma and remaining prominence threads move from reconnection region towards another segment of prominence in the eastward direction. The prominence-prominence/loop interaction and associated reconnection generate jet-like eruptions with the speed of 178-183 km/s. After the formation of jet, the overlying magnetic channel is disappeared in the corona.