Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics

TL;DR

This study uses radiative magnetohydrodynamic simulations to analyze the magnetic structure and plasma thermodynamics of a flux rope eruption, revealing detailed thermal and emission properties during the eruption process.

Contribution

It provides a comprehensive simulation-based analysis of flux rope eruption, highlighting the thermodynamic evolution and observable signatures in EUV and X-ray emissions.

Findings

Flux rope rises quasi-statically before eruption without EUV signatures.

A current shell and sheet form during eruption, heating plasma to over 10 MK.

Post-flare loops produce abundant soft X-ray emission, while the flux rope remains visible in cooler EUV passbands.

Abstract

It is widely believed that magnetic flux ropes are the key structure of solar eruptions; however, their observable counterparts are not clear yet. We study a flare associated with flux rope eruption in a comprehensive radiative magnetohydrodynamic simulation of flare-productive active regions, especially focusing on the thermodynamic properties of the plasma involved in the eruption and their relation to the magnetic flux rope. The pre-existing flux rope, which carries cold and dense plasma, rises quasi-statically before the eruption onsets. During this stage, the flux rope does not show obvious signatures in extreme ultraviolet (EUV) emission. After the flare onset, a thin `current shell' is generated around the erupting flux rope. Moreover, a current sheet is formed under the flux rope, where two groups of magnetic arcades reconnect and create a group of post-flare loops. The plasma within the `current shell', current sheet, and post-flare loops are heated to more than 10 MK. The post-flare loops give rise to abundant soft X-ray emission. Meanwhile a majority of the plasma hosted in the flux rope is heated to around 1 MK, and the main body of the flux rope is manifested as a bright arch in cooler EUV passbands such as AIA 171 \AA~channel.