{ "id": "2206.14188", "version": "v1", "published": "2022-06-28T17:53:00.000Z", "updated": "2022-06-28T17:53:00.000Z", "title": "Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics", "authors": [ "Can Wang", "Feng Chen", "Mingde Ding", "Zekun Lu" ], "comment": "Accepted for publication in ApJ Letters", "categories": [ "astro-ph.SR" ], "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.", "revisions": [ { "version": "v1", "updated": "2022-06-28T17:53:00.000Z" } ], "analyses": { "keywords": [ "magnetic flux rope", "radiative magnetohydrodynamic simulation", "magnetic structure", "plasma thermodynamics", "confined eruption" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }