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It is widely believed that magnetic flux ropes are the key structure of solareruptions; however, their observable counterparts are not clear yet. We study aflare associated with flux rope eruption in a comprehensive radiativemagnetohydrodynamic simulation of flare-productive active regions, especiallyfocusing on the thermodynamic properties of the plasma involved in the eruptionand their relation to the magnetic flux rope. The pre-existing flux rope, whichcarries cold and dense plasma, rises quasi-statically before the eruptiononsets. During this stage, the flux rope does not show obvious signatures inextreme ultraviolet (EUV) emission. After the flare onset, a thin `currentshell' is generated around the erupting flux rope. Moreover, a current sheet isformed under the flux rope, where two groups of magnetic arcades reconnect andcreate 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. Thepost-flare loops give rise to abundant soft X-ray emission. Meanwhile amajority of the plasma hosted in the flux rope is heated to around 1 MK, andthe main body of the flux rope is manifested as a bright arch in cooler EUVpassbands such as AIA 171 \AA~channel.

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