Magnetohydrodynamic simulation of a flare including the effect of anisotropic heat conduction, chromo-spheric evaporation, and radiative cooling based on the magnetic reconnection model is performed. In the simulation model the coronal magnetic energy is converted into thermal energy of the plasma by magnetic reconnection. This energy is transported to the chromosphere by heat conduction along magnetic field lines and causes an increase in temperature and pressure of the chromospheric plasma. The pressure gradient force drives upward motion of the plasma toward the corona. i.e. chromospheric evaporation. This enhances the density of the coronal reconnected flare loops, and such evaporated plasma is considered to be the source of the observed soft X-ray emission of a flare. The flare loops filled with evaporated dense plasma cool down due to the radiative cooling effect. EUV emitting post-flare loops thus are reproduced in the simulation.
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