Simulation of magnetic reconnection with heat conduction

Magnetohydrodynamic (MHD) equations are numerically solved to study 2.5-dim ensional magnetic reconnection with field-aligned heat conduction, which is also compared with the adiabatic case. The dynamical evolution starts afte r anomalous resistivity is introduced into a hydrostatic solar atmosphere w ith a force-free current sheet, which might be similar to the configuration before some solar hares. The results show that two jets (i.e., the outflow s of the reconnection region) appear. The downward jet collides with the cl osed line-tied held lines, and a bright loop is formed with a termination s hock at the loop top. As the reconnection goes on, the loop rises almost un iformly with a speed of tens of km s(-1) and the two footpoints of the loop separate with a speed comparable to the loop rise speed. Besides the appar ent loop motion, the magnetic loops below the loop top shrink weakly. Such a picture is consistent with that given by observations of two-ribbon solar flares. Moreover, the results indicate that the slow MHD shock contributes to the bright loop heating. Some detailed structures of the reconnection p rocess are also discussed.