Numerical model for coronal shock wave formation in two-fluid approximation

We present results of modeling of shock waves, generated by coronal transients and expanding flare loops. We consider loss of hydrostatic equilibrium of a magnetic loop as a result of an increase of the magnetic field under the loop and as a result of a flare-induced heating of plasma inside the loop. The expanding magnetic loops act as a piston on coronal plasma and produce shock waves propagating in the solar wind. The shock waves are computed in one-dimensional, two-fluid approximation, by taking into account the processes of turbulent dissipation. The corresponding gas-dynamic equations are solved simultaneously with equations of motion of the magnetic tube to provide a self-consistent picture of the shock formation by the transients.