An instability of radiative shock wave in the presence of magnetic field

The mathematical modelling of the matter deceleration in a magnetohydrodynamics radiative shock wave was performed. The problem is relevant to classical T Tauri stars. We consider the limit where the initial deceleration and heating of plasma (at the entrance to the cooling zone) occurs in a fast magnetohydrodynamic shock wave. To calculate the intensity of radiative losses we use “real” and “power-law” radiative functions. We determine the stability/instability of the radiative shock wave as a function of parameters of the incoming flow: velocity, strength of the magnetic field, and its inclination to the surface of the star. In a number of simulation runs with the “real” radiative function, we find a simple criterion for stability of the radiative shock wave for infalling matter velocity is $1.3\cdot10^7$ cm/sec.