On the propagation of a shock wave in solar space

The purpose of the present investigation is to consider the propagation of a MHD strong shock wave, originated by solar flares, through a nonuniform medium of decreasing density into the outwardly flowing solar wind, as it approaches the outer surface of the sun. The flow, behind the shock which assumes self-similar character, is assumed to be isothermal rather than adiabatic. The effect of heat exponent, density exponent, and magnetic field is described in detail through the integral curves. Whitham's (1958) characteristic rule is applied to calculate the shock exponent for different values of the parameter in the undisturbed density law, the heat exponent, and the magnetic field parameter. It is found that the magnetic field modifies the values of the shock exponent.