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The propagation of a strong magneto-gas dynamic, rotating and gravitating shock wave originating in a stellar interior is considered, when it approaches the surface of the star. The flow behind the shock wave is assumed to be spatially isothermal rather than adiabatic to simulate the conditions of large radiative transfer near the stellar surface. It has been observed that gravitation and rotation have important impact upon the emergence of shock at the surface of the star.

mathematical and computational applications

The Emergence of Spherical Magneto-Gas Dynamic Strong Shock with Radiation near the Surface of a Star with a Rotating , Gravitating, Non-Uniform Atmosphere