Abstract
The propagation of a shock-wave, originating in a stellar interior, is considered when it approaches the surface of the star. The flow behind the magnetogasdynamic shock wave is assumed to be spatially isothermal rather than adiabatic to stimulate the conditions of large radiative transfer near the stellar surface. The exact shock-propagation laws obtained by solving the equations in similarity variables, for different values of the parameter δ in the undisturbed density law, ρ0 ∝ γδ
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Verma, B.G., Srivastava, R.C. & Khan, A.H. Strong spherical magnetogasdynamic shock with radiation near the surface of a star. Astrophys Space Sci 97, 137–143 (1983). https://doi.org/10.1007/BF00684616
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DOI: https://doi.org/10.1007/BF00684616