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The equilibrium state of shock-heated rotating atmosphere under the force of gravitation

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Abstract

Equations are developed to describe the flow of a rotating atmosphere under force of gravitation heated by an arbitrary distribution of cylindrical shock waves. Solutions are obtained for the outer solar atmosphere with a steady mass motion in which the heat supplied by shock wave is balanced by the convective heat loss due to this motion. It is found that, for very large range of shock strength and frequencies, the temperature profile is similar to that predicted by the constant shock-strength hypothesis. This hypothesis is used as the basis of a model of the outer solar atmosphere starting near the solar atmosphere.

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Authors and Affiliations

  1. Dept. of Maths., S.C.P.G. College, Ballia, U.P., India

    Onkar Nath

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  1. Onkar Nath
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Nath, O. The equilibrium state of shock-heated rotating atmosphere under the force of gravitation. Astrophys Space Sci 158, 183–187 (1989). https://doi.org/10.1007/BF00639722

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  • DOI: https://doi.org/10.1007/BF00639722

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