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On the energy dissipation of fast hydromagnetic shock waves in the solar chromosphere

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Abstract

MHD equations including dissipation terms are applied to study the most important irreversible processes occurring in fast hydromagnetic shock waves under the conditions of the outer solar atmosphere. The atmosphere is assumed to be permeated by a nearly horizontal, uniform magnetic field, the magnitude and inclination angle of which being parameters of the analysis. Numerical examples, corresponding to situations which might occur in the upper chromosphere, are computed in order to demonstrate the procedure.

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  1. Lehrstuhl für Theoretische Astrophysik, Universität Tübingen, Germany

    R. Mäckle

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  1. R. Mäckle
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Mäckle, R. On the energy dissipation of fast hydromagnetic shock waves in the solar chromosphere. Sol Phys 10, 348–356 (1969). https://doi.org/10.1007/BF00145523

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  • DOI: https://doi.org/10.1007/BF00145523

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