Strong spherical magnetogasdynamic shock with radiation near the surface of a star

Details Strong spherical magnetogasdynamic shock with radiation near the surface of a star Strong spherical magnetogasdynamic shock with radiation near the surface of a star

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..97..137v&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 97, no. 1, Nov. 1983, p. 137-143.

Astronomy and Astrophysics

Astrophysics

1

Magnetohydrodynamic Waves, Shock Wave Propagation, Stellar Models, Equations Of Motion, Pressure Distribution, Radiative Transfer, Runge-Kutta Method, Stellar Interiors, Stellar Magnetic Fields, Velocity Distribution

Scientific paper

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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