The emergence of a spherical magnetogasdynamic shock wave at the surface of a star

Details The emergence of a spherical magnetogasdynamic shock wave at the surface of a star The emergence of a spherical magnetogasdynamic shock wave at the surface of a star

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..92..359s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 92, no. 2, May 1983, p. 359-364. Research supported by the University Gran

Astronomy and Astrophysics

Astrophysics

1

Magnetohydrodynamic Waves, Shock Wave Propagation, Stellar Models, Density Distribution, Flow Equations, Magnetic Fields, Pressure Distribution, Stellar Interiors, Velocity Distribution

Scientific paper

The propagation of a magnetogasdynamic 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 isothermal rather than adiabatic to stimulate the conditions of large radiative transfer near the stellar surface. The product solution of McVittie has been used to obtain exact solution of the problem. It has been obtained that velocity, density, pressure and magnetic field increases as one moves from shock surface towards the nucleus of the star.

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