Propagation of shock waves in hot stars

Details Propagation of shock waves in hot stars Propagation of shock waves in hot stars

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ncimb..70..212o&link_type=abstract

Nuovo Cimento B, Serie 11, vol. 70B, Aug. 11, 1982, p. 212-220.

Astronomy and Astrophysics

Astrophysics

1

Hot Stars, Shock Wave Propagation, Density Distribution, Radiation Pressure, Rankine-Hugoniot Relation

Scientific paper

The method developed by Whitham (1958) is used to study the problem of propagation of shock waves in a hot stellar model. An astrophysical situation in which the radiation flux can be neglected in comparison with radiation energy and radiation pressure is chosen in order to simplify the basic equations and derive the law of propagation of shock waves. The density distribution of the undisturbed gaseous configuration is taken to fall off from the center and the characteristic flow field is much longer than the mean free path of radiation. It is shown that, in the particular one-dimensional plane, model radiation fields retard the growth of shock waves.

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