Rapidly rotating stars with optically thin stellar winds

Details Rapidly rotating stars with optically thin stellar winds Rapidly rotating stars with optically thin stellar winds

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...195..145m&link_type=abstract

Astrophysical Journal, vol. 195, Jan. 1, 1975, pt. 1, p. 145-155. Research supported by the National Research Council of Canada

Astronomy and Astrophysics

Astrophysics

32

B Stars, Early Stars, Optical Thickness, Radiation Effects, Stellar Rotation, Stellar Winds, Electron Scattering, Far Ultraviolet Radiation, Momentum Transfer, O Stars, Radiant Cooling, Transonic Flow, Ultraviolet Spectra

Scientific paper

The analysis of Cassinelli and Castor, concerning the role of the radiation field in the heating, cooling, and transfer of momentum to the atmospheres of early-type stars, is extended to the case of rapidly rotating stars in general, and of Be stars in particular. The general equations for steady flow are presented and the solution discussed for flow in the equatorial plane and in the region near the pole under the assumptions of an optically thin wind and radially streaming radiation. Limiting values for the ratio of velocity of escape to mean thermal speed at the sonic point are obtained if transonic flow is to occur. The observational evidence presently available is considered and is shown to support the theoretical predictions.

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