Some effects of rotation on the structure and dynamics of a radiation-driven wind from a hot star

Details Some effects of rotation on the structure and dynamics of a radiation-driven wind from a hot star Some effects of rotation on the structure and dynamics of a radiation-driven wind from a hot star

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..706m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 15, 1984, p. 706-723. Research supported by the Science Research

Other

24

B Stars, Hot Stars, O Stars, Stellar Envelopes, Stellar Rotation, Stellar Winds, Kinetic Energy, Magnetohydrodynamic Flow, Radiation Pressure, Stellar Structure, Stellar Temperature

Scientific paper

Some of the ways in which rotation modifies a radiation-driven stellar wind, as described by Castor, Abbott, and Klein, are considered. The general equations for flow in the equatorial plane of a rotating nonmagnetic star are presented, and their solution is discussed for isothermal winds. Two cases are considered: winds with kinetic temperature much greater than the effective temperature and winds with kinetic temperature equal to the effective temperature. Differences in the structure and dynamics of the wind in the equatorial region of a rotating star compared with the polar region are also considered. The results are then applied to Be stars. Dynamical evidence supporting the ad hoc, disklike model of part of the circumstellar envelope is discussed. A steady state model for the circumstellar envelope of a Be star, including both the superionized ions and the signatures of the ad hoc, disklike model, is suggested.

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