Dynamics of the envelopes of Be stars in the equatorial plane

Details Dynamics of the envelopes of Be stars in the equatorial plane Dynamics of the envelopes of Be stars in the equatorial plane

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...384..605c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 384, Jan. 10, 1992, p. 605-612. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

16

B Stars, Radiative Transfer, Stellar Envelopes, Stellar Motions, Stellar Spectra, Dynamic Models, Emission Spectra, Line Spectra, Stellar Models

Scientific paper

The dynamics in the equatorial plane of models for the envelopes of Be stars has been investigated first by inverting the equation of motion to solve for the unknown force, Fx(r), in addition to those arising from gravitation, rotation, and gas pressure gradient, required to produce a radial component of velocity having an assumed functional form. Fx(r) is then determined for both a beta velocity and a power-law velocity dependence, and for each investigated the consequences for Fx(r) of the assumptions of angular momentum conservation, Keplerian rotation, and the variation of kinetic temperature with r. Between the surface of the star and a turning point of order of 10-100 stellar radii, Fx(r) decreases with increasing r, but less rapidly than does gravity. Beyond the turning point, Fx(r) increases with r at least initially; however, it may again decrease with further increases in r. Several physical effects, one or more of which may be responsible for this common form of Fx(r), are discussed.

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