Dynamics of the envelopes of Be stars and shell stars in the equatorial plane - A potential similarity and difference based upon the continuous energy distribution

Details Dynamics of the envelopes of Be stars and shell stars in the equatorial plane - A potential similarity and difference based upon the continuous energy distribution Dynamics of the envelopes of Be stars and shell stars in the equatorial plane - A potential similarity and difference based upon the continuous energy distribution

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...408..646m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 408, no. 2, p. 646-650.

Astronomy and Astrophysics

Astrophysics

6

B Stars, Energy Distribution, Shell Stars, Stellar Envelopes, Stellar Spectra, Binary Stars, Early Stars, Stellar Winds

Scientific paper

The paper determines the additional force, F(x)(r), exclusive of those arising form gravity, rotation, and the gas pressure gradient, which is required in the disk model of Waters et al. (1988, 1991) to produce the radial component of velocity for each of three Be and shell stars. F(x)(r) for the six stars exhibits the same behavior. Between the surface of the star and the turning point F(x)(r) decreases with increasing r but a little less rapidly than does gravity. Beyond the turning point F(x)(r) increases dramatically with r. The normalized F(x)(r) has several characteristic properties. It is suggested that some shell stars have envelopes which are more extended than those of Be stars.

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