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Title:
Equatorial disk formation around rotating stars due to Ram pressure confinement by the stellar wind
Authors:
Bjorkman, J. E.; Cassinelli, J. P.
Affiliation:
AA(Wisconsin Univ., Madison), AB(Wisconsin Univ., Madison)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 409, no. 1, p. 429-449. (ApJ Homepage)
Publication Date:
05/1993
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
B STARS, EARLY STARS, ROTATING DISKS, STELLAR ENVELOPES, STELLAR MASS EJECTION, STELLAR ROTATION, STELLAR WINDS, ANGULAR VELOCITY, EMISSION SPECTRA, LINE SPECTRA, STELLAR SPECTRA
DOI:
10.1086/172676
Bibliographic Code:
1993ApJ...409..429B

Abstract

The axisymmetric 2D supersonic solution of a rotating, radiation-driven stellar wind presently obtained by a simple approximation predicts the formation of a dense equatorial disk, when the star's rotation rate lies above a threshold value that depends on the ratio of the wind's terminal speed to the escape speed of the star. The disk is formed because the trajectories of the wind leaving the stellar surface at high latitudes carry it down to the equatorial plane; there, the material passes through a standing oblique shock atop the disk; it is therefore the ram pressure of the polar wind that compresses and confines the disk.

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