Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...409..429b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 409, no. 1, p. 429-449.
Astronomy and Astrophysics
Astrophysics
377
B Stars, Early Stars, Rotating Disks, Stellar Envelopes, Stellar Mass Ejection, Stellar Rotation, Stellar Winds, Angular Velocity, Emission Spectra, Line Spectra, Stellar Spectra
Scientific paper
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.
Bjorkman Jon E.
Cassinelli Joe P.
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