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Equatorial disk formation around rotating stars due to ram pressure confinement by the stellar windThe 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.
Document ID
19930053268
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Bjorkman, J. E.
(NASA Headquarters Washington, DC United States)
Cassinelli, J. P.
(Wisconsin Univ. Madison, United States)
Date Acquired
August 16, 2013
Publication Date
May 20, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 409
Issue: 1
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A37265
Funding Number(s)
CONTRACT_GRANT: NAGW-422
CONTRACT_GRANT: NAS5-26777
Distribution Limits
Public
Copyright
Other

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