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Modeling mass loss from B(e) starsIt was suggested by Zickgraf et al. (1986) that the outer atmospheres of some B(e) stars have a two-component structure: a fast, radiation-driven wind from the pole, and a dense, slow outflow from the equator. Poe et al. (1989) developed this theory to explain the momentum problem associated with WR stars. This paper uses the multiforce wind theory of Poe et al. to model the B(e) outflow phenomenon. Two general questions are investigated: (1) whether B(e) stars can be rotating near critical speed, and if so, (2) what constraints can be placed on the parameters that determine the two-component flow structure.
Document ID
19900045963
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Cassinelli, J. P.
(Wisconsin Univ. Madison, WI, United States)
Schulte-Ladbeck, R. E.
(Wisconsin Univ. Madison, WI, United States)
Abbott, M.
(Wisconsin, University Madison, United States)
Poe, C. H.
(High Altitude Observatory Boulder, CO, United States)
Date Acquired
August 14, 2013
Publication Date
January 1, 1989
Subject Category
Astrophysics
Meeting Information
Meeting: IAU Colloquium
Location: Val Morin
Country: Canada
Start Date: August 15, 1988
End Date: August 18, 1988
Sponsors: IAU, Universite de Montreal, NSERC, Canadian Institute for Theoretical Astrophysics
Accession Number
90A33018
Funding Number(s)
CONTRACT_GRANT: NAS5-26777
CONTRACT_GRANT: NAGW-422
Distribution Limits
Public
Copyright
Other

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