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Modeling mass loss from B[e] stars

Published online by Cambridge University Press:  12 April 2016

J.P. Cassinelli ,
R.E. Schulte-Ladbeck ,
C.H. Poe  and
M. Abbott
J.P. Cassinelli
Affiliation:
Department of AstronomyUniversity of Wisconsin-Madison475 N. Charter StreetMadison, WI 53706
R.E. Schulte-Ladbeck
Affiliation:
Department of AstronomyUniversity of Wisconsin-Madison475 N. Charter StreetMadison, WI 53706
C.H. Poe
Affiliation:
Department of AstronomyUniversity of Wisconsin-Madison475 N. Charter StreetMadison, WI 53706
M. Abbott
Affiliation:
Department of AstronomyUniversity of Wisconsin-Madison475 N. Charter StreetMadison, WI 53706

Extract

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It has been suggested by Zickgraf et al. (1986) that the outer atmosphere of some B[e] stars has a two-component structure: a fast, radiation-driven wind from the pole, and a dense, slow outflow from the equator. This is also die basic picture investigated by Poe, Friend, and Cassinelli (1989) (hereafter PFC) to explain the momentum problem associated with Wolf-Rayet stars. Here we apply the PFC multiforce wind theory to model the B[e] outflow phenomenon.

Type
Section I: Main Papers, General Discussions, and Two Panel Discussions
Information
International Astronomical Union Colloquium , Volume 113: Physics of Luminous Blue Variables , 1989 , pp. 121 - 126
Copyright
Copyright © Kluwer 1989

References

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