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The Relation Between Mass Loss and Luminosity For Be Stars

Published online by Cambridge University Press:  23 September 2016

L.B.F.M. Waters ,
H.J.G.L.M. Lamers  and
J. Coté
L.B.F.M. Waters
Affiliation:
SRON Laboratory for Space Research, Beneluxlaan 21, 3527 HS Utrecht, Netherlands
H.J.G.L.M. Lamers
Affiliation:
SRON Laboratory for Space Research, Beneluxlaan 21, 3527 HS Utrecht, Netherlands
J. Coté
Affiliation:
SRON Laboratory for Space Research, Beneluxlaan 21, 3527 HS Utrecht, Netherlands

Abstract

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The mass loss rates of a large sample of Be stars derived from the UV and the IR are compared. The IR rates were derived using a simple equatorial disc model, and are typically a factor 100 larger than those derived from the UV. In terms of mass fluxes, the mass flux in the polar regions (derived from the UV observations) is about a factor 103 smaller than the mass flux in the equatorial regions. The dependence of MIR and Muv on stellar luminosity is studied. It is shown that MIR depends weaker on L than Muv. This suggests that two different mechanisms are responsible for the mass flux in polar and equatorial regions.

Type
III. The Circumstellar Gas
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 245 - 249
Copyright
Copyright © Cambridge University Press 1987

References

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