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Continuum Flux Excess in Be Stars Determined from Spectral Lines1

Published online by Cambridge University Press:  12 April 2016

J. Zorec ,
D. Ballereau  and
J. Chauville
J. Zorec
Affiliation:
Institut d’Astrophysique de Paris, CNRS, 98bisbd. Arago, F-75014 Paris, France
D. Ballereau
Affiliation:
Observatoire de Paris-Meudon, DASGAL/UMR 8633 du CNRS, F-92195 Meudon Principal Cedex, France
J. Chauville
Affiliation:
Observatoire de Paris-Meudon, DASGAL/UMR 8633 du CNRS, F-92195 Meudon Principal Cedex, France

Abstract

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We study the continuum flux excess at λ4471 by comparing the observed He I λ4471 line profiles with non-LTE model line profiles. Assuming that emission of the Hγ line is formed nearly in the same regions of the circumstellar envelope as those where the visible continuum flux excess rises, we estimate the continuum opacity needed to account for the veiling of the He I λ4471 line. The flux excess so derived is then studied as a function of the stellar aspect angle in an attempt to determine the degree of incidence of the envelope geometry near the central star on the continuum flux of Be stars.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 502 - 505
Copyright
Copyright © Astronomical Society of the Pacific 2000

Footnotes

1

Data obtained at ESO-La Silla (Chile) and OHP (France)

References

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Stee, Ph., Vakili, F., Bonneau, D. et al. 1998, A&A 332, 268 Google Scholar