Hostname: page-component-745bb68f8f-d8cs5 Total loading time: 0 Render date: 2025-02-03T11:57:31.875Z Has data issue: false hasContentIssue false
  • English
  • Français

Fundamental Parameters of Be Stars Seen Equator-On

Published online by Cambridge University Press:  12 April 2016

J. Zorec ,
Y. Frémat ,
A.M. Hubert  and
M. Floquet
J. Zorec
Affiliation:
Institut d’Astrophysique de Paris, CNRS, France
Y. Frémat
Affiliation:
DASGAL, Observatoire de Paris-Meudon, France
A.M. Hubert
Affiliation:
DASGAL, Observatoire de Paris-Meudon, France
M. Floquet
Affiliation:
DASGAL, Observatoire de Paris-Meudon, France

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The geometric deformation, as well as the non-uniform surface gravity and temperature distributions induced by the fast rotation, are taken into account to determine the fundamental parameters of 10 Be stars seen nearly equator-on. The stars occur in the first half of the main sequence evolutionary span, which suggests that their fast rotation is related to initial formation conditions, rather than to evolutionary effects.

Type
Part 2.2. B-Type Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 244 - 245
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

Chauville, J., Zorec, J., Ballereau, D., et al. 2001, A&A, submittedGoogle Scholar
Divan, L. & Zorec, J. 1982, ESA SP-177, 101 Google Scholar
Hubert, A.M. & Floquet, M. 1998, A&A, 335, 565 Google Scholar
Schaller, G., Schaerer, D., Meynet, G., et al. 1992, A&AS, 96, 269 Google Scholar