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Rotational Velocity Versus Mass Loss in be Stars

Published online by Cambridge University Press:  14 August 2015

V. Doazan ,
M. L. Franco ,
R. Stalio  and
R. N. Thomas
V. Doazan
Affiliation:
Observatoire de Paris, France; Scuola Internazionale Superiore di Studi Avanzati (SISSA), Trieste, Italy; Osservatorio Astronomico and SISSA, Trieste, Italy; Institut d'Astrophysique, Paris, France
M. L. Franco
Affiliation:
Observatoire de Paris, France; Scuola Internazionale Superiore di Studi Avanzati (SISSA), Trieste, Italy; Osservatorio Astronomico and SISSA, Trieste, Italy; Institut d'Astrophysique, Paris, France
R. Stalio
Affiliation:
Observatoire de Paris, France; Scuola Internazionale Superiore di Studi Avanzati (SISSA), Trieste, Italy; Osservatorio Astronomico and SISSA, Trieste, Italy; Institut d'Astrophysique, Paris, France
R. N. Thomas
Affiliation:
Observatoire de Paris, France; Scuola Internazionale Superiore di Studi Avanzati (SISSA), Trieste, Italy; Osservatorio Astronomico and SISSA, Trieste, Italy; Institut d'Astrophysique, Paris, France

Abstract

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C IV and Si IV resonance line profiles of 21 Be, B-shell and normal stars are studied with the aim of detecting evidences for mass loss. We found that almost all our sampled stars are loosing mass. A relation between an estimated lower limit for the rate of mass loss and the observed rotational velocity was searched but not found.

Type
V. Rotation and Binarity
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 319 - 324
Copyright
Copyright © Reidel 1982 

References

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