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Rotational Velocities of “Field” Be Stars

Published online by Cambridge University Press:  26 May 2016

J. Zorec ,
R. Levenhagen ,
J. Chauville ,
F. Royer ,
N. V. Leister ,
Y. Frémat  and
D. Ballereau
J. Zorec
Affiliation:
Institut d'Astrophysique de Paris, UMR7095/CNRS, 98bis bd. Arago, F-75014 Paris, France (zorec@iap.fr)
R. Levenhagen
Affiliation:
Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Sao Paulo, Brazil
J. Chauville
Affiliation:
Observatoire de Paris-Meudon, GEPI, FRE/2459, 92195 Meudon, France
F. Royer
Affiliation:
Observatoire de Genève, 1290 Sauverny, Switzerland
N. V. Leister
Affiliation:
Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Sao Paulo, Brazil
Y. Frémat
Affiliation:
Observatoire de Paris-Meudon, GEPI, FRE/2459, 92195 Meudon, France
D. Ballereau
Affiliation:
Observatoire de Paris-Meudon, GEPI, FRE/2459, 92195 Meudon, France

Abstract

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Distributions of true rotational velocities as a function of spectral type for different luminosity class groups of B and Be Stars are compared. While the distributions for B stars differ clearly from one luminosity class to another, those of Be Stars differ less, which indicates that due to rotational effects many Be Stars are considered more evolved than they actually are. Be Stars ‘select’ a narrow range of true rotational velocities to display the Be phenomenon and those of latter spectral types rotate only marginally faster than the early ones.

Information

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 89 - 90
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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