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The Initial Mass Function of Be Stars

Published online by Cambridge University Press:  26 May 2016

J. Zorec ,
R. Levenhagen ,
J. Chauville ,
Y. Frémat ,
D. Ballereau ,
A. M. Hubert ,
M. Floquet  and
N. V. Leister
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
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
A. M. Hubert
Affiliation:
Observatoire de Paris-Meudon, GEPI, FRE/2459, 92195 Meudon, France
M. Floquet
Affiliation:
Observatoire de Paris-Meudon, GEPI, FRE/2459, 92195 Meudon, France
N. V. Leister
Affiliation:
Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Sao Paulo, Brazil

Abstract

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Allowing for systematic differences in the counting of Be Stars due to their overluminosity, changes produced by their fast rotation on spectral types and time spent in the main sequence, a difference between the IMF (Be) and IMF(B) appears, which indicates that the appearance of the Be phenomenon may relay on differences in the initial star formation conditions.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 83 - 84
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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