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Be Stars in the Magellanic Clouds

Published online by Cambridge University Press:  12 April 2016

Stefan C. Keller ,
M.S. Bessell  and
G.S. DaCosta
Stefan C. Keller
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University
M.S. Bessell
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University
G.S. DaCosta
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University

Abstract

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We present the results of our studies of Be stars within the Magellanic Clouds. We have studied the Be population within four young populous clusters, NGC 330 in the SMC, NGC 1818, 2004 and 2100 in the LMC as well as the field population around NGC 2004. The Be fraction within each cluster is seen to peak towards the luminosity of the main sequence turnoff. The field, which exhibits a large spread of ages, has a Be fraction more uniformly distributed in luminosity. We interpret this difference as evidence for an evolutionary enhancement of the Be phenomenon that occurs towards the end of the main sequence lifetime.

Type
1. Overview
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 75 - 78
Copyright
Copyright © Astronomical Society of the Pacific 2000

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