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The Connection between Classical Be Stars and Herbig Ae/Be Stars

Published online by Cambridge University Press:  12 April 2016

T. Böhm  and
L.A. Balona
T. Böhm
Affiliation:
Laboratoire Astrophysique, Observatoire Midi-Pyrenees, 14 av Edouard Belin, F - 31400 Toulouse, France
L.A. Balona
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory 7935, Cape Town, South Africa

Abstract

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We use a phenomenological approach to derive new constraints on the mass loss mechanisms working in the classical Be and the Herbig Ae/Be stars, which represent two groups of stars located very nearby in the HR diagram. We discuss observational similarities of classical Be and Herbig Be stars on one side, and stress, on the other side, the major differences between Herbig Ae and Herbig Be stars. For further details and a detailed bibliography, see Balona & Böhm (2000). A more quantitative approach will be needed and is deferred to future work.

Type
1. Overview
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 103 - 107
Copyright
Copyright © Astronomical Society of the Pacific 2000

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