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Spectroscopy of be stars

Published online by Cambridge University Press:  11 April 2011

J.-P. Rozelot ,
C. Neiner  and
C. Neiner
C. Neiner*
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France
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Abstract

This chapter describes non supergiant B-type stars that show emission lines, called Be stars. The emission is caused by the presence of a circumstellar decretion disk. Many physical phenomena are thought to be involved in these stars, such as rapid rotation, pulsations and magnetic fields, and give rise to variations. Spectroscopy is used as a diagnostic tool to study Be stars, by professional astronomers as well as by amateurs.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 47: Astronomical Spectrography for Amateurs , 2011 , pp. 139 - 163
Copyright
© EAS, EDP Sciences, 2011

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