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Spectroscopic Observations of Be Stars in the Photographic and Visual Regions

Published online by Cambridge University Press:  14 August 2015

Arne Slettebak
Arne Slettebak*
Affiliation:
Perkins Observatory, Ohio State and Ohio Wesleyan Universities, Delaware, Ohio 43015, U.S.A.

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The term “Be star” has been used at times to describe classes of objects which are physically rather different from one another. While it could include early-type supergiant stars with Hα emission, early-type pre-main sequence nebular variables, or quasi-planetary nebulae like MWC 349, I will limit this review paper to a discussion of the “classical” Be stars. These are defined as stars of luminosity classes III to V, usually rapid rotators, which show normal B-type spectra with superposed Balmer (and sometimes Fe II) emission. Included also, however, will be the Oe stars and the A-type shell stars, which seem to represent extensions of the classical Be phenomenon to higher and lower temperatures, respectively.

Type
III. Spectroscopy
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 109 - 124
Copyright
Copyright © Reidel 1982 

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