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The Relationship of the Oe to the Be Stars

Published online by Cambridge University Press:  14 August 2015

Stewart A. Frost  and
Peter S. Conti
Stewart A. Frost
Affiliation:
Joint Institute for Laboratory Astrophysics University of Colorado and National Bureau of Standards
Peter S. Conti
Affiliation:
Dept. of Physics and Astrophysics University of Colorado, Boulder, Color., U.S.A.

Abstract

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Oe stars are earlier type analogues of the better known Be class. These stars have relatively narrow emission in the hydrogen lines and sometimes in the helium lines, which often appears to be double. In several Oe stars, the emission is intermittent. Other properties of the class include relatively broad absorption lines and luminosities near the main sequence. Line profiles in three representative Oe stars are presented and discussed. The similarity of the spectra of Oe and Be stars suggests that the formation mechanism for the emitting region, whatever it is, must extend to the mid O-type stars, at least.

Type
Part II: Be Stars as Rotating Stars
Information
Symposium - International Astronomical Union , Volume 70: Be and Shell Stars , 1976 , pp. 139 - 147
Copyright
Copyright © Reidel 1976 

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