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Luminous Blue Stars: Distribution and Numbers

Published online by Cambridge University Press:  04 August 2017

Catharine D. Garmany
Catharine D. Garmany*
Affiliation:
Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards, Boulder, Colorado 80309

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Because the term “luminous blue stars” is relative, let me begin by delineating what region of the H-R diagram I am considering. For the purpose of this talk, I will discuss primarily 0-type stars, with Teff > 30,000 K and Mbol > − 7, but I will also mention their evolved descendants the B supergiants with 30,000 K > Teff > 10,000 K and Mbol > −8, and their even later evolutionary form, the Wolf-Rayet (W-R) stars with Teff > 30,000 K and uncertain Mbol. Although these stars are not among the visually brightest stars, they are the bolo-metrically most luminous as well as the hottest stars. They are also the most massive. They are an important channel in the metal enrichment in a galaxy through the action of mass loss via stellar winds and their ultimate disruption as supernovae (Maeder 1981). They also contribute in a major way to the energy balance of the interstellar medium (Abbott 1982).

Type
Session 1. Main Sequence and Supergiant Stars - I
Information
Symposium - International Astronomical Union , Volume 116: Luminous Stars and Associations in Galaxies , 1986 , pp. 19 - 30
Copyright
Copyright © Reidel 1986 

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