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Radio Continuum Measurements of Mass Loss from Wolf-Rayet Stars

Published online by Cambridge University Press:  14 August 2015

David C. Abbott ,
John H. Bieging  and
Ed Churchwell
David C. Abbott
Affiliation:
Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards, Boulder, CO
John H. Bieging
Affiliation:
Radio Astronomy Laboratory, University of California, Berkeley, CA
Ed Churchwell
Affiliation:
Washburn Observatory, University of Wisconsin, Madison, WI

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The Wolf-Rayet phenomenon is defined by the striking emission line spectrum which is observed at UV, optical, and IR wavelengths. The usual interpretation is that this characteristic emission-line spectrum results from a stellar wind which has such a high density that even relatively weak lines are formed in the extended envelope formed by the outflow. This model leads to the expectation that the Wolf-Rayet phenomenon is linked to stars which have very high rates of mass loss. The purpose of this paper is to examine the relationship between the mass loss rate and the spectral appearance of O, Of, and WR stars.

Type
SESSION 3 — MASS-LOSS FROM WR STARS: OBSERVATIONS AND THEORY
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 215 - 220
Copyright
Copyright © Reidel 1982 

References

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