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Radio Emission from WR Stars

Published online by Cambridge University Press:  14 August 2015

David E. Hogg
David E. Hogg*
Affiliation:
National Radio Astronomy Observatory

Extract

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In principle radio observations of WR stars offer the best possibility of determining the rate of mass loss, since for a simple model of the extended atmosphere the mass loss rate depends primarily on quantities—the flux density, the velocity, and the distance—which are observable (Barlow 1979). Until now, detections of Wolf-Rayet stars have been limited by the sensitivity and resolution of available telescopes. The advent of the Very Large Array makes a search for emission from a large number of these stars feasible.

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. 221 - 224
Copyright
Copyright © Reidel 1982 

References

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Smith, L. F.: 1973, Proc. IAU Symp. 49, eds. Bappu, M.K.J., Sahade, J. (D. Reidel), pp. 15–36.Google Scholar
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