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Evolution of O stars and the WR connection

Published online by Cambridge University Press:  14 August 2015

Peter S. Conti
Peter S. Conti*
Affiliation:
Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards, and Department of Astro-Geophysics, University of Colorado, Boulder, CO 80309

Abstract

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The stellar wind mass loss rates of at least some single Of type stars appear to be sufficient to remove much if not all of the hydrogen-rich envelope such that nuclear processed material is observed at the surface. This highly evolved state can then be naturally associated with classic Population I WR stars that have properties of high luminosity for their mass, helium enriched composition, and nitrogen or carbon enhanced abundances. If stellar wind mass loss is the dominant process involved in this evolutionary scenario, then stars with properties intermediate between Of and WR types should exist. The stellar parameters of luminosity, temperature, mass and composition are briefly reviewed for both types. All late WN stars so far observed are relatively luminous like Of stars, and also contain hydrogen. All early WN stars, and WC stars, are relatively faint and contain little or no hydrogen. The late WN stars seem to have the intermediate properties required if a stellar wind is the dominant mass loss mechanism that transforms an Of star to a WR type.

Type
Session 8: Evolutionary Scenario and the WR Connection
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 431 - 445
Copyright
Copyright © Reidel 1979 

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