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H/He Ratios for WN Stars in the LMC and the Galaxy

Published online by Cambridge University Press:  14 August 2015

Douglas N. Perry  and
Peter S. Conti
Douglas N. Perry
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
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

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The chemical abundances of hydrogen, helium, carbon, nitrogen, and oxygen in the winds of W-R stars bears directly on the problem of their evolutionary stage. The commonly held view that W-R stars are highly evolved objects has been based upon the apparent deficiencies of H in their envelopes and the enhanced strengths of CNO lines in the two sequences WN and WC (e.g. Gamow 1943). The picture that emerges is one in which many W-R stars are in the helium burning phase with the WC types more evolved than the WN stars. for this reason it is important to estimate the H content of as many WR stars as possible.

Type
SESSION 2 — THE CHEMISTRY OF THE WOLF-RAYET STARS
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 109 - 112
Copyright
Copyright © Reidel 1982 

References

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