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Chemical Composition of Wolf-Rayet Stars: Abundant Evidence for Anomalies

Published online by Cambridge University Press:  14 August 2015

C. D. Garmany  and
P. S. Conti
C. D. Garmany
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
P. 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

Extract

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We have observed 45 WN stars in our Galaxy and the LMC with the IUE satellite at a resolution of 6 å. Examination of the spectra reveals surprising differences in line strength, in many cases at a given spectral subtype. This is similar to the description of the visual spectra given by Leep (1982). One generalization that can be made is that the equivalent width of He II λ1640 is correlated with the H/He ratio measured by Perry and Conti (1982), but not with spectral type.

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. 105 - 107
Copyright
Copyright © Reidel 1982 

References

Conti, P. S. 1982, in this volume.Google Scholar
Leep, E. M.: 1982, in this volume.Google Scholar
Nussbaumer, H., Schmutz, W., Smith, L. J. and Willis, A. J. 1981, Astron. Astrophys. Suppl. (in press).Google Scholar
Perry, D. and Conti, P. S. 1982, in this volume.Google Scholar