Hostname: page-component-669899f699-qzcqf Total loading time: 0 Render date: 2025-05-02T19:40:41.227Z Has data issue: false hasContentIssue false
  • English
  • Français

BE 381: WN9 or O8 Iafpe?

Published online by Cambridge University Press:  14 August 2015

Bruce Bohannan
Bruce Bohannan*
Affiliation:
Department of Astro-Geophysics, University of Colorado, Boulder, Colorado 80309 USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

As John Hutchings summarized at the opening of this symposium the most easily detected symptom of mass loss in hot stars is emission at Hα. Some years ago I made a survey of the Large Magellanic Cloud for stars with Hα in emission (Bohannan and Epps 1974) and since then have obtained low resolution spectra of some of these stars to establish their spectral identity. I would like to talk today of one of these objects, BE 381, which displays spectroscopic features of both the extreme Of and low excitation WN Wolf-Rayet classifications.

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. 479 - 482
Copyright
Copyright © Reidel 1979 

References

Bohannan, B., and Epps, H. W.: 1974, Astron. Astrophys. Suppl., 18, pp. 47–79.Google Scholar
Conti, P. S.: 1976, Proc. 20th Liege International Astrophysical Colloquium, Mem. Soc. Roy. Sci. Liege 9, pp. 193–212.Google Scholar
Conti, P. S.: 1978, I.A.U. Symposium #80 (in press).Google Scholar
Conti, P. S., and Alschuler, W. R.: 1971, Ap. J. 170, pp. 325–344.Google Scholar
Hutchings, J. B.: 1968, M.N.R.A.S. 141, pp. 219–249.Google Scholar
Walborn, N. R.: 1974, Ap. J. 189, pp. 269–271.CrossRefGoogle Scholar
Walborn, N. R.: 1977, Ap. J. 215, pp. 53–61.CrossRefGoogle Scholar
Westerlund, B.E., and Smith, L. F.: 1964, M.N.R.A.S. 128, pp. 311–325.Google Scholar