Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-14T09:51:31.191Z Has data issue: false hasContentIssue false
  • English
  • Français

Le Spectre des Etoiles Oe dans le Rouge et le Proche Infrarouge

Published online by Cambridge University Press:  14 August 2015

Y. Andrillat ,
J. M. Vreux  and
M. Dennefeld
Y. Andrillat
Affiliation:
Observatoire de Haute Provence
J. M. Vreux
Affiliation:
Institut d'Astrophysique de Liège
M. Dennefeld
Affiliation:
Institut d'Astrophysique de Paris

Abstract

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.

Among the 0 stars, Conti and Leep (1974) define the Oe class as those stars showing emission in the hydrogen lines but without emission in N III or 4686 He II.

In the blue-red region, aside from the presence of Lambda 4542 in absorption, the overall appearance is similar to Be stars. So far no Oe star has been observed until 1.1 μ: the aim of this paper is to fill this gap. We present observations of Oe stars in the near infra-red region as well as new observations of Hα profiles.

Type
IV. Infrared Observations
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 229 - 233
Copyright
Copyright © Reidel 1982 

References

Andrillat, Y. and Houziaux, L.: 1967, J. Obs. 50, 107 =Publ. OHP 9,n°11.Google Scholar
Conti, P.S. and Leep, E.M.: 1974, Astrophys. J. 193, 113.Google Scholar
Frost, S.A. and Conti, P.S.: 1976,in Slettebak, A.(ed.), Be and shell stars, D. Reidel Publ. Co., Dordrecht-Holland, 139.CrossRefGoogle Scholar
Polidan, R.S. and Peters, G.J.: 1976,in Slettebak, A.(ed.), Be and shell stars, D. Reidel Publ. Co., Dordrecht-Holland, 59.Google Scholar