Hostname: page-component-848d4c4894-x24gv Total loading time: 0 Render date: 2024-05-29T10:36:17.734Z Has data issue: false hasContentIssue false
  • English
  • Français

The behaviour of λ 4686 line of He II in Wolf-Rayet binaries

Published online by Cambridge University Press:  04 August 2017

B. S. Shylaja
B. S. Shylaja*
Affiliation:
Indian Institute of Astrophysics Koramangala, Bangalore 560034, India

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.

Being one of the brightest lines in emission in the optical region of Wolf-Rayet (WR) stars, the λ4686 line of He II has attracted the attention of many investigators (Sahade, 1958; Ganesh and Bappu, 1967). Here, the binaries with subgroup WN components have been chosen, with periods ranging from 1.64d to 21.63d, for understanding the effect of the companion on the formation of this line.

Type
Mass Loss from Hot Stars
Information
Symposium - International Astronomical Union , Volume 122: Circumstellar Matter , 1987 , pp. 459 - 460
Copyright
Copyright © Reidel 1987 

References

Auer, L.H., van Blerkom, D., 1972, Astrophys. J., 178, 175.CrossRefGoogle Scholar
Ganesh, K.S. Bappu, M.K.V., 1967, Kodaikanal Obs. Bull., Ser A, 185, 104.Google Scholar
Sahade, J., 1958, Mem. Soc. Roy. Sci., Liege, Ser 4e, 20, p.46.Google Scholar
Sahade, B., Wood, F.B., 1980, in Interacting Binary Stars, Pergamon Press, p.101.Google Scholar
Shylaja, B.S., 1986, J. Astrophys. Astron (in press).Google Scholar