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Optical spectroscopic variability of possible Wolf-Rayet binaries

Published online by Cambridge University Press:  25 May 2016

Aaron Flores ,
Octavio Cardona  and
Gloria Koenigsberger
Aaron Flores
Affiliation:
Instituto Nacional de Astrofisica Optica y Electronica, Mexico
Octavio Cardona
Affiliation:
Instituto Nacional de Astrofisica Optica y Electronica, Mexico
Gloria Koenigsberger
Affiliation:
Instituto de Astronomia, UNAM, Mexico

Extract

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There are a number of Wolf-Rayet stars which, based on their emission line profile variations, were proposed to be WR+cc systems (Firmani et al. 1980; Cherepashchuk & Aslanov 1984). However, recent intensive monitoring with different observational techniques, has given rise to alternative explanations for the variability in these WR stars including the presence of a disk, rotating jet-like structures (Vreux et al. 1992), and corotating interaction regions (St-Louis et al. 1995).

Type
Part 1. Basic observational properties of Wolf-Rayet stars and other hot massive stars
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 65 - 66
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

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Firmani, C., Koenigsberger, G., Bisiacchi, G.F., Moffat, A.F.J. Issertedt, J. 1980, ApJ 239, 607 Google Scholar
St-Louis, N., Dalton, M.J., Marchenko, S.V., Moffat, A.F.J., Willis, A.J. 1995, ApJ 452, L57 Google Scholar
Vreux, J.-M., Gosset, E., Bohannan, B., Conti, P.S. 1992, A&A 256, 148 Google Scholar