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Optical spectroscopic variability of possible Wolf-Rayet binaries

  • Aaron Flores (a1), Octavio Cardona (a1) and Gloria Koenigsberger (a2)

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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).

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References

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Auer, L.H., Koenigsberger, G. 1994, ApJ 436, 859
Cherepashchuk, A.M., Aslanov, A.A. 1984, ApSS 102, 97
Firmani, C., Koenigsberger, G., Bisiacchi, G.F., Moffat, A.F.J. Issertedt, J. 1980, ApJ 239, 607
St-Louis, N., Dalton, M.J., Marchenko, S.V., Moffat, A.F.J., Willis, A.J. 1995, ApJ 452, L57
Vreux, J.-M., Gosset, E., Bohannan, B., Conti, P.S. 1992, A&A 256, 148

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Optical spectroscopic variability of possible Wolf-Rayet binaries

  • Aaron Flores (a1), Octavio Cardona (a1) and Gloria Koenigsberger (a2)

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