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An eight year study of the radio emission from the WR binary HD 193793

Published online by Cambridge University Press:  07 August 2017

Robert H. Becker  and
Richard L. White
Robert H. Becker
Affiliation:
Physics Dept., University of California, Davis, CA 95616, USA and Lawrence Livermore National Laboratory/IGPP
Richard L. White
Affiliation:
Space Telescope Science Institute, 3100 San Martin Dr., Baltimore, MD 21218, USA

Abstract

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Although we now know of quite a few WR-O star binary systems, only HD 193793 is well studied across the entire electromagnetic spectrum. Hence it affords us the best opportunity to test various models for the system against a wealth of observational data. In this paper we present the results of 8 years of monitoring the radio flux density from HD 193793 with the VLA. This database is unique both in terms of its dense coverage of an entire binary cycle and because it extends the radio coverage to 2 cm wavelength, a shorter wavelength than previously available. With this data we are able to simultaneously solve for the time dependent attenuation in the system and the intrinsic radio luminosity. The standard model of spherically symmetric colliding winds faces severe difficulties in explaining the observations. We conclude that the radio data are most readily interpreted in the context of a WR star wind which is confined to a disk. A disk model for the WR wind also provides a natural explanation for the sudden formation of dust just after periastron.

Type
Session VII - Hydrodynamics and high-energy physics of colliding winds
Information
Symposium - International Astronomical Union , Volume 163: Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution , 1995 , pp. 450 - 459
Copyright
Copyright © Kluwer 1995 

References

Becker, R.H., White, R.L. 1985, ApJ 297, 649 Google Scholar
Eichler, D., Usov, V. 1993, ApJ 402, 271 Google Scholar
Florkowski, D.R. 1982, in: de Loore, C.W.H. & Willis, A.J. (eds.), Wolf-Rayet Stars: Observations, Physics, Evolution, Proc. IAU Symp No. 99 (Dordrecht: Reidel), p. 63 Google Scholar
McDonald, J.K., 1947, Pub. DAO 7, 311 Google Scholar
Moffat, A.F.J., Lamontagne, R., Williams, P.M., Horn, J., Seggewiss, W. 1987, ApJ 312, 807 Google Scholar
van der Hucht, K.A. 1991, in: van der Hucht, K.A. & Hidayat, B. (eds.), Wolf-Rayet Stars and Interactions with other Massive Stars in Galaxies, Proc. IA U Symp No. 143 (Dordrecht: Kluwer), p. 19 Google Scholar
Williams, P.M., van der Hucht, K.A., van der Woerd, H., Wamsteker, W.M., Geballe, T.R., Garmany, C.D., Pollock, A.M.T. 1987, in Lamers, H.J.G.L.M. & de Loore, C.W.H. (eds.), Instabilities in Luminous Early Type Stars (Dordrecht: Reidel), p. 221 Google Scholar
Williams, P.M., van der Hucht, K.A., Pollock, A.M.T., Florkowski, D.R., van der Woerd, H., Wamsteker, W.M. 1990, MNRAS 243, 662 Google Scholar