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Models for Optical and Infrared Polarization from CW1103+254

Published online by Cambridge University Press:  12 April 2016

G. Chanmugam  and
K. Wu
G. Chanmugam
Affiliation:
Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana, U.S.A.
K. Wu
Affiliation:
Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana, U.S.A.

Abstract

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Multiband observations of the AM Herculis-type binary CW1103+254 show significant circular polarization (~ 13%) in the J band. Recently, a model with high temperature (kT ~ 20 keV) and small dimensionless plasma parameter (Λ ~ 10 4) was suggested for the emitting region. However, it gives negligible polarization in the J band. In this paper, a method, in which the J band polarization and the peak frequency v* of the spectrum are taken into account, is used to determine T and Λ. For the viewing angle θ = 80° and the magnetic field B = 30MG, we find that kT = 5.0 keV and Λ = 106. The temperature of the emitting region is close to the value (kT = 8.7 keV) derived for the region emitting cyclotron lines in VV Puppis. If these radiations arise from the post-shock regions, then these temperatures are significantly lower than those predicted by standard accretion models or the shock structure is inhomogenous and more complex than previously assumed.

Type
VI. Magnetic Cataclysmic Systems
Information
International Astronomical Union Colloquium , Volume 93: Cataclysmic Variables: Recent Multi-Frequency Observations and Theoretical Developments , 1987 , pp. 657 - 663
Copyright
Copyright © Reidel 1987

References

Bailey, J. et. al.: 1985, Monthly Notices Roy. Astron. Soc., 215, 179 CrossRefGoogle Scholar
Barrett, P.E. and Chanmugam, G.: 1985, Astrophys. J., 298, 743 CrossRefGoogle Scholar
Chanmugam, G. and Dulk, G.A. : 1981, Astrophys. J., 244, 569 CrossRefGoogle Scholar
Greenstein, J.L. et. al.: 1970, Astrophys. J., 161, 519 CrossRefGoogle Scholar
Lamb, D.Q. : 1985, in Lambs, D.Q. and Patterson, J. (eds.), Cataclysmic Variables and Low-Mass X-Ray Binaries, D. Reidel Publ. Co., Dordrecht, Holland, p. 179.CrossRefGoogle Scholar
Liebert, J. and Stockman, H.S. : 1985, in Lamb, D.Q. and Patterson, J. (eds.), Cataclysmic Variables and Low-Mass X-Ray Binaries, D. Reidel Publ. Co., Dordrecht, Holland, P. 151.CrossRefGoogle Scholar
Schmidt, G.D., Stockman, H.S. and Grandi, S.A. : 1983, Astrophys. J. 271, 735.CrossRefGoogle Scholar
Wickramasinghe, D.T. and Meggitt, S.M.A.: 1982, Monthly Notices Roy. Astron. Soc., 198, 975 CrossRefGoogle Scholar
Wickramasinghe, D.T. and Meggitt, S.M.A.: 1985, Monthly Notices Roy. Astron. Soc., 216, 857.CrossRefGoogle Scholar