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X-ray and optical observations of BY Cam

Published online by Cambridge University Press:  12 April 2016

Gavin Ramsay  and
Paul A. Mason
Gavin Ramsay
Affiliation:
Astronomical Institute, The University of Utrecht, Postbus 80000, Utrecht, NL 3508 TA, The Netherlands
Paul A. Mason
Affiliation:
Astronomy Department, Case Western Reserve University, Cleveland, OH 44106, USA

Extract

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We present preliminary results of an analysis of X-ray and optical data of the asynchronous AM Her star BY Cam [1]. We use X-ray data from EXOSAT (0.1… 50 keV), Ginga (1.5… 50 keV) and ROSAT (0.1…2.0 keV) and optical data obtained during a 45-day campaign in 1994.

There are 4 known periods: the orbital period (201.30 m), the spin period of the white dwarf (199.3303 m), a spin-orbit beat period (14.15 d) and a side-band period (197.4 m). The detection of this side-band period lends credence to the theory of [2], who suggest that for a stream accreting, diskless, magnetic CV a frequency, f = 2ωspin − Ωorb (=197.399 m), will appear as a strong spike in the power spectrum for certain systems. Wu & Mason (this volume) discuss a competing model where Pspin = 197.4 m.

Type
Polar Systems
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 213 - 214
Copyright
Copyright © Kluwer 1996

References

1. Mason, P.A., Andronov, I.L., Kolesnikov, S.V., et al. 1995, in “Magnetic Cataclysmic Variables”, eds Buckley, D., Warner, B., ASP Conf. Ser. 85, 493 Google Scholar
2. Wynn, G., King, A.R., 1992, MNRAS, 255, 83 CrossRefGoogle Scholar