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The Eclipses of the Close Binary Star BE UMa

Published online by Cambridge University Press:  12 April 2016

Janet H. Wood ,
E. L. Robinson  and
E.-H. Zhang
Janet H. Wood
Affiliation:
Physics Department, Keele University, Keele, ST5 5BG, UK
E. L. Robinson
Affiliation:
Department of Astronomy, University of Texas, Austin, TX 78712, USA
E.-H. Zhang
Affiliation:
Department of Astronomy, University of Texas, Austin, TX 78712, USA

Extract

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BE UMa is a close binary star, not transferring mass, with an extremely hot primary star irradiating the inner face of the cool secondary star. The light curve shows a large-amplitude, sinusoidal variation with a period of 2.29 d, and an eclipse that is centered on the minimum of the variation [1], [3]. According to [1], the eclipse is partial, not total. However, it has been argued [2] that the eclipse was really flat bottomed and thus total. This has important repercussions for the deduced model of the system. To resolve this issue we obtained simultaneous UBVR photometry of BE UMa using the Stiening 4-channel, high-speed photometer on the 82-inch telescope at McDonald Observatory. The mean light curves are shown in Fig. 1. The eclipse in all colours is round bottomed and partial. The different depths are caused by the different contribution from the red secondary star in each bandpass.

Type
Post Common Envelope Binaries & Evolution
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 471 - 472
Copyright
Copyright © Kluwer 1996

References

1. Ando, H., Okazaki, A., Nishimura, S., 1982, PASJ, 34, 141 Google Scholar
2. Crampton, D., Cowley, A.P., Hutchings, J.B., 1983, Ap. J., 272, 202 Google Scholar
3. Kurochkin, N.E., 1971, Perem. Zvezdy., 18, 85 Google Scholar
4. Wesemael, F., Auer, L.H., van Horn, H.M., et al., 1980, Ap. J. Supp., 43, 159 Google Scholar