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R. G. Samec, E. Sims, D. Wolfe, N. C. Hawkins (Bob Jones University)
We present here our initial analysis of the near-contact binary, CR Canis Majoris [GSC 5973 1733, \alpha(2000) = 7h 18m 2.14s, \delta(2000) = -19\arcdeg 40' 57.7"]. The observations were taken at CTIO on 26, 27, 29, 30, December 2002 and 1 January 2003, by RGS with the 0.9-m reflector and the CFIM T2K CCD camera in quad mode. About 240 observations were taken in U,Rc and Ic and 220 in B and V. The comparison and check stars were GSC 5973 1418 (\alpha (2000) = 7h 18m 15.25s, \delta(2000) = -19\arcdeg 40' 27.7") and GSC 5973 2291 (\alpha (2000) = 7h 18m 3.86s, \delta(2000) = -19\arcdeg 40' 31.8"), respectively. Mean epochs of minimum light for two primary eclipses, HJD = 2452639.7905(6) and 2452641.6634(8) as well as one secondary eclipse 2452635.7345(7) were calculated. We averaged parabola fits for all bands to obtain these consistent values. We calculated the following ephemerides from all available timings of minimum light:
J.D. Hel Min I = 2452641.6634 (52) + 0.624141545 (23) d*E, (1) and
J.D. Hel Min I = 2452641.66309 (60) + 0.62408 (10) d*E. (2)
Equation (1) represents a fit to all available times of minimum light and equation (2) is from our present observations only. The eclipse depths CR CMa are 0.51 mag and 0.12 mag (V) in the primary and secondary eclipses, respectively. A Binary Maker fit and perhaps a Wilson Code solution will be presented. This work was done as a part of our undergraduate observational astronomy class. We wish to thank Cerro Tololo InterAmerican Observatory for their allocation of observing time, and the grant from NASA administered by the American Astronomical Society which supported this run.
The author(s) of this abstract have provided an email address for comments about the abstract: rsamec@bju.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.