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R. G. Samec, S. M. Jones, T. Scott, J. Branning, J. Miller (Bob Jones University), D. R. Faulkner (USC, Lancaster), N. C. Hawkins (University of Oklahoma)
We present preliminary analyses of V963 and V965 Cygni based on observations taken at the National Undergraduate Research Observatory (NURO). Our CCD observations were taken 07-12 March 2005 and 19-25 July 2004 by DRF,RGS, and NCH with the Lowell Observatory 31-inch reflector. Standard UBVRI filters were used. Preliminary light curve analyses and updated periodicity studies are presented for these variables.
V963 Cyg (GSC 2656 1995,\alpha(2000) = 19h 44m 04.92s, \delta(2000) = +31 41 50.17) is a detached binary discovered by Wachmann (Ast Abh Ham St VI, #1, 1961). The eclipse depths are nearly equal, ~0.78 and ~0.67 magnitudes in in V in the primary and secondary eclipses, respectively, causing observers to MISTAKINGLY classify it as an Algol-type system. Thus the two stars are similar in temperature and the period has to be DOUBLED. The curves appear fairlysymmetrical with a depressed section following the primary eclipse in R and I about 0.2 phase units wide. In BVRI, 100 to 130 observations were taken along with 75 in U. We determined three new times of minimum light, two secondary eclipses, HJD Min II = 2453207.76857±0.00029d and 2453211.9540±0.0032d, and one primary eclipse HJD Min I = 2453209.86073±0.00095d. A corrected period and an improved ephemeris was computed using available times of minimum light: HJD Min I = 2453209.8616(±0.0011)d + 1.39466792(±0.00000019)*E.
GSC 1419 0091 (Brh V132) [\alpha(2000) = 10h 11m 59.152s,\delta(2000) = +16 52 30.28] is an overcontact binary discovered by Klaus Bernhard (BAV, http://www.var-mo.de/star/brh_v132.htm). We took approximately 60-65 observations in each of B,V,R, and I. We determined four new times of minimum light: HJD Min I = 2453437.8293(±0.0003) and 2453441.8291(±0.0019), and HJD Min II = 2453437.6973(±0.0012) and 2453442.76317(±0.0005). We computed an improved ephemeris from all available times of minimum and low light: HJD Min I = 2452754.4733(±0.0030)d + 0.2667251*E(±0.0000011). The light curves show shallow eclipse amplitudes of 0.46 and 0.43 mags in B and V, respectively, and a time of constant light in the secondary eclipse of 31 m.
We wish to thank the NURO for their allocation of observing time, as well as NASA and the American Astronomical Society for their support in paying for travel and publication expenses.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.