Period Variations in the Close Binary BM UMa

Details Period Variations in the Close Binary BM UMa Period Variations in the Close Binary BM UMa

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010oap....23..148v&link_type=abstract

Odessa Astronomical Publications, vol. 23, p.148-151

Astronomy and Astrophysics

Astronomy

Variable Stars, Stars, Bm Uma, Period Variations, Eclipsing Variables, Binary Systems, Modeling

Scientific paper

We present the results of analysing of the light curve and O-C variations in the eclipsing system BM UMa, based on V-band observations which cover the period from JD 2454933 to 2454961 using two robotic remotely-controlled telescopes of Tzec Maun Observatory (USA) along with observations made with the RK-600 telescope of Odessa Astronomical Observatory. The full light curve displays a total primary eclipse with a duration 0.06 of the period, or 24 minutes, and a partial secondary eclipse, with both maxima of equal magnitude. For our obesrvations, we determined the statistically optimal values of the initial epoch of T0 = 2454944.2814 ± 0.0001 and orbital period of P = 0.d 271226 ± 0.000002. The depths of primary and secondary minima are nearly equal, 0.838m ± 0.006 and 0.m 748 ± 0.006, respectively. The physical parameters of the system were calculated using the Wilson-Devinney code, appended with the Monte Carlo search algorithm. The result establishes BM UMa as a contact system (fillout factor 10.7%) with parameters: mass ratio 0.538 ± 0.001, inclination 86.° 815 ± 0.005, and temperatures of components 4700 ± 20 K and 4510 ± 10 K. The more massive component is larger and cooler. The 72 archival and 11 newly-obtained times of light minimum cover the interval 1961-2010 and allowed us to exclude possible systematic period variations in BM UMa and to determine an initial epoch of HJD 2447927.382 and orbital period of P = 0.2712209 d ± 0.0000006.

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