Optical observations study of W UMa eclipsing binary system of CVN using ASAS, KWS, and SuperWasp archives
Abstract
This study aims to determine the physical and geometrical parameters of the eclipsing binary system DF CVn, and compare three automated sky survey archives (All Sky Automated Survey (ASAS), Kamogata-Kiso-Kyoto Wide-field Survey (KWS), and Super Wide Angle Search for Planets (SuperWASP) for stellar optical observation. The BVR light curves of our system (DF CVn) were obtained on May 2009 from Kottamia Astronomical Observatory (KAO), Egypt, and the V light curves were obtained from the ASAS, KWS, and SuperWASP archives. The asymmetric V light curves were modeled by a dark spot on a more massive component. Furthermore, 103 new times of minima were determined from the SuperWASP observations. Using PHOEBE software, the light curves were analyzed to determine the geometric and photometric parameters of the system. Our results indicate that DF CVn is an A subtype of the UMa eclipsing binary (weak contact), with a mass ratio q =0.357, and its inclination i = 72.58 °. From the O-C curve of the minima times, we found that the orbital period changes (ΔP/P) = -4.5836X10^{-11}.
- Publication:
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Romanian Astronomical Journal
- Pub Date:
- December 2020
- Bibcode:
- 2020RoAJ...30..189A
- Keywords:
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- Variable stars;
- Eclipsing binary;
- W UMa binary system