Orbital Period Investigation of the RS CVn-Type Binary CG Cygni
Abstract
We collected all minima times of the RS CVn-type binary CG Cyg that we were able to find in the literature and databases. The orbital period variations of the system were examined by analyzing its O - C curves (1) through the weighted least-squares method, and (2) through the first continuous method. It was found that the results obtained from the two methods are different. We compared our results with the former author's work, and drew the orbital-period variation of CG Cyg, which indicates that it undergoes a long-term period increase at a rate of dP/dt = +2.48 × 10-8 d yr-1. We discuss the implications of the result regarding the link between the orbital-period variation and the mass transfer of the system.
- Publication:
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Publications of the Astronomical Society of Japan
- Pub Date:
- December 2012
- DOI:
- 10.1093/pasj/64.6.121
- Bibcode:
- 2012PASJ...64..121S
- Keywords:
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- stars: binaries: eclipsing;
- stars: binaries: orbital period;
- stars: individual (CG Cygni)