Light equation in eclipsing binary CV Boo: third body candidate in elliptical orbit

Abstract

A short period eclipsing binary star CV Boo is tested for the possible existence of additional bodies in the system with a help of the light equation method. We use data on the moments of minima from the literature as well as from our observations during 2014 May--July. A variation of the CV Boo's orbital period is found with a period of $\approx 75$ d. This variation can be explained by the influence of a third star with a mass of $\approx 0.4M_{\odot }$ in an eccentric orbit with $e\approx 0.9$. A possibility that the orbital period changes on long time scales is discussed. The suggested tertiary companion is near the chaotic zone around the central binary, so CV Boo represents an interesting example to test its dynamical evolution. A list of 14 minima moments of the binary obtained from our observations is presented.

8 pages, 4 figures, 1 table, accepted for publication in Ap&SS

References in corpus (5)

• Tertiary companions to close spectroscopic binaries
• Chaos in the Test Particle Eccentric Kozai-Lidov Mechanism
• Chaotic zones around gravitating binaries
• Tidal and rotational effects in the perturbations of hierarchical triple stellar systems. II. Eccentric systems - the case of AS Camelopardalis
• Absolute properties of the spotted eclipsing binary star CV Bootis

Cited by in corpus (1)

• Timing of AB And eclipses