  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.
