New Photometric Investigation of the G-Type Contact Binary GSC 0763-0572

We present new CCD photometric light curves of the W UMa-type binary system GSC 0763-0572 in the $ V$ , $ R$ , and $ I$ bands. Here, the light curves in the $ R$ and $ I$ bands are the first to be obtained. The primary component of this system belongs to a G-type solar-like star; our new observation indicates that the activities of GSC 0763-0572 may be stable. Based on all available times of the light minimum, we found that the orbital period is variable. The $ O$ $-$ $ C$ curve suggested that the period of GSC 0763-0572 is undergoing a continuous increase at a rate of $ dP/dt$ $ =$ $ +$ 5.81(33) $ \times$ 10 $ ^{-7}$ d yr $ ^{-1}$ . Photometric solutions were derived by using the Wilson–Devinney code. We confirmed that this system is A-subtype overcontact binary with a degree of contact factor of $ f$ $ =$ 31.0% ( $ \pm$ 1.5%), a mass ratio of $ q$ $ =$ 0.2330, and a temperature difference of $ \Delta{T}$ $ =$ 31 K. The long-term increase of the orbital period can be explained by mass transfer from the less-massive component to the more-massive one. It's inferred that GSC 0763-0572 may presently be in an expanding state of thermal relaxation oscillation, and may finally evolve into a rapid-rotating single star.