Abstract A photometric solution of an A-type W UMa binary, GSC 0763–0572, is examined with a revised orbital period. The overcontact degree is found to be f = 40.66%, with a low mass ratio of q = 0.2554. The result demonstrates an unambiguous increase in the orbital period with a relative period change of ΔP/P = +5.69 × 10−7 d yr−1. This indicates that GSC 0763–0572 is undergoing a process of mass transfer from the secondary component to the primary one with a rate of relative mass change of Δm1 /m = +5.18 × 10−8 yr−1 , for a conservative model of mass transfer. We find that GSC 0763–0572 might transform into a rapidly rotating star, if total spin angular momentum increases until it is greater than one-third of the orbital angular momentum, without breaking the contact configuration.

Keywords stars: binaries: close — stars: binaries: eclipsing — stars: individual (GSC 0763–0572)

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