  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
$\Delta P\slash P = +5.69\times10^{-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
$\Delta$$m_1$$\slash$$m$ $=+5.18\times10^{-8}$ 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.
