  The $\gamma$ Cephei system is one of the most closely bound binary planet
hosts known to date. The companion ($\gamma$ Cep B) to the planet-hosting star
($\gamma$ Cep A) should have truncated any protoplanetary disk around $\gamma$
Cep A, possibly limiting planet formation in the disk. We explore this problem
by calculating the truncation radii of protoplanetary disk models around
$\gamma$ Cep A to determine whether or not there is sufficient material
remaining in the disk to form a planet. We vary the accretion rate and
viscosity parameter of the disk models to cover a range of reasonable
possibilities for the disks properties and determine that for accretion rates
of $\geq 10^{-7}$ M$_{\sun}$/yr and low viscosity parameter, sufficient
material in gas and solids exist for planet formation via core accretion to be
possible. Disk instability is less favored, as this can only occur in the most
massive disk model with an extremely high accretion rate.
