  I present models of disk evolution around young binary stars. I show that the
primary factor in determining circumbinary disk lifetimes is the rate of disk
photoevaporation. I also find that photoevaporative clearing leaves a signature
on the distribution of circumbinary disk lifetimes, with a sharp increase in
disk lifetimes for binary separations a<~0.3-1AU. Observations of young binary
stars can therefore be used to test models of disk evolution, and I show that
current data set a strong upper limit to the rate of on-going photoevaporation
(<1e-9 M_sun/yr). Finally I discuss the implications of these results for
planet formation, and suggest that circumbinary planets around close (a<~1AU)
binaries should be relatively common.
