  The presence of protostellar disks can greatly increase the dissipation
during close stellar encounters, leading to the formation of a significant
population of binaries during the initial collapse and virialization of a
cluster. We have used N-body simulations of collapsing globular clusters to
find the major factors that determine the efficiency of binary formation
through star-disk captures. This work serves the dual purpose of verifying the
results of earlier analytic work as well as examining parameters not testable
by that work. As in the earlier work, typical binary fractions of a few percent
are found. For the parameters studied, the results are found to depend
remarkably little upon disk evolution, the mass distribution of the stars, or
their spatial distribution, though distributions in which the stars are highly
clumped yield binary fractions larger by a factor of a few. The direct N-body
integrations limit the models to relatively small values of N. Semiempirical
relations are derived, however, which allow the results to be extrapolated to
values of N appropriate to globular clusters.
