  We study the dynamical evolution of globular clusters using our 2D Monte
Carlo code with the inclusion of primordial binary interactions for equal-mass
stars. We use approximate analytical cross sections for energy generation from
binary-binary and binary-single interactions. After a brief period of slight
contraction or expansion of the core over the first few relaxation times, all
clusters enter a much longer phase of stable "binary burning" lasting many tens
of relaxation times. The structural parameters of our models during this phase
match well those of most observed globular clusters. At the end of this phase,
clusters that have survived tidal disruption undergo deep core collapse,
followed by gravothermal oscillations. Our results clearly show that the
presence of even a small fraction of binaries in a cluster is sufficient to
support the core against collapse significantly beyond the normal core collapse
time predicted without the presence of binaries. For tidally truncated systems,
collapse is easily delayed sufficiently that the cluster will undergo complete
tidal disruption before core collapse. As a first step toward the eventual goal
of computing all interactions exactly using dynamical three- and four-body
integration, we have incorporated an exact treatment of binary-single
interactions in our code. We show that results using analytical cross sections
are in good agreement with those using exact three-body integration, even for
small binary fractions where binary-single interactions are energetically most
important.
