  The results of N-body simulations of the expulsion of residual gas from young
globular clusters are presented. Globular clusters with a variety of initial
masses, Galactocentric radii, concentration and initial mass function slope
with star formation efficiencies (SFEs) below 50% were investigated. The
residual gas in the clusters was simply treated as an external potential acting
upon the star particles which was reduced in a number of ways to simulate the
loss of the gas. The states of the clusters after ~50 Myr was compared to the
results of Chernoff & Shapiro (1987) in order to estimate if the clusters would
be able to survive for a Hubble time or would be disrupted. The rapid expulsion
of large amounts of a cluster's initial mass is found to considerably effect
the structures of clusters, but they may be able to survive with SFEs far lower
than 50%. It is suggested that the Galactic globular cluster population could
have formed from a proto-cluster populations with SFEs ~40% and central
densities approximately the same as those found in giant molecular clouds.
