  I present a simplified analytical model that simulates the evolution of the
binary population in a dynamically evolving globular cluster. A number of
simulations have been run spanning a wide range in initial cluster and
environmental conditions by taking into account the main mechanisms of
formation and destruction of binary systems. Following this approach, I
investigate the evolution of the fraction, the radial distribution, the
distribution of mass ratios and periods of the binary population. According to
these simulations, the fraction of surviving binaries appears to be dominated
by the processes of binary ionization and evaporation. In particular, the
frequency of binary systems changes by a factor 1-5 depending on the initial
conditions and on the assumed initial distribution of periods. The comparison
with the existing estimates of binary fractions in Galactic globular clusters
suggests that significant variations in the initial binary content could exist
among the analysed globular cluster. This model has been also used to explain
the observed discrepancy found between the most recent N-body and Monte Carlo
simulations in the literature.
