  Fokker-Planck models are used to give estimates for the retention fractions
for newly-born neutron stars in globular clusters as a function of kick
velocity. These can be used to calculate the present day numbers of neutron
stars in globular clusters and in addressing questions such as the origin of
millisecond pulsars. As an example, the Population I kick velocity distribution
of Lyne & Lorimer (1994) is used to estimate the retained fractions of neutron
stars originating as single stars and in binary systems. For plausible initial
conditions fewer than 4% of single neutron stars are retained. The retention
fractions from binary systems can be 2 to 5 times higher. The dominant source
of retained neutron stars is found to be through binary systems which remain
bound after the first supernova, ie. high-mass X-ray binaries. The retained
fraction decreases with an increasing number of progenitors, but the retention
fraction decreases more slowly than the number of progenitors increases. On
balance, more progenitors give more neutron stars in the cluster.
