Fokker-Planck models are used to give estimates for the retention frac
tions for newly born neutron stars in globular clusters as a function
of kick velocity. These can be used to calculate the present-day numbe
rs of neutron stars in globular clusters and to address questions such
as the origin of millisecond pulsars. As an example, the Population I
kick velocity distribution derived by Lyne & Lorimer is used to estim
ate the retained fractions of neutron stars originating as single star
s and in binary systems. For plausible initial conditions fewer than 4
per cent of single neutron stars are retained. The retention fraction
s 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, i.e., high-mass X-ray binaries
. The fraction retained decreases with an increasing number of progeni
tors, but the retention fraction decreases more slowly than the number
of progenitors increases. On balance, more progenitors give more neut
ron stars in the cluster.