  Population synthesis is used to model the number of neutron stars in globular
clusters that are observed as LMXBs and millisecond PSRs. The dynamical
interaction between binary and single stars in a GC are assumed to take place
with a permanently replenished "background" of single stars whose density
distribution keeps track with the cluster evolution as a whole and evolution of
single stars. We use the hypothesis (Podsiadlowski et al) that NS forming in
binary systems from components with initial masses \sim 8-12 M_\odot during the
electron-capture collapse of the degenerate O-Ne-Mg core do not acquire a high
space velocities (kicks). The remaining NSs (i.e. from single stars with M>8
M_\odot or binary comonents with M>12 M_\odot) are assumed to be born with high
kicks, as found from obsrevations of single pulsars (Hobbs et al. 2005). Under
this assumption, a sizeable fraction of NSs remain in GCs (about 1000 NSs in a
GC with a mass of 5\times 10^5 M_\odot). The number of ms PSRs formed in the
cluster via accretion spin-up in binaries is then about 10, which is consistent
with observations. Our modelling reproduces the observed shape of the X-ray
luminosity function for accreting NSs in binaries with normal and degenerate
components and the distribution of spin periods of ms PSRs in GCs under the
assumption of accretion-driven magnetic field decay of NSs up to a bottom value
of 10^8 G. The number of LMXBs and ms PSRs dynamically expelling from GCs is
also calculated.
