  We present a systematic study of the evolution of intermediate- and low-mass
X-ray binaries consisting of an accreting neutron star of mass $1.0-1.8
M_{\odot}$ and a donor star of mass $1.0-6.0 M_{\odot}$. In our calculations we
take into account physical processes such as unstable disk accretion, radio
ejection, bump-induced detachment, and outflow from the $L_{2}$ point.
Comparing the calculated results with the observations of binary radio pulsars,
we report the following results. (1) The allowed parameter space for forming
binary pulsars in the initial orbital period - donor mass plane increases with
increasing neutron star mass. This may help explain why some MSPs with orbital
periods longer than $\sim 60$ days seem to have less massive white dwarfs than
expected. Alternatively, some of these wide binary pulsars may be formed
through mass transfer driven by planet/brown dwarf-involved common envelope
evolution. (2) Some of the pulsars in compact binaries might have evolved from
intermediate-mass X-ray binaries with anomalous magnetic braking. (3) The
equilibrium spin periods of neutron stars in low-mass X-ray binaries are in
general shorter than the observed spin periods of binary pulsars by more than
one order of magnitude, suggesting that either the simple equilibrium spin
model does not apply, or there are other mechanisms/processes spinning down the
neutron stars.
