The Pulsar Population in Globular Clusters and in the Galaxy
  In this paper, I review some of the basic properties of the pulsar population
in globular clusters (GCs) and compare it with the the Galactic disk
population. The neutron stars (NSs) in GCs were likely formed - and appear to
continue forming - in highly symmetric supernovae (SNe), likely from
accretion-induced collapse (AIC). I review the many pulsar finds and discuss
some particularly well populated GCs and why they are so. I then discuss some
particularly interesting objects, like millisecond pulsars (MSPs) with
eccentric orbits, which were heavily perturbed by passing stars. Some of these
systems, like NGC 1851A and NGC 6544B, are almost certainly the result of
exchange interactions, i.e., they are witnesses to the very same processes that
created the large population of MSPs in the first place. I also review briefly
the problem posed by the presence of young pulsars in GCs (with a special
emphasis on a sub-class of young pulsars, the super-energetic MSPs), which
suggest continuing formation of NSs in low-velocity SNe. In the final section,
I discuss the possibility of an analogous population in the Galaxy and
highlight a particularly interesting case, PSR J1903+0327, where the primary
neutron star appears to have formed with a small-velocity kick and small
fractional mass loss. Systems with primary NSs formed in electron-capture SNe
should constitute a distinct low-velocity Galactic population akin in many
respects to the GC population. Current high-resolution surveys of the Galactic
plane should be able to detect it clearly.
