  Observations of pulsar glitches remain a powerful tool for studying the
interior of neutron stars. Many of the observed glitch properties are shown to
result from the evolution of glitches in the different manifestations of
neutron stars. Specifically, the type of glitches associated with the Crab and
Vela pulsars are explained by this model. We are, also, able to adequately
account for the absence, or very low rate, of glitches among the youngest and
the very old pulsars.
