  The neutron star crust is rigid material floating on a neutron-proton liquid
core. As the star's spin rate slows, the changing stellar shape stresses the
crust and causes fractures. These starquakes may trigger pulsar glitches as
well as the jumps in spin-down rate that are observed to persist after some
glitches. Earlier studies found that starquakes in spinning-down neutron stars
push matter toward the magnetic poles, causing temporary misalignment of the
star's spin and angular momentum. After the star relaxes to a new equilibrium
orientation, the magnetic poles are closer to the equator, and the magnetic
braking torque is increased. The magnitude and sign of the predicted torque
changes are in agreement with the observed persistent spin-down offsets. Here
we examine the relaxation processes by which the new equilibrium orientation is
reached. We find that the neutron superfluid in the inner crust slows as the
star's spin realigns with the angular momentum, causing the crust to spin more
rapidly. For plausible parameters the time scale and the magnitude of the
crust's spin up agree with the giant glitches in the Vela and other pulsars.
