  Treatment of the vortex motion in the superfluids of the inner crust and the
outer core of neutron stars is a key ingredient in modeling a number of pulsar
phenomena, including glitches and magnetic field evolution. After recalculating
the microscopic vortex velocity in the inner crust, we evaluate the velocity
for the vortices in the outer core for the first time. The vortex motion
between pinning sites is found to be substantially faster in the inner crust
than in the outer core, $v_0^{\rm crust} \sim 10^{7}\mbox{\cms} \gg v_0^{\rm
core} \sim 1\mbox{\cms}$. One immediate result is that vortex creep is always
in the nonlinear regime in the outer core in contrast to the inner crust, where
both nonlinear and linear regimes of vortex creep are possible. Other
implications for pulsar glitches and magnetic field evolution are also
presented.
