  The build up of the stress whose relaxation is presumed to account for pulsar
frequency glitches can be attributed to various mechanisms, of which the most
efficient involve differential rotation of the neutron superfluid in the inner
layers of the (magnetically braked) solid crust of a rotating neutron star. In
such a case it is usually supposed that the stress is attributable to pinning
of superfluid vortices to crust nuclei, but it has been suggested that, even if
the pinning effect is too weak, a comparably large stress might still arise
just from the deficit of centrifugal buoyancy in the slowed down crust. The
present work is a re-examination that investigates the way such processes may
be affected by considerations that were overlooked in the previous work --
notably uncertainties about the ``effective'' masses that have to be attributed
to the ``free'' superfluid neutrons to allow for their entrainment by the ionic
crust material. Though restricted to a Newtonian formulation, this analysis
distinguishes more carefully than has been usual between true velocities, which
are contravariantly vectorial, and so called ``superfluid velocities'' that are
proportional to momenta, which are essentially covectorial, a technicality that
is important when more than one independent current is involved. The results
include a Proudman type theorem to the effect that the superfluid angular
velocity must be constant on slightly deformed Taylor cylinders in the force
free case, and it is shown how to construct a pair of integral constants of the
motion that determine the solution for the pinned case assuming beta
equilibrium.
