  Our recent Newtonian treatment of the smooth-averaged mutual-friction force
acting on the neutron superfluid and locally induced by the pinning of
quantized neutron vortices to proton fluxoids in the outer core of superfluid
neutron stars is here adapted to the general-relativistic framework. We show
how the local nonrelativistic motion of individual vortices can be matched to
the global dynamics of the star using the fully 4D covariant Newtonian
formalism of Carter & Chamel (2004). We derive all the necessary dynamical
equations for carrying out realistic simulations of superfluid rotating neutron
stars in full general relativity, as required for the interpretation of pulsar
frequency glitches. The role of vortex pinning on the global dynamics appears
to be nontrivial.
