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We consider a mechanism by which most of the magnetic field in the core of a spinning-down neutron star can be driven out from the core on a time scale of a few million years but will leave a residual field ≥10 8 G on the Hubble time scale (∼3×10 10 yr). Such a driving force arises from the fact that the magnetized vortices of the 3 P 2 neutron superfluid are effectively pinned by the magnetic fluxoids of the 1 S 0 proton superconducting fluid

The magnetized vortex lines of the 3 P 2 paired neutron superfluid are effectively pinned by the magnetic energy barriers produced by the flux tubes of the 1 S 0 paired proton superconducting fluid. The stellar crust and the core superfluid can be coupled primarily via thermal vortex creep against the barriers. The postglitch relaxation of the core superfluid is studied by using the thermal vortex creep model in the limit where the motion of flux tubes is slow compared with that of the vortex lines

The production mechanisms of medium-energy γ-rays from accreting X-ray pulsars are studied. The models concern electrons accelerated in strongly shielded accelerators above the inner part of the accretion disk whose energies are limited by curvature radiation reaction. The curvature photons are sufficiently energetic to produce secondary e ± pairs in collisions with the hard X-rays from the accretion shock front above the neutron star surface outside the acceleration regions, which are shielded from X-rays