IMPLICATIONS OF P-3(2) SUPERFLUIDITY IN THE INTERIOR OF NEUTRON-STARS

The magnetized vortex lines of the 3P2 Paired neutron superfluid are effectively pinned by the magnetic energy barriers produced by the flux tubes of the 1S0 paired proton superconducting fluid. The stellar crust and the core superfluid can be coupled primarily via thermal vortex creep against the barriers. We study the postglitch relaxation of the core superfluid 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. Our model results impose some serious constraints on the strength of the core magnetic field, the internal temperature of the star, and the interaction between neutrons and protons in the regime of nuclear matter density.