Phase Transition Between superfluid and Normal states of Neutrons in Neutron Stars--The Origin of Glitches of Pulsars

Abstract

Starting from a neutron star heating mechanism by the magnetic dipole radiation from the 3^P_2 neutron superfluid vortices in neutron stars, we propose a neutron phase oscillation model which describes the phase transition between the normal neutron Fermi fluid and the 3^P_2 neutron superfluid vortices at the transition temperature of T_{trans}=(5-6)\times 10^8 K. With this model, we can give qualitative explanation to most of the pulsar glitches observed up to date.