  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.
