New insight into the physical essence of pulsar glitch

Based on the oscillation between the B phase and A phase of ³P₂ neutron superfluid in neutron stars, we propose a new glitch model for young pulsars. According to our model, the glitch is explained as a repeat phenomena from the quasi period ³P₂ neutron superfluid B phase, to A phase, then to B phase (many repeated glitches with quasi-period). With the repeating of the phase transition, the vortex quantum number of ³P₂ neutron superfluid vortices is gradually reduced, and the heating rate ^{ε (B)} in B phase also gets lower and lower. After a number of glitches, the time intervals between successive glitches will gradually become longer, and the glitch amplitude decreases. When the heating rate ^{ε (B)} of an old neutron star becomes lower than the cooling rate of the direct Urca, which can happen in a super-strongmagnetic field, the B phase of the ³P₂ neutron superfluid vortices is no longer returned to the A phase state and the phase oscillation of the system is stopped immediately. The slowing glitch phenomenon of some older pulsars is a natural result of our theory, which means that very old pulsars will no longer present the glitch. Our model will be tested in future pulsar glitch observations.