Abstract Considering neutron star heating by magnetic dipole radiation from 3PF2 superfluid neutron vortices inside the star, we propose a neutron phase oscillation model between the normal neutron Fermi fluid and the 3PF2 superfluid neutron vortices at the transition temperature of Ttrans = (2−3)×108 K. With this model we can qualitatively explain most of the observations on pulsar glitches up to date.
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