Neutron star magnetic field evolution, crust movement, and glitches

Spinning superfluid neutrons in the core of a neutron star interact strongly with coexisting superconducting protons. One consequence is that the outward (inward) motion of core superfluid neutron vortices during spin-down (spin-up) of a neutron star may alter the core's magnetic field. Such core field changes are expected to result in movements of the stellar crust and changes in the star's surface magnetic field that reflect those in the core below. Observed magnitudes and evolution of the spin-down indices of canonical pulsars are understood as a consequence of such surface field changes. If the growing crustal strains caused by the changing core magnetic field configuration in canonical spinning-down pulsars are relaxed by large-scale crust-cracking events, special properties are predicted for the resulting changes in spin period. These agree with various glitch observations, including glitch activity, permanent shifts in spin-down rates after glitches in young pulsars, the intervals between glitches, families of glitches with different magnitudes in the same pulsar, the sharp drop in glitch intervals and magnitudes as pulsar spin periods approach 0.7 s, and the general absence of glitching beyond this period.