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Observations of pulsar glitches have the potential to provide constraints onthe dynamics of the high density interior of neutron stars. However, to do so,realistic glitch models must be constructed and compared to the data. We take astep towards this goal by testing non-linear models for the mutual frictionforce, which is responsible for the exchange of angular momentum between theneutron superfluid and the observable normal component in a glitch. Inparticular, we consider a non-linear dependence of the drag force on therelative velocity between superfluid vortices and the normal component, inwhich the contributions of both kelvon and phonon excitations are included.This non-linear model produces qualitatively new features, and is able toreproduce the observed bimodal distribution of glitch sizes in the pulsarpopulation. The model also suggests that the differences in size distributionsin individual pulsars may be due to the glitches being triggered in regionswith different pinning strengths, as stronger pinning leads to higher vortexvelocities and a qualitatively different mutual friction coupling with respectto the weak pinning case. Glitches in pulsars that appear to glitchquasi-periodically with similar sizes may thus be due to the same mechanisms assmaller events in pulsars that have no preferred glitch size, but simplyoriginate in stronger pinning regions, possibly in the core of the star.

The effect of non-linear mutual friction on pulsar glitch sizes and rise times