Kavli Affiliate: Renxin Xu
| Summary:
The starquake model of pulsar glitches is revisited in light of accumulated observational data. A statistical comparison between the time-predictable and the magnitude-predictable models, borrowed from seismology and grounded in the classical spring-slider framework, is performed against a sample of 245 glitch events from 9 pulsars. It is found that the data supports the time-predictable model, i.e., a quake resulting in a glitch could be triggered when the developed stress reaches a critical threshold, $τ_rm c$, while the remaining elastic energy (correspondingly the residual stress, $τ_rm r$) after quakes is not fixed. The critical stress could be the order of $τ_rm csimeq (10^34-10^35) rm dyn,cm^-2$ if the residual stress after a quake with maximum stress drops could be considered negligible (i.e., $τ_rm rsimeq 0$), to explain the glitch amplitudes and the intervals. This $τ_rm c$-value is the order of the shear modulus of strangeon stars, but would be several orders higher than that of conventional neutron stars.
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