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We develop a minimal model for \textit{pulsar glitches} by introducing asolid-crust potential in the three-dimensional (3D) Gross-Pitaevskii-Poissonequation (GPPE), which we have used earlier to study gravitationally boundBose-Einstein Condensates (BECs), i.e., bosonic stars. In the absence of thecrust potential, we show that, if we rotate such a bosonic star, it is threadedby vortices. We then show, via extensive direct numerical simulations (DNSs),that the interaction of these vortices with the crust potential yields (a)stick-slip dynamics and (b) dynamical glitches. We demonstrate that, if enoughmomentum is transferred to the crust from the bosonic star, then the vorticesare expelled from the star and the crust's angular momentum $J_c$ exhibitsfeatures that can be interpreted naturally as glitches. From the time series of$J_c$, we compute the cumulative probability distribution functions (CPDFs) ofevent sizes, event durations, and waiting times. We show that these CPDFs havesignatures of self-organized criticality (SOC), which have been seen inobservations on pulsar glitches.

Rotating self-gravitating Bose-Einstein condensates with a crust: a minimal model for pulsar glitches