Pulsar glitches provide a unique way to study neutron star microphysics because short post-glitch dynamics are directly linked to strong frictional processes on small scales .
To illustrate this connection between macroscopic observables and microphysics , we review calculations of vortex interactions focusing on Kelvin wave excitations and determine the corresponding mutual friction strength for realistic microscopic parameters in the inner crust .
These density-dependent crustal coupling profiles are combined with a simplified treatment of the core coupling and implemented in a three-component neutron star model to construct a predictive framework for glitch rises .
As a result of the density-dependent dynamics , we find the superfluid to transfer angular momentum to different parts of the crust and the core on different timescales .
This can cause the spin frequency change to become non-monotonic in time , allowing for a maximum value much larger than the measured glitch size , as well as a delay in the recovery .
The exact shape of the calculated glitch rise is strongly dependent on the relative strength between the crust and core mutual friction , providing the means to probe not only the crustal superfluid but also the deeper neutron star interior .
To demonstrate the potential of this approach , we compare our predictive model with the first pulse-to-pulse observations recorded during the December 2016 glitch of the Vela pulsar .
Our analysis suggests \textcolor blackthat the glitch rise behavior is relatively insensitive to the crustal mutual friction strength as long as \mathcal { B } \gtrsim 10 ^ { -3 } , while being strongly dependent on the core coupling strength , which we find to be in the range 3 \times 10 ^ { -5 } \lesssim \mathcal { B } _ { core } \lesssim 10 ^ { -4 } .