http://arxiv.org/abs/1804.02706
Pulsar glitches provide a unique way to study neutron star microphysics because short post-glitch timescales are directly linked to strong frictional processes on small scales. To illustrate the connection between macroscopic observables and microphysics, we calculate the mutual friction strength associated with Kelvin wave excitation for realistic microscopic parameters. These new density-dependent profiles are then combined with a simple three-component model to study the neutron star glitch rise. We find that the superfluid transfers angular momentum to different parts of the crust and then core during the first $30 \, $s after the onset of the glitch. This causes the spin frequency change to become non-monotonic in time, with a maximum value much larger than the measured glitch size, as well as a possible delay in recovery beyond $30 \, $s. We suggest that future telescopes, like the Square Kilometer Array, might be able to distinguish such coupling profiles and provide constraints on the complex small-scale physics.
V. Graber, A. Cumming and N. Andersson
Tue, 10 Apr 18
7/79
Comments: 7 pages, 1 table, 3 figures, submitted to ApJL