Postglitch behavior of the plasma inside neutron stars

An analytically soluble model of the postglitch response of the quantum plasma inside neutron stars is presented, and the idealizations are discussed. The results support the assumption made in the two-component model that, following a period jump, the plasma spins up to the new angular velocity in a time very short compared to the observed relaxation times, which are presumably due to the neutron superfluid. The plasma spin-up time is likely to be tens of seconds or shorter, for reasonable values of the interior temperature and magnetic-field strength. The plasma spins up by the formation of a boundary layer at the inner crust and suction of fluid into the boundary layer. There are two possible types of layer, depending on whether the magnetic field or the plasma viscosity is primarily responsible. In cooler stars, viscosity is dominant, giving well-known Ekman spin-up. In hotter stars, the magnetic field is the dominant mechanism. In the latter case, the plasma spin-up is oscillatory