  Glitches in the rotational frequency of a spinning neutron star could be
promising sources of gravitational wave signals lasting between a few
microseconds to a few weeks. The emitted signals and their properties depend
upon the internal properties of the neutron star. In neutron stars, the most
important physical properties of the fluid core are the viscosity of the fluid,
the stratification of flow in the equilibrium state and the adiabatic sound
speed. Such models were previously studied by van Eysden and Melatos [73] and
Bennett et al. [26] following simple assumptions on all contributing factors,
in which the post-glitch relaxation phase could be driven by the well-known
process of Ekman pumping [76, 17]. We explore the hydrodynamic properties of
the flow of fluid during this phase following more relaxed assumptions on the
stratification of flow and the pressure-density gradients within the neutron
star than previously studied. We calculate the time-scales of duration as well
as the amplitudes of the resulting gravitational wave signals, and we detail
their dependence on the physical properties of the fluid core. We find that it
is possible for the neutron star to emit gravitational wave signals in a wide
range of decay time-scales and within the detection sensitivity of aLIGO for
selected domains of physical parameters.
