R-mode oscillations and rocket term in rotating superfluid neutron stars

Details R-mode oscillations and rocket term in rotating superfluid neutron stars R-mode oscillations and rocket term in rotating superfluid neutron stars

2010-07-14

arxiv.org/abs/1007.2304v1

Physics

High Energy Physics

High Energy Physics - Phenomenology

15 pages, 2 figures

Scientific paper

We discuss a novel damping mechanism of r-mode oscillations in neutron stars due to processes that change the number of protons, neutrons and electrons. Deviations from equilibrium between the number densities of the various species lead to the appearance in the Euler equations of the system of a dissipative force, the so-called rocket term. Such a force affects the evolution of the r-mode oscillations of a rotating neutron star and we estimate the corresponding damping timescale. In the description of the system we employ a two-fluid model, with one fluid consisting of all the charged components locked together by the electromagnetic interaction, while the second fluid consists of superfluid neutrons. Both components can oscillate and we consider two different kind of r-mode oscillations, one predominantly associated with comoving displacements of the two fluids and a second one associated with countermoving, out of phase, displacements. In the former case we find that the dissipation mechanism associated with the rocket term is not effective in preventing the growth of r-mode instabilities. In the latter case the rocket term prevents the growth of the r-mode instability for temperatures larger than about $10^{9}$ K. In our analysis we include the mutual friction dissipative process between the neutron superfluid and the charged component. In order to simplify the computation we neglect the interaction between the two r-mode oscillations as well as effects related with the crust of the star. Moreover, we use a simplified model of neutron star assuming a uniform mass distribution.

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