Quasi-Normal Modes of General Relativistic Superfluid Neutron Stars

Details Quasi-Normal Modes of General Relativistic Superfluid Neutron Stars Quasi-Normal Modes of General Relativistic Superfluid Neutron Stars

1999-08-12

arxiv.org/abs/gr-qc/9908040v1

Phys.Rev. D60 (1999) 104025

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

31 pages, RevTex, 17 figures

Scientific paper

10.1103/PhysRevD.60.104025

We develop a general formalism to treat, in general relativity, the linear oscillations of a two-fluid star about static (non-rotating) configurations. Such a formalism is intended for neutron stars, whose matter content can be described, as a first approximation, by a two-fluid model: one fluid is the neutron superfluid, which is believed to exist in the core and inner crust of mature neutron stars; the other fluid is a conglomerate of all other constituents (crust nuclei, protons, electrons, etc...). We obtain a system of equations which govern the perturbations both of the metric and of the matter variables, whatever the equation of state for the two fluids. As a first application, we consider the simplified case of two non-interacting fluids, each with a polytropic equation of state. We compute numerically the quasi-normal modes (i.e. oscillations with purely outgoing gravitational radiation) of the corresponding system. When the adiabatic indices of the two fluids are different, we observe a splitting for each frequency of the analogous single fluid spectrum. The analysis also substantiates the claim that w-modes are largely due to spacetime oscillations.

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