On the dynamics of superfluid neutron star cores

Details On the dynamics of superfluid neutron star cores On the dynamics of superfluid neutron star cores

2001-01-11

arxiv.org/abs/astro-ph/0101193v2

Mon.Not.Roy.Astron.Soc.328:1129,2001

Astronomy and Astrophysics

Astrophysics

14 pages, MNRAS style, no figures

Scientific paper

10.1046/j.1365-8711.2001.04923.x

We discuss the nature of the various modes of pulsation of superfluid neutron stars using comparatively simple Newtonian models. The matter in these stars is described in terms of a two-fluid model, where one fluid is the neutron superfluid, which is believed to exist in the core and inner crust of mature neutron stars, and the other fluid represents a conglomerate of all other constituents (crust nuclei, protons, electrons, etc.). In our model, we incorporate the non-dissipative interaction due to the so-called entrainment effect, whereby the momentum of one constituent (e.g. the neutrons) carries along part of the mass of the other constituent. We show that there is no independent set of propagating g-modes in a superfluid neutron star core. We also approach the toroidal pulsation modes of a slowly rotating superfluid star. We show that the superfluid equations support a new class of r-modes. Finally, the role of the entrainment effect on the superfluid mode frequencies is shown explicitly via solutions to local dispersion relations.

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