Relativistic mechanics of neutron superfluid in (magneto) elastic star crust

Details Relativistic mechanics of neutron superfluid in (magneto) elastic star crust Relativistic mechanics of neutron superfluid in (magneto) elastic star crust

2006-05-03

arxiv.org/abs/gr-qc/0605024v2

Class.Quant.Grav. 23 (2006) 5367-5388

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

29 pages, Latex. V. 2. Minor changes, matches published version

Scientific paper

10.1088/0264-9381/23/17/015

At densities below the neutron drip threshold, a purely elastic solid model (including, if necessary, a frozen-in magnetic field) can provide an adequate description of a neutron star crust, but at higher densities it will be necessary to allow for the penetration of the solid lattice by an independently moving current of superfluid neutrons. In order to do this, the previously available category of relativistic elasticity models is combined here with a separately developed category of relativistic superfluidity models in a unified treatment based on the use of an appropriate Lagrangian master function. As well as models of the purely variational kind, in which the vortices flow freely with the fluid, such a master function also provides a corresponding category of non-dissipative models in which the vortices are pinned to the solid structure.

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