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

Abstract

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.

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

References in corpus (2)

• Elastic or magnetic? A toy model for global magnetar oscillations with implications for QPOs during flares
• Poly-essential and general Hyperelastic World (brane) models

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• Inverse Temperature 4-vector in Special Relativity
• Elastic stars in general relativity: IV. Axial perturbations
• Modelling the dynamics of superfluid neutron stars