The dynamics of neutron star crusts: Lagrangian perturbation theory for a relativistic superfluid-elastic system

Abstract

The inner crust of a mature neutron star is composed of an elastic lattice of neutron-rich nuclei penetrated by free neutrons. These neutrons can flow relative to the crust once the star cools below the superfluid transition temperature. In order to model the dynamics of this system, which is relevant for a range of problems from pulsar glitches to magnetar seismology and continuous gravitational-wave emission from rotating deformed neutron stars, we need to understand general relativistic Lagrangian perturbation theory for elastic matter coupled to a superfluid component. This paper develops the relevant formalism to the level required for astrophysical applications.

arXiv comment31 pages, double spacing, minor typos fixed

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Cited by in corpus (21)

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• Relativistic fluid dynamics: physics for many different scales
• Young magnetars with fracturing crusts as fast radio burst repeaters
• Modelling neutron star mountains in relativity
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