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Differential rotation of relativistic superfluid in neutron stars

David Langlois·David M. Sedrakian·Brandon Carter
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Abstract

It is shown how to set up a mathematically elegant and fully relativistic superfluid model that can provide a realistic approximation (neglecting small anisotropies due to crust solidity, magnetic fields, et cetera, but allowing for the regions with vortex pinning) of the global structure of a rotating neutron star, in terms of just two independently moving constituents, one of which represents the differentially rotating neutron superfluid, while the other part represents the combination of all the other ingredients, including the degenerate electrons, the superfluid protons in the core, and the ions in the crust, whose electromagnetic interactions will tend to keep them locked together in a state of approximately rigid rotation. Order of magnitude estimates are provided for relevant parameters such as the resistive drag coefficient and the maximum pinning force.

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David Langlois, David M. Sedrakian, Brandon Carter. 1997-11-05. Differential rotation of relativistic superfluid in neutron stars. https://doi.org/10.1046/j.1365-8711.1998.01575.x

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