Stationary structure of relativistic superfluid neutron stars

TL;DR

This paper discusses recent numerical advances in modeling rapidly rotating superfluid neutron stars within general relativity, focusing on two-fluid interactions and configurations with different rotation rates.

Contribution

It presents a detailed numerical framework for modeling superfluid neutron stars with two interacting fluids and explores their stationary configurations in full general relativity.

Findings

Existence of configurations with one fluid in a prolate shape confirmed

Models allow different rotation rates for the two fluids

Progress in numerical methods for superfluid neutron star structure

Abstract

We describe recent progress in the numerical study of the structure of rapidly rotating superfluid neutron star models in full general relativity. The superfluid neutron star is described by a model of two interpenetrating and interacting fluids, one representing the superfluid neutrons and the second consisting of the remaining charged particles (protons, electrons, muons). We consider general stationary configurations where the two fluids can have different rotation rates around a common rotation axis. The previously discovered existence of configurations with one fluid in a prolate shape is confirmed.