Neutron Stars in Teleparallel Gravity

TL;DR

This paper investigates neutron stars within teleparallel gravity, using numerical simulations to explore the relationship between gravitational and source angular momentum, and identifies regimes where linear relations hold.

Contribution

It introduces a numerical framework to analyze neutron stars in teleparallel gravity and establishes new relations between gravitational and source angular momentum.

Findings

Linear relation between gravitational angular momentum and moment of inertia

Spatial distribution of gravitational energy depends linearly on squared angular velocity

Identified stable neutron star configurations with specific angular momentum properties

Abstract

In this paper we deal with neutron stars, which are described by a perfect fluid model, in the context of the teleparallel equivalent of general relativity. We use numerical simulations to find the relationship between the angular momentum of the field and the angular momentum of the source. Such a relation was established for each stable star reached by the numerical simulation once the code is fed with an equation of state, the central energy density and the ratio between polar and equatorial radii. We also find a regime where linear relation between gravitational angular momentum and moment of inertia (as well as angular velocity of the fluid) is valid. We give the spatial distribution of the gravitational energy and show that it has a linear dependence with the squared angular velocity of the source.