Stable and self-consistent compact star models in teleparallel gravity

TL;DR

This paper develops stable, self-consistent models of charged compact stars within teleparallel gravity, matching observed pulsar data and analyzing their stability through physical conditions and mass-radius relations.

Contribution

It introduces a new charged star model in teleparallel gravity with specific solutions fitting observed pulsars and analyzes their stability and physical properties.

Findings

Model fits observed pulsar PSR J 1614--2230 data.

Mass-radius relation consistent with observations.

Model demonstrates stability under physical conditions.

Abstract

In the framework of Teleparallel Gravity, we derive a charged non-vacuum solution for a physically symmetric tetrad field with two unknown functions of radial coordinate. The field equations result in a closed-form adopting particular metric potentials and a suitable anisotropy function combined with the charge. Under these circumstances, it is possible to obtain a set of configurations compatible with observed pulsars. Specifically, boundary conditions for the interior spacetime are applied to the exterior Reissner-Nordstr\"om metric to constrain the radial pressure that has to vanish through the boundary. Starting from these considerations, we are able to fix the model parameters. The pulsar $\textit {PSR J 1614--2230}$, with estimated mass $M= 1.97 \pm 0.04\, M_{\circledcirc},$ and radius $R= 9.69 \pm 0.2$ km is used to test numerically the model. The stability is studied, through the causality conditions and adiabatic index, adopting the Tolman-Oppenheimer-Volkov equation. The mass-radius $(M,R)$ relation is derived. Furthermore, the compatibility of the model with other observed pulsars is also studied. We reasonably conclude that the model can represent realistic compact objects.