The criteria of the anisotropic quark star models in Rastall gravity

TL;DR

This paper explores the internal structure and properties of quark stars within Rastall gravity, highlighting deviations from general relativity and analyzing the impact of anisotropic pressure on mass-radius relations.

Contribution

It introduces a model for quark stars in Rastall gravity, deriving hydrostatic equilibrium equations and examining the effects of the Rastall parameter on star properties.

Findings

Rastall gravity causes measurable deviations in quark star mass-radius relations.

Anisotropic pressure significantly influences the internal structure of quark stars.

The model extends understanding of dense matter physics beyond general relativity.

Abstract

Quark stars are terrestrial laboratories to study fundamental physics at ultrahigh densities and temperatures. In this work, we investigate the internal structure and the physical properties of quark stars (QSs) in the Rastall gravity. Rastall gravity is considered a non-conservative theory of gravity, which is an effective gravity theory at high energy density, e.g., relevant to the early universe and dense, compact objects. We derive the hydrostatic equilibrium structure for QSs with the inclusion of anisotropic pressure. More specifically, we find the QS mass-radius relations for the MIT bag model. We focus on the model depending on the Rastall free parameter $\eta$ and examine the deviations from the General Relativity (GR) counterparts.