Anisotropic quark stars in energy-momentum squared gravity with an interacting quark equation of state

TL;DR

This paper explores how anisotropic quark stars modeled with an interacting quark equation of state behave within energy-momentum squared gravity, revealing potential for denser stars than in isotropic models through numerical analysis and comparison with observations.

Contribution

It introduces a novel study of anisotropic quark stars in EMSG, incorporating ${ m O}(m_s^4)$ corrections and analyzing the effects of the GB coupling on star properties.

Findings

Anisotropy allows for denser quark stars in EMSG.

The GB coupling parameter significantly influences the mass-radius relation.

Results are consistent with astronomical observational data.

Abstract

We investigate anisotropic quark stars within the context of energy-momentum squared gravity (EMSG), assuming the internal composition consists of homogeneous, charge-neutral 3-flavor interacting quark matter with ${\cal O}(m_s^4)$ corrections. We performed numerical calculations of the equation of state (EoS) and the modified Tolman-Oppenheimer-Volkoff (TOV) structure equation. Additionally, we discussed the impact of the GB coupling parameter $\alpha $ on the mass-radius relationship. Furthermore, we compared our results with astronomical observational data. Our research offers a new perspective, proposing that in EMSG, accounting for anisotropy could lead to denser stars than in isotropic scenarios.