Investigating Stable Quark Stars in Rastall-Rainbow Gravity and Their Compatibility with Gravitational Wave Observations

TL;DR

This paper models stable quark stars within Rastall-Rainbow gravity, demonstrating larger maximum masses compatible with gravitational wave observations, by numerically solving modified TOV equations and analyzing stability criteria.

Contribution

It introduces a novel combined Rastall-Rainbow gravity framework to model quark stars and explores their properties and stability, aligning with recent gravitational wave data.

Findings

Predicts larger maximum masses for quark stars.

Results are compatible with GW190814 and GW170817 constraints.

Provides numerical mass-radius relations for the model.

Abstract

We present a stable model for quark stars in Rastall-Rainbow (R-R) gravity. The structure of this configuration is obtained by utilizing an interacting quark matter equation of state. The R-R gravity theory is developed as a combination of two distinct theories, namely, the Rastall theory and the gravity's rainbow formalism. Depending on the model parameters ($\bar{\lambda}, \eta, \Sigma$), the mass-radius relations are numerically computed for modified Tolman-Oppenheimer-Volkoff (TOV) equations with proper boundary conditions. The stability of equilibrium configuration has been checked through the static stability criterion, adiabatic index and the sound velocity. Our calculations predict larger maximum masses for quark stars, and the obtained results are compatible with accepted masses and radii values, including constraints from GW190814 and GW170817 events in all the studied cases.