Properties of interacting quark star in light of Rastall gravity

TL;DR

This paper investigates the properties of quark stars within Rastall gravity, deriving mass-radius relations, analyzing stability, and comparing results with observational data to assess their viability in a modified gravity context.

Contribution

It introduces a detailed analysis of quark star properties under Rastall gravity, incorporating observational constraints and stability assessments, which is novel compared to previous studies in standard gravity.

Findings

Mass-radius relationships differ from general relativity predictions.

Quark stars can be stable within Rastall gravity under certain parameters.

Model parameters are constrained by GW190425 observational data.

Abstract

This study explores the properties of quark stars (QS) formulated with an interacting quark matter equation of state (EoS) within the framework of Rastall gravity, a modified theory of gravity. We derive the mass-radius relationships and calculate the maximum gravitational masses and their corresponding radii, comparing these results under both Rastall gravity and general relativity. Our analysis incorporates recent observational data, including the GW190425 event, to constrain the model parameters ($\bar{\lambda}, \eta, B_{\rm eff}$). We also assess the stability of these quark stars by evaluating their static stability, adiabatic index, and sound velocity profiles, thus confirming their viability within the modified gravitational framework.