Modeling and Analyzing Stability of Hybrid Stars within $f(Q)$ Gravity

TL;DR

This paper models hybrid stars containing strange quark matter within $f(Q)$ gravity, analyzing their physical properties, stability, and mass-radius relations, and compares results with observational data of compact stars.

Contribution

It introduces a hybrid star model in $f(Q)$ gravity with strange quark matter and analyzes its physical viability and observational consistency.

Findings

Maximum masses and radii match observational data

Model demonstrates physical stability of hybrid stars

Results support $f(Q)$ gravity as a plausible framework

Abstract

This study uses the Krori-Barua type metric to represent hybrid stars within the $f(Q)$ theory of gravity. We postulate that the hybrid star also contains strange quark matter in addition to regular baryonic matter. To investigate the physical viability of the hybrid star model, we present the graphical behavior of the energy density, radial pressure, and tangential pressure, equation of state parameters, anisotropy, and stability analysis, respectively, by choosing the compact star EXO 1785-248 with a mass of $1.3_{-0.2}^{+0.2}~M_{\odot}$ and radius $8.849_{-0.4}^{+0.4}$ km with five different values of the coupling constants as $a=2$, $a=4$, $a=6$, $a=8$, and $a=10$. The maximum allowed masses and corresponding radii have been calculated using the $M-R$ curve for three different coupling parameter '$a$' values which match the observational data of three distinct compact stars, namely LMC X-4, SMC X-1, and 4U 1538-52. So, the $f(Q)$ theory of gravity can provide results that are plausible for describing the macroscopical characteristics of hybrid star candidates.