Impact of $f(\mathcal{Q})$ Theory on the Stability of Compact Spherical Solutions

TL;DR

This paper investigates the stability and physical viability of compact stars within the $f( ext{Q})$ gravity framework, analyzing their structure, matter content, and stability criteria using specific models and junction conditions.

Contribution

It introduces a specific $f( ext{Q})$ model to study compact star stability, extending previous analyses to non-metricity-based modified gravity theories.

Findings

Compact stars are physically viable in $f( ext{Q})$ gravity.

Stars exhibit stability under sound speed and adiabatic index criteria.

The model satisfies energy and physical bounds.

Abstract

This research paper examines the feasibility and stability of compact stars in the context of $f(\mathcal{Q})$ theory, where $\mathcal{Q}$ represents the non-metricity scalar. To achieve this objective, a static spherical line element is assumed in the interior region and the Schwarzschild spacetime is used in the exterior region of the star. The unknown constants are determined by using the Darmois junction conditions. We consider a specific model of this theory to investigate the viability of compact stars through various physical quantities such as matter contents, energy bounds, anisotropy and state parameters. The stability states for the stellar objects under consideration are determined by the speed of sound and adiabatic index, respectively. The resulting data indicate that the compact stars in this modified framework are physically viable and stable.