Analysis of Charged Compact Stars with Bardeen Black Hole in $f(\mathfrak{Q}, \mathcal{T})$ Gravity

TL;DR

This paper explores the internal structure and physical properties of charged compact stars within the $f( ext{Q}, ext{T})$ gravity framework, employing Bardeen's model and Finch-Skea metric to analyze stability and observational features.

Contribution

It introduces a novel application of $f( ext{Q}, ext{T})$ gravity to charged compact stars using Bardeen's model and Finch-Skea metric, providing new insights into their structure and stability.

Findings

The solutions are physically valid and consistent.

Energy conditions and stability criteria are satisfied.

Mass-radius and redshift properties align with observational expectations.

Abstract

This study investigates the behavior of charged compact stars within the $f(\mathfrak{Q}, \mathcal{T})$ gravitational framework, where $\mathfrak{Q}$ denotes the non-metricity scalar and $\mathcal{T}$ represents the trace of the energy-momentum tensor. Recognized as a promising model for explaining the accelerated expansion of the universe, this approach offers a strong theoretical foundation. A central focus of this research is the application of Bardeen's model to describe the exterior spacetime. Additionally, the study examines the internal structure of compact stars using a solution based on the Finch-Skea metric potential. Various physical properties, including energy density, pressure components, anisotropy, energy conditions and equation of state parameters are analyzed through graphical representations. Equilibrium conditions are explored via the Tolman-Oppenheimer-Volkoff equation while key characteristics such as the mass-radius relationship, compactness, surface redshift and stability criteria based on the causality condition and adiabatic index are thoroughly evaluated. The analysis concludes that the proposed solutions for charged compact stars in this framework are both theoretically consistent and physically valid.