Physical properties and the maximum compactness bound of a class of compact stars in $f(Q)$ gravity

TL;DR

This paper investigates the internal structure and physical properties of compact stars within linear $f(Q)$ gravity, deriving a maximum compactness bound and analyzing how modifications affect mass-radius relationships.

Contribution

It introduces a closed-form interior solution for anisotropic stars in linear $f(Q)$ gravity and explores the impact of model parameters on stellar properties and stability.

Findings

Maximum compactness depends on the Vaidya-Tikekar curvature parameter $K$.

Higher $eta$ (or $eta$) values lead to decreased maximum mass and radius.

The model can support low-mass stars and fit observed pulsar data.

Abstract

Motivation: Motivated by the growing interest in understanding the role of non-metricity in describing dense stellar systems, in this paper, we study compact stellar configurations within the framework of linear $f(Q)$ gravity. Methodology: By adopting a linear modification of the form $f(Q) = \alpha Q+\beta$, we analyze the internal structure and physical properties of an anisotropic relativistic star within the framework of $f(Q)$ gravity. We employ the Karmarkar's condition together with the Vaidya-Tikekar metric ansatz to obtain a closed-form interior solution of the star. The interior solution is then matched to the Schwarzschild exterior solution across the boundary of the star. By varying the model parameters, we analyze physical features of the resultant stellar configuration. Results: We note distinctive features in the density, pressure, anisotropy and total mass of the star under a such modification. By enforcing the condition that the central pressure remains finite, we obtain the maximum compactness bound which is shown to depend solely on the Vaidya-Tikekar curvature parameter $K$. We recover the Buchdahl bound for the curvature parameter $K=0$, which corresponds to the solution for an isotropic and homogeneous fluid sphere. Utilizing the energy density and radial pressure profiles, we numerically integrate the modified Tolman-Oppenheimer-Volkoff equations and obtain the mass-radius ($M-R$) relationships for different values of the model parameter $\alpha$. We note that for higher values of $\alpha$, the maximum mass and radius decrease, shifting the stable branch towards ultra-compact configurations. An interesting observation in our analysis is that a linearly modified $f(Q)$ gravity model can support comparatively low mass stars. Utilizing the observed mass of some known pulsars, we demonstrate how our model can be used to fine-tune the radius of the star.