Structure, maximum mass, and stability of compact stars in f(Q,T) gravity

TL;DR

This paper explores how a modified gravity theory, f(Q,T), affects the structure, maximum mass, and stability of neutron stars, deriving exact solutions and comparing predictions with observational data without assuming specific equations of state.

Contribution

It provides an exact solution in f(Q,T) gravity for neutron stars, showing stability and size differences from GR without relying on equations of state, constrained by pulsar observations.

Findings

Negative ta predicts larger star sizes than GR for same mass.

The model remains stable and consistent with observational constraints.

No equations of state were assumed in deriving the solutions.

Abstract

Physically based changes to general relativity (GR) often predict significant differences in how spacetime behaves near massive neutron stars. One of these modifications is represented by $f(\mathcal{Q}, { \mathcal{T}})$, with $\mathcal{Q}$ being the non-metricity and ${ \mathit{T}}$ representing the energy-momentum tensor trace. This theory is viewed as a neutral expansion of GR. Neutron stars weighing more than 1.8 times the mass of the Sun, when observed as radio pulsars, provide valuable opportunities to test fundamental physics under extreme conditions that are rare in the observable universe and cannot be replicated in experiments conducted on land. We derive an exact solution through utilizing the form $f(\mathcal{Q}, { \mathcal{T}})=\mathcal{Q}+\psi { \mathcal{T}}$, where $\psi$ represents a dimensional expression. We elucidate that all physical quantities within the star can be expressed using the dimensional parameter $\psi$ and the compactness, which is defined as $C=\frac{ 2GM}{Rc^2}$. We set $\psi$ to a maximum value of $\psi_1=\frac{\psi}{\kappa^2}=-0.04$ in the negative range, based on observational constraints related to radius and mass of the pulsar ${\textit SAX J1748.9-2021}$. Here, ${\mathrm \kappa^2}$ represents the coupling constant of Einstein, defined as ${\mathrm \kappa^2=\frac{8\pi G}{c^4}}$. Unlike in GR, the solution we derived results in a stable compact object without violating the conjectured sound speed condition $c_s^2\leq\frac{c^2}3$.It is crucial to mention that no equations of state were assumed in this investigation. Nevertheless, our model fits nicely with linear form. Generally, when $\psi$ is negative, the theory predicts a star with a slightly larger size than GR for the same mass. The difference in predicted size between the theory with a negative $\psi$ and GR for the same mass is attributed to an additional force.