Energy-momentum squared symmetric Teleparallel gravity: $f(Q,T_{\mu\nu}T^{\mu\nu})$ gravity

TL;DR

This paper introduces a new modified gravity theory, $f(Q,T_{ ueta}T^{ ueta})$, extending previous models by incorporating non-metricity and matter tensor squared terms, with implications for early universe singularity avoidance and cosmological evolution.

Contribution

The work develops the $f(Q,T_{ ueta}T^{ ueta})$ gravity theory, deriving field equations, exploring vacuum solutions, and analyzing specific models that mimic quantum gravity effects and avoid singularities.

Findings

Admits de-Sitter-like vacuum solutions.

Models show early universe dominance of non-linear corrections.

Theory constrained by energy conditions and observational data.

Abstract

In this work we propose the $f(Q,T_{\mu\nu}T^{\mu\nu})$ gravity as a further extension of the $f(Q)$ and $f(Q,T)$ gravity theories. The action involves an arbitrary function of the non-metricity $Q$ and $T_{\mu\nu}T^{\mu\nu}$ in the gravity Lagrangian. The field equations for the theory are derived in the metric-affine formalism by varying the action with respect to the metric. The theory involves a non-minimal coupling between the geometric and the matter sectors, and hence the covariant divergence of the energy-momentum tensor is non-zero, thus implying the non-conservation of the same. The vacuum solutions of the theory are investigated and it is found that the theory perfectly admits a de-Sitter-like evolution of the universe. The cosmological equations are derived and it is found that there are two correction terms arising as modification of the gravity. Two specific toy models of the form $Q+\eta \left(\textbf{T}^2\right)^{n}$ and $f_{0}Q^{m} \left(\textbf{T}^2\right)^{n}$ are explored to gain further insights into the dynamics of the theory. It is seen that the field equations of both the models have terms similar to those arising from the quantum gravity effects and are thus responsible for the avoidance of singularity. One striking feature of the model is that the non-linear correction terms dominate in the early universe and gradually fade away at later times giving the standard FLRW universe. Solutions for the FLRW equations are found wherever possible and the evolution of the scale factor and the matter-energy density are plotted. Finally, the energy conditions are explored in the background of the theory. Using these conditions and some observational data the theory is considerably constrained.