Strong Energy Condition in $R + R^2$ Gravity

TL;DR

This paper investigates the Strong Energy Condition in $R + eta R^2$ gravity, revealing that the conditions for avoiding singularities differ from Einstein's gravity and depend on spatial curvature and matter density decay rate.

Contribution

It derives modified Strong Energy Conditions for $R + eta R^2$ gravity, showing how they vary with spatial curvature and matter decay rate, impacting singularity predictions.

Findings

For $k<0$, S.E.C. holds for $0 extless n extless 4$

For $k=0$, S.E.C. holds for $1 extless n extless 4$

For $k>0$, S.E.C. holds for $2 extless n extless 4$

Abstract

In this paper, we study Raychaudhuri's equation in the background of $R + \beta R^2$ gravity with a phenomenological matter ($\rho \propto a(t)^{-n}$). We conclude that even though the Strong Energy Condition (S.E.C.) for Einstein's gravity, which guarantees singularity, is $n\geq 2$ for $\rho \propto a(t)^{-n}$, a perturbative analysis of Raychaudhuri's equation in the background of $R + \beta R^2$ gravity reveals that the big bang singularity may not be guaranteed for $n > 4$. We derive the following Strong Energy Conditions for $R + \beta R^2$ ($\beta \not= 0$): 1) For $k<0$ FRW metric, S.E.C. is ($0\leq n\leq 4$) i.e., $-\rho_n \leq p_n \leq {1\over 3}\rho_n$. 2) For $k=0$ FRW metric, S.E.C. is ( $1\leq n\leq 4$) i.e., $-{2\over 3}\rho_n \leq p_n \leq {1\over 3}\rho_n$. 3) For $k>0$ FRW metric, S.E.C. is ($2\leq n\leq 4$) i.e., $-{1\over 3}\rho_n \leq p_n \leq {1\over 3}\rho_n$.