Density perturbations in $f(R,\phi)$-gravity with an application to the (varying power)-law model

TL;DR

This paper derives the dynamical equations for density perturbations in general $f(R,)$ gravity models and applies them to a specific (varying power)-law model, showing it can match observational data without fine tuning.

Contribution

The paper provides a general framework for analyzing density perturbations in $f(R,)$ gravity and applies it to a new toy-model, deriving key inflationary parameters and matching observations.

Findings

The model predicts a tensor-to-scalar ratio consistent with observations.

Inflation occurs at an energy scale below the GUT-scale (~10^{14} GeV).

Density perturbations are recovered with high precision without fine tuning.

Abstract

Density perturbations in the cosmic microwave background within general $f(R,\phi)$ models of gravity are investigated. The general dynamical equations for the tensor and scalar modes in any $f(R,\phi)$ gravity model are derived. An application of the equations to the (varying power)-law modified gravity toy-model is then made. Formulas and numerical values for the tensor-to-scalar ratio, the scalar tilt and the tensor tilt are all obtained within this specific model. While the model cannot provide a theoretical reason for the value of the energy scale at which inflation should occur, it is found, based on the latest observations of the density perturbations in the sky, that the model requires inflation to occur at an energy scale less than the GUT-scale; namely, $\sim10^{14}\,{\rm GeV}$. The different energy intervals examined here show that the density perturbations recently obtained from observations are recovered naturally, with very high precision, and without fine tuning the model's parameters.