# On $f(R)$ gravity in scalar-tensor theories

## TL;DR

This paper explores $f(R)$ gravity within scalar-tensor theories, analyzing four models' cosmological behavior and inflationary predictions, revealing diverse scalar field dynamics and potential transitions relevant for early-universe cosmology.

## Contribution

It provides a detailed analysis of four $f(R)$ models in scalar-tensor form, including solutions to the Klein-Gordon equation and inflationary parameter calculations.

## Key findings

- Scalar field decays asymptotically in the first model.
- Crossing points of $(t)$ vary with $eta$ in the second model.
- Potential behaviors resemble inflationary potentials in the third model.

## Abstract

We study $f(R)$ gravity models in the language of scalar-tensor theories. The correspondence between $f(R)$ gravity and scalar-tensor theories is revisited since $f(R)$ gravity is a subclass of Brans-Dicke models, with a vanishing coupling constant ($\omega=0$). In this treatment, four $f(R)$ toy models are used to analyze the early-universe cosmology, when the scalar field $\phi$ dominates over standard matter. We have obtained solutions to the Klein-Gordon equation for those models. It is found that for the first model $\left(f(R)=\beta R^{n}\right)$, as time increases the scalar field decreases and decays asymptotically. For the second model $\left(f(R)=\alpha R+\beta R^{n}\right)$ it was found that the function $\phi(t)$ crosses the $t$-axis at different values for different values of $\beta$. For the third model $\left(f(R)=R-\frac{\nu^{4}}{R}\right)$, when the value of $\nu$ is small the potential $V(\phi)$ behaves like the standard inflationary potential. For the fourth model $\left(f(R)=R-(1-m)\nu^{2}\Big(\frac{R}{\nu^{2}}\Big)^{m}-2\Lambda\right)$, we show that there is a transition between $1.5<m<1.55$. The behavior of the potentials with $m<1.5$ is totally different from those with $m>1.55$. The slow-roll approximation is applied to each of the four $f(R)$ models and we obtain the respective expressions for the spectral index $n_{s}$ and the tensor-to-scalar ratio $r$.