Interior dynamics of neutral and charged black holes in f(R) gravity

TL;DR

This paper investigates the interior dynamics of neutral and charged black holes within $f(R)$ gravity, analyzing scalar field behavior, singularity formation, and the effects of modifying the gravity model with an $R^2$ term.

Contribution

It provides a detailed simulation of black hole interiors in $f(R)$ gravity, including the impact of scalar fields and modifications to avoid singularities, extending understanding beyond general relativity.

Findings

Scalar field behavior is influenced by the scalar degree of freedom $$, being suppressed or magnified.

Adding an $R^2$ term can prevent Ricci scalar singularities during collapse.

Classical singularities persist in the combined $f(R)+R^2$ gravity model.

Abstract

In this paper, we explore the interior dynamics of neutral and charged black holes in $f(R)$ gravity. We transform $f(R)$ gravity from the Jordan frame into the Einstein frame and simulate scalar collapses in flat, Schwarzschild, and Reissner-Nordstr\"om geometries. In simulating scalar collapses in Schwarzschild and Reissner-Nordstr\"om geometries, Kruskal and Kruskal-like coordinates are used, respectively, with the presence of $f'$ and a physical scalar field being taken into account. The dynamics in the vicinities of the central singularity of a Schwarzschild black hole and of the inner horizon of a Reissner-Nordstr\"om black hole is examined. Approximate analytic solutions for different types of collapses are partially obtained. The scalar degree of freedom $\phi$, transformed from $f'$, plays a similar role as a physical scalar field in general relativity. Regarding the physical scalar field in $f(R)$ case, when $d\phi/dt$ is negative (positive), the physical scalar field is suppressed (magnified) by $\phi$, where $t$ is the coordinate time. For dark energy $f(R)$ gravity, inside black holes, gravity can easily push $f'$ to $1$. Consequently, the Ricci scalar $R$ becomes singular, and the numerical simulation breaks down. This singularity problem can be avoided by adding an $R^2$ term to the original $f(R)$ function, in which case an infinite Ricci scalar is pushed to regions where $f'$ is also infinite. On the other hand, in collapse for this combined model, a black hole, including a central singularity, can be formed. Moreover, under certain initial conditions, $f'$ and $R$ can be pushed to infinity as the central singularity is approached. Therefore, the classical singularity problem, which is present in general relativity, remains in collapse for this combined model.