# Charged spherically symmetric black holes in $f(R)$ gravity and their stability analysis

## TL;DR

This paper derives new charged black hole solutions in specific $f(R)$ gravity models, analyzes their thermodynamics, stability, and perturbations, revealing conditions for physical viability and potential instabilities related to negative entropy.

## Contribution

It introduces new analytic charged black hole solutions in $f(R)$ gravity with detailed thermodynamic and stability analysis, including conditions for physical parameters and stability criteria.

## Key findings

- Black holes exhibit negative entropy under certain conditions.
- Thermodynamic quantities constrain the parameter $oldsymbol{eta}$ to $0<eta<0.5$.
- Black holes are linearly stable for odd modes with radial speed equal to 1.

## Abstract

A new class of analytic charged spherically symmetric black hole solutions, which behave asymptotically as flat or (A)dS spacetimes, is derived for specific classes of $f(R)$ gravity, i.e., $f(R)=R-2\alpha\sqrt{R}$ and $f(R)=R-2\alpha\sqrt{R-8\Lambda}$, where $\Lambda$ is the cosmological constant. These black holes are characterized by the dimensional parameter $\alpha$ that makes solutions deviate from the standard solutions of general relativity. The Kretschmann scalar and squared Ricci tensor are shown to depend on the parameter $\alpha$ which is not allowed to be zero. Thermodynamical quantities, like entropy, Hawking temperature, quasi-local energy and the Gibbs free energy are calculated. From these calculations, it is possible to put a constrain on the dimensional parameter $\alpha$ to have $0<\alpha<0.5$, so that all thermodynamical quantities have a physical meaning. The interesting result of these calculations is the possibility of a negative black hole entropy. Furthermore, present calculations show that for negative energy, particles inside a black hole, behave as if they have a negative entropy. This fact gives rise to instability for $f_{RR}<0$. Finally, we study the linear metric perturbations of the derived black hole solution. We show that for the odd-type modes, our black hole is always stable and has a radial speed with fixed value equal to $1$. We also, use the geodesic deviation to derive further stability conditions.