Instabilities and (anti)-evaporation of Schwarzschild–de Sitter black holes in modified gravity

Abstract

We investigate the future evolution of Nariai black hole which is extremal limit of Schwarzschildde Sitter one in modified gravity. The perturbation equations around Nariai black hole are derived in static and cosmological patches for general F (R)-gravity. The analytical and numerical study of several realistic F (R)-models shows the occurence of rich variety of scenarios: instabilities, celebrated Hawking evaporation and anti-evaporation of black holes. The realization of specific scenario depends on the model under consideration. It is remarkable that the presence of such primordial black holes at current universe may indicate towards the modified gravity which supports the antievaporation as preferable model. As some generalization we extend the study of Nariai black hole evolution to modified Gauss-Bonnet gravity. The corresponding perturbation equations turn out to be much more complicated than in the case of F (R)-gravity. For specific example of modified Gauss-Bonnet gravity we demonstrate that Nariai solution maybe stable.

Anti-Evaporation of Black Holes in Bigravity

“…On the other hand, it has been shown that the anti-evaporation may occur even on the classical level in F (R) gravity theories [47][48][49], although the quantum corrections play an important role in general relativity. The anti-evaporation without the quantum corrections could be due to the change of field equations from the Einstein equation, because the behavior of perturbations depends on the equations of motion.…”

Thermodynamic analysis of topological black holes in Gauss–Bonnet gravity with nonlinear source

“…In this extremal regime, the two horizons have the same temperature and they are in the thermal equilibrium. Using a suitable choice of boundary conditions one may discuss about antievaporation as it happens for Nariai anti-evaporating black holes [60][61][62][63].…”

Influence of modification of gravity on the dynamics of radiating spherical fluids

“…Capozziello et al [34] calculated modified versions of Poisson and Boltzmann dynamical equations for relativistic self-gravitating structures in f (R) gravity and found that some more unstable modes of the evolving systems at N region due to f (R) dark source terms. Sebastiani et al [35] described evolving phases of spherical relativistic systems with f (R) background and found a wide range of different instability regions for the evolving compact systems. Recently, Yousaf and Bhatti [36] explored that some f (R) model configurations would support more compact cylindrical objects with smaller radii as compared to general relativity (GR).…”