Evolution of Primordial Black Holes in a radiation and phantom energy environment

TL;DR

This paper investigates how primordial black holes evolve in a universe with radiation and dark energy characterized by a super-negative equation of state, focusing on accretion, evaporation, and thermodynamic implications.

Contribution

It extends previous models by including phantom energy effects and analyzes their impact on black hole mass evolution and thermodynamics.

Findings

Radiation accretion becomes negligible after a certain epoch.

Hawking evaporation can be significant depending on black hole mass.

Phantom energy influences late-time black hole dynamics and thermodynamics.

Abstract

In this work we extend previous work on the evolution of a Primordial Black Hole (PBH) to address the presence of a dark energy component with a super-negative equation of state as a background, investigating the competition between the radiation accretion, the Hawking evaporation and the phantom accretion, the latter two causing a decrease on black hole mass. It is found that there is an instant during the matter-dominated era after which the radiation accretion becomes negligible compared to the phantom accretion. The Hawking evaporation may become important again depending on a mass threshold. The evaporation of PBHs is quite modified at late times by these effects, but only if the Generalized Second Law of thermodynamics is violated.