Primordial black hole formation from a type II perturbation in the absence and presence of pressure

TL;DR

This paper explores the formation of primordial black holes from large primordial curvature fluctuations, classifying different types of perturbations and analyzing their evolution and horizon structures, with implications for understanding early universe black hole genesis.

Contribution

It introduces a classification of primordial curvature fluctuations into type I/II and analyzes their evolution into black holes, establishing equivalence with horizon configurations in dust models and discussing pressure effects.

Findings

Type II fluctuations have a stationary point on the initial slice.

Types I/II and A/B horizon classifications are equivalent in dust models.

Pressure influences the equivalence of these classifications.

Abstract

We investigate primordial black holes (PBHs) formed from extremely large amplitudes of primordial curvature fluctuations, classified as type II. Type II fluctuations differ from type I by the presence of a stationary point on the initial time slice, when we see the areal radius as a function of the radial coordinate. Starting from these type II perturbations to form black holes, the nonlinear evolution governed by the Einstein equations generally results in two distinct types, A and B, of horizon configurations, respectively characterized by the absence and presence of a bifurcating trapping horizon where past and future trapping horizons meet. In this paper, we use the Lemaitre-Tolman-Bondi solution to show that type I/II and type A/B classifications are equivalent for a spherically symmetric dust fluid system, regardless of the fluctuation profile. However, this equivalence does not generally hold in the presence of pressure.