Dynamical Black Hole Emission

TL;DR

This paper investigates the dynamic process of black hole emission in four dimensions using a non-local effective action, revealing how Hawking radiation develops in real-time during black hole formation.

Contribution

It introduces a numerical approach to solve the time-dependent stress tensor equations, demonstrating the dynamical generation of Hawking radiation near the horizon.

Findings

Hawking radiation is generated dynamically during black hole formation.

Outgoing energy flux builds up from zero before the black hole forms.

The study resolves the pre-Hawking radiation issue in static approximations.

Abstract

Semiclassical black hole emission in four spacetime dimensions is studied using a non-local effective action. The field equations that determine the time-dependent renormalized stress tensor are solved numerically for a black hole formed by an ingoing null shock wave, and otherwise smooth initial data. We find that Hawking radiation is generated dynamically near the black hole horizon and freely propagates out to null infinity, resulting in an outgoing energy flux that builds up from zero at early retarded times before the black hole forms. This resolves the long-standing issue of pre-Hawking radiation, suffered by calculations based on a static approximation to the stress tensor in an Unruh state, and paves the way towards four-dimensional black hole evolution with semiclassical back-reaction included.