Self-Interaction Correction to Black Hole Radiance

TL;DR

This paper investigates how accounting for the self-gravitation of radiation modifies black hole emission, leading to non-thermal spectra and altered particle trajectories, with implications for understanding black hole information.

Contribution

It introduces a simplified mode truncation approach to incorporate self-interaction effects into black hole radiation calculations, revealing non-thermal corrections.

Findings

Radiation spectrum becomes non-thermal due to self-gravitation effects.

Particles do not follow geodesics when self-interaction is considered.

Method can be extended to analyze radiation correlations.

Abstract

We consider the modification of the formulas for black hole radiation, due to the self-gravitation of the radiation. This is done by truncating the coupled particle-hole system to a small set of modes, that are plausibly the most significant ones, and quantizing the reduced system. In this way we find that the particles no longer move along geodesics, nor is the action along the rays zero for a massless particle. The radiation is no longer thermal, but is corrected in a definite way that we calculate. Our methods can be extended in a straightforward manner to discuss correlations in the radiation, or between incoming particles and the radiation.