Randall-Sundrum Black Holes at Colliders

TL;DR

This paper investigates the evolution and potential stability of black holes produced at colliders within the Randall-Sundrum framework, highlighting the possibility of stable remnants due to microcanonical effects.

Contribution

It introduces the first prediction of stable black hole remnants in the Randall-Sundrum scenario using semiclassical gravity methods.

Findings

Black hole lifetime ~10^{-25}s for 10TeV mass

Microcanonical approach predicts non-evaporating stable remnants

Comparison shows similarities and differences with ADD model results

Abstract

In this paper we calculate the evolution of black holes at colliders in the Randall-Sundrum scenario, taking the effect of accretion from the quark-gluon plasma into account. We calculate the evolution using both the canonical and microcanonical ensemble approaches and compare the results to each other and to the well-known corresponding lifetimes for ADD. We find that for an initial mass of 10TeV the canonical lifetime is of the order of $10^{-25}s$, which is of the same order of magnitude as its ADD counterpart. In the microcanonical approach, like in ADD, the microcanonical deviations from thermality slow down the evaporation of the black hole, but, unlike in ADD, the black hole does not completely evaporate; it tends to a stable final state of 0.16GeV. As far as we are aware this is the first prediction of a stable black hole remnant using semiclassical gravity.