Speaker
Description
In order to increase our understanding of the black hole information loss paradox
it appears mandatory to incorporate backreaction effects into the black hole evaporation process. We propose a natural extension of the well known linear,
backreaction free, perturbation theory of black holes. The extended framework
is based on the reduced phase space approach and therefore is able to reconcile
gauge invariance with higher order perturbation theory. The resulting reduced
Hamiltonian describes the interaction between symmetric ("background") and
non-symmetric ("perturbations") observable modes and can be expanded to any desired order. A given truncation of that Hamiltonian and similar truncations of evaporation sensitive observables such as the apparent horizon area can then be
quantised.
