Quantum evolution of the Hawking state for black holes

We give a general description of the evolving quantum state of a Schwarzschild black hole, in the quantum field theory approximation. Such a time-dependent description is based on introducing a choice of time slices. We in particular consider slices that smoothly cross the horizon, and introduction of stationary such slices simplifies the analysis. This analysis goes beyond standard derivations of Hawking radiation that focus on asymptotic excitations, and in particular gives an evolving state that is regular at the horizon, with no explicit trans-Planckian dependence, and that can in principle be generalized to incorporate interacting fields. It is also argued to be useful in connecting to information-theoretic investigation of black hole evolution. The description of the evolving state depends on the choice of slices as well as coordinates on the slices and mode bases; these choices give different pictures analogous to that of Schrodinger. Evolution does have a simpler appearance in an energy eigenbasis, but such a basis is also singular at the horizon; evolution of regular modes has a more complicated appearance, whose properties may be inferred by comparing with the energy eigenbasis. In a regular description, Hawking quanta are produced in a black hole atmosphere, at scales comparable to the horizon size. This approach is also argued to extend to more general asymptotics, such as that of anti de Sitter space. In the latter context, this analysis provides a description of the Hamiltonian and evolution of a black hole that may be compared to the large -N dynamics of the proposed dual CFT.

Automated summary

In this article, a general description of the evolving quantum state of a Schwarzschild black hole is given using the quantum field theory approximation. The description depends on the choice of time slices, coordinates on the slices and mode bases. The evolving state can simplify the analysis and has connections to information-theoretic investigation of black hole evolution.