Semiclassical S-matrix for black holes
arXiv:1503.07181 · doi:10.1007/JHEP12(2015)002
Abstract
We propose a semiclassical method to calculate S-matrix elements for two-stage gravitational transitions involving matter collapse into a black hole and evaporation of the latter. The method consistently incorporates back-reaction of the collapsing and emitted quanta on the metric. We illustrate the method in several toy models describing spherical self-gravitating shells in asymptotically flat and AdS space-times. We find that electrically neutral shells reflect via the above collapse-evaporation process with probability exp(-B), where B is the Bekenstein-Hawking entropy of the intermediate black hole. This is consistent with interpretation of exp(B) as the number of black hole states. The same expression for the probability is obtained in the case of charged shells if one takes into account instability of the Cauchy horizon of the intermediate Reissner-Nordstrom black hole. Our semiclassical method opens a new systematic approach to the gravitational S-matrix in the non-perturbative regime.
41 pages, 13 figures; Introduction rewritten, references added; journal version
References in corpus (12)
- Subtleties in the quasi-classical calculation of Hawking radiation
- Observation of Incipient Black Holes and the Information Loss Problem
- Black Hole Formation and Classicalization in Ultra-Planckian 2 -> N Scattering
- Problems with Tunneling of Thin Shells from Black Holes
- Towards an S-matrix Description of Gravitational Collapse
- Chaos in the black hole S-matrix
- Quantum Radiation from Quantum Gravitational Collapse
- Restoring predictability in semiclassical gravitational collapse
- On the Mechanism of Hawking Radiation
- Complex trajectories in chaotic dynamical tunneling
- Global geometry of two-dimensional charged black holes
- Transmission through a potential barrier in quantum mechanics of multiple degrees of freedom: complex way to the top