Kinematics of evaporating black holes
arXiv:hep-th/0511182 · doi:10.1016/j.aop.2005.12.004
Abstract
The correspondence principle and causality divide the spacetime of a macroscopic collapsing mass into three regions: classical, semiclassical, and ultraviolet. The semiclassical region covers the entire evolution of the black hole from the macroscopic to the microscopic scale if the latter is reached. It is shown that the metric in the semiclassical region is expressed purely kinematically through the Bondi charges. The only quantum calculation needed is the one of radiation at infinity. The ultraviolet ignorance of semiclassical theory is irrelevant. The metric with arbitrary Bondi charges is obtained and studied.
arXiv comment58 pages, 2 figures. Latex 2.09. Figures PNG
References in corpus (1)
Cited by in corpus (8)
- Effective Action of Vacuum: Semiclassical Approach
- Towards an S-matrix Description of Gravitational Collapse
- Black hole evaporation in a spherically symmetric non-commutative space-time
- Renormalization group improved black hole space-time in large extra dimensions
- IR Renormalisation of General Effective Actions and Hawking Flux in 2D Gravity Theories
- Post-radiation evolution of black holes
- Evading the Trans-Planckian problem with Vaidya spacetimes
- Quasi-evaporating black holes and cold dark matter