Kinematics of evaporating black holes

Details Kinematics of evaporating black holes Kinematics of evaporating black holes

2005-11-18

arxiv.org/abs/hep-th/0511182v1

Annals Phys. 321 (2006) 2717-2756

Physics

High Energy Physics

High Energy Physics - Theory

58 pages, 2 figures. Latex 2.09. Figures PNG

Scientific paper

10.1016/j.aop.2005.12.004

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.

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