2001/02/02 by Roberto Casadio
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole thermodynamics #Canonical quantum gravity #Hawking #Hawking radiation #Micro black hole #Noncommutative and Quantum Gravity Theories #Problem of time #Quantum Electrodynamics and Casimir Effect #Quantum gravity #Semiclassical physics #Time evolution #Wheeler–DeWitt equation #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1016/s0370-2693(01)00634-7
published as Phys.Lett. B511 (2001) 285-290 · LaTeX using elsart.sty, 10 pages, 3 EPS figures
arxiv created 2001/02/02 · openalex publication_date 2001/07/01 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The time evolution of black holes involves both the canonical equations of quantum gravity and the statistical mechanics of Hawking radiation, neither of which contains a time variable. In order to introduce the time, we apply the semiclassical approximation to the Hamiltonian constraint on the apparent horizon and show that, when the backreaction is included, it suggests the existence of a long-living remnant, similarly to what is obtained in the microcanonical picture for the Hawking radiation.