1999/11/30 by Hiroaki Terashima · 3 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Quantum Electrodynamics and Casimir Effect #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.61.104016
published as Phys.Rev. D61 (2000) 104016 · 28 pages, 5 figures, section 1 and the paragraph before subsection 3.1 are improved and enlarged
arxiv created 2000/01/17 · openalex publication_date 2000/04/25 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We examine the possibility that, when a black hole is formed, the information on the collapsed star is stored as the entanglement entropy between the outside and the thin region (of the order of the Planck length) of the inside of the horizon. For this reason, we call this the entanglement entropy of the black hole ``horizon.'' We construct two models: one is in Minkowski spacetime and the other is in the Rindler wedge. To calculate the entropy explicitly, we assume that the thin regions of the order of the Planck length of the outside and the inside of the horizon are completely entangled by quantum effects. We also use the property of the entanglement entropy that it is symmetric under an interchange of the observed and unobserved subsystems. Our setting and this symmetric property substantially reduce the needed numerical calculations. As a result of our analysis, we can explain the Bekenstein-Hawking entropy itself (rather than its correction by matter fields) in the context of entanglement entropy.