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Title: Hawking Radiation without Black Hole Entropy

Abstract

Hawking radiation is a purely kinematic effect that is generic to Lorentzian geometries containing event horizons; it is independent of dynamics. On the other hand, the classical laws of black hole mechanics and the semiclassical laws of black hole thermodynamics are both inextricably linked with dynamics: Black hole entropy is proportional to area (plus corrections) if and only if the dynamics is Einstein-Hilbert (plus corrections). Hawking radiation can occur in physical situations in which the laws of black hole mechanics do not apply, and in physical situations in which the notion of black hole entropy does not even make any sense. {copyright} {ital 1998} {ital The American Physical Society}

Authors:
 [1]
  1. Physics Department, Washington University, Saint Louis, Missouri 63130-4899 (United States)
Publication Date:
OSTI Identifier:
601022
Resource Type:
Journal Article
Journal Name:
Physical Review Letters
Additional Journal Information:
Journal Volume: 80; Journal Issue: 16; Other Information: PBD: Apr 1998
Country of Publication:
United States
Language:
English
Subject:
66 PHYSICS; BLACK HOLES; ENTROPY; RADIATIONS; EINSTEIN FIELD EQUATIONS; GEOMETRY; GENERAL RELATIVITY THEORY; QUANTUM GRAVITY; PERTURBATION THEORY; SEMICLASSICAL APPROXIMATION

Citation Formats

Visser, M. Hawking Radiation without Black Hole Entropy. United States: N. p., 1998. Web. doi:10.1103/PhysRevLett.80.3436.
Visser, M. Hawking Radiation without Black Hole Entropy. United States. https://doi.org/10.1103/PhysRevLett.80.3436
Visser, M. Wed . "Hawking Radiation without Black Hole Entropy". United States. https://doi.org/10.1103/PhysRevLett.80.3436.
@article{osti_601022,
title = {Hawking Radiation without Black Hole Entropy},
author = {Visser, M},
abstractNote = {Hawking radiation is a purely kinematic effect that is generic to Lorentzian geometries containing event horizons; it is independent of dynamics. On the other hand, the classical laws of black hole mechanics and the semiclassical laws of black hole thermodynamics are both inextricably linked with dynamics: Black hole entropy is proportional to area (plus corrections) if and only if the dynamics is Einstein-Hilbert (plus corrections). Hawking radiation can occur in physical situations in which the laws of black hole mechanics do not apply, and in physical situations in which the notion of black hole entropy does not even make any sense. {copyright} {ital 1998} {ital The American Physical Society}},
doi = {10.1103/PhysRevLett.80.3436},
url = {https://www.osti.gov/biblio/601022}, journal = {Physical Review Letters},
number = 16,
volume = 80,
place = {United States},
year = {1998},
month = {4}
}