Wald's entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling

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Date
2009
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Brustein, Ram
Hadad, Merav
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Physical Review D ; 79 (2009), 4. - 044025. - American Physical Society (APS). - ISSN 0556-2821. - eISSN 1089-4918
Abstract
The Bekenstein-Hawking entropy of black holes in Einstein’s theory of gravity is equal to a quarter of the horizon area in units of Newton’s constant. Wald has proposed that in general theories of gravity the entropy of stationary black holes with bifurcate Killing horizons is a Noether charge which is in general different from the Bekenstein-Hawking entropy. We show that the Noether charge entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling on the horizon defined by the coefficient of the kinetic term of a specific metric perturbation polarization on the horizon. We present several explicit examples of static spherically symmetric black holes.
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570 Biosciences, Biology
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ISO 690BRUSTEIN, Ram, Dan GORBONOS, Merav HADAD, 2009. Wald's entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling. In: Physical Review D. American Physical Society (APS). 79(4), 044025. ISSN 0556-2821. eISSN 1089-4918. Available under: doi: 10.1103/PhysRevD.79.044025
BibTex
@article{Brustein2009Walds-51509,
  year={2009},
  doi={10.1103/PhysRevD.79.044025},
  title={Wald's entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling},
  number={4},
  volume={79},
  issn={0556-2821},
  journal={Physical Review D},
  author={Brustein, Ram and Gorbonos, Dan and Hadad, Merav},
  note={Article Number: 044025}
}
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    <dcterms:abstract xml:lang="eng">The Bekenstein-Hawking entropy of black holes in Einstein’s theory of gravity is equal to a quarter of the horizon area in units of Newton’s constant. Wald has proposed that in general theories of gravity the entropy of stationary black holes with bifurcate Killing horizons is a Noether charge which is in general different from the Bekenstein-Hawking entropy. We show that the Noether charge entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling on the horizon defined by the coefficient of the kinetic term of a specific metric perturbation polarization on the horizon. We present several explicit examples of static spherically symmetric black holes.</dcterms:abstract>
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