Black Hole Entropy from Loop Quantum Gravity

Rovelli, Carlo

doi:10.1103/physrevlett.77.3288

Cited by 559 publications

(670 citation statements)

References 15 publications

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“…Subsequent works in different formalisms for quantum gravity (especially in string theory and loop quantum gravity) have not only provided an explanation to Bekenstein's result [3,4], but also revealed that the linear behavior of the entropy should be modified by a leading order correction that is logarithmic for large areas [5,6]. Similar results have been derived also by considering general properties of black holes [7].…”

Section: Introductionsupporting

confidence: 63%

Entropy and temperature of black holes in a gravity’s rainbow

Galán

Marugán

2006

Phys. Rev. D

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The linear relation between the entropy and area of a black hole can be derived from the Heisenberg principle, the energy-momentum dispersion relation of special relativity, and general considerations about black holes. There exist results in quantum gravity and related contexts suggesting the modification of the usual dispersion relation and uncertainty principle. One of these contexts is the gravity's rainbow formalism. We analyze the consequences of such a modification for black hole thermodynamics from the perspective of two distinct rainbow realizations built from doubly special relativity. One is the proposal of Magueijo and Smolin and the other is based on a canonical implementation of doubly special relativity put forward recently by the authors. In these scenarios, we obtain modified expressions for the entropy and temperature of black holes. We show that, for a family of doubly special relativity theories satisfying certain properties, the temperature can vanish in the limit of zero black hole mass. For the Magueijo and Smolin proposal, this is only possible for some restricted class of models with bounded energy and unbounded momentum. With the proposal of a canonical implementation, on the other hand, the temperature may vanish for more general theories; in particular, the momentum may also be bounded, with bounded or unbounded energy. This opens new possibilities for the outcome of black hole evaporation in the framework of a gravity's rainbow.

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Section: Introductionsupporting

confidence: 63%

Entropy and temperature of black holes in a gravity’s rainbow

Galán

Marugán

2006

Phys. Rev. D

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“…In [19] the entropy is defined as logarithm of the number of microstates for which the sum (6) is between N and N + ∆N, N ≫ ∆N ≫ 1 (here and below the notations of the present article are used). The conclusion made in [19] is that the value of this logarithm is in the interval (0.96 − 1.38)N. However, under the only condition N ≫ 1, without any assumption made about the distribution of the angular momenta j over the edges, how can one arrive at the above numbers (0.96 − 1.38)N? The same question (in fact, objection) refers to the results obtained in [20].…”

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confidence: 99%

Entropy and area of black holes in loop quantum gravity

Khriplovich¹

2002

Physics Letters B

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Simple arguments related to the entropy of black holes strongly constrain the spectrum of the area operator for a Schwarzschild black hole in loop quantum gravity. In particular, this spectrum is fixed completely by the assumption that the black hole entropy is maximum. Within the approach discussed, one arrives in loop quantum gravity at a quantization rule with integer quantum numbers n for the entropy and area of a black hole.1 khriplovich@inp.nsk.su

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“…In this Letter we show how, within the tunneling framework, the presence of a quantum ergosphere can be related to the appearance of a logarithmic correction to the Bekenstein-Hawking entropyarea relation of the type emerging in different quantum gravity scenarios [8,9,10,11,12,13,14,15]. This provides a link between quantum gravity microscopic description of black holes and the origin of the quantum fluctuations responsible for the formation of the quantum ergosphere.…”

Section: Introductionmentioning

confidence: 99%

“…Calculations of the black hole entropy in several quantum gravity scenarios [8,9,10,11,12,13,14,15], besides reproducing the familiar linear relation between area and entropy obtained a leading order "quantum" correction with a logarithmic 3 dependence on the area 4…”

Section: A Tunnel Through the Quantum Horizonmentioning

confidence: 99%

Black hole entropy, log corrections and quantum ergosphere

Arzano

2006

Physics Letters B

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Quantum-gravity corrections to the probability of emission of a particle from a black hole in the Parikh-Wilczek tunneling framework are studied. We consider the effects of zero-point quantum fluctuations of the metric on the emission probability for a tunneling shell. Quantum properties of the geometry are responsible for the formation of a "quantum egosphere" whose effects on the emission probability can be related to the emergence of a logarithmic correction to the Bekenstein-Hawking entropy-area formula.

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Black Hole Entropy from Loop Quantum Gravity

Cited by 559 publications

References 15 publications

Entropy and temperature of black holes in a gravity’s rainbow

Entropy and temperature of black holes in a gravity’s rainbow

Entropy and area of black holes in loop quantum gravity

Black hole entropy, log corrections and quantum ergosphere

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