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Horizon spectroscopy in and beyond general relativity
General Relativity and Quantum Cosmology · Submitted 18 Nov 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In particular, the three approaches show that the Bekenstein-like spectra for the horizon entropy is a robust result.
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The abstract, sentence by sentence
In this work we generalize the results for the entropy spectra typically derived for black holes in general relativity to a generic horizon within the spherically symmetric (asymptotically flat and non-flat) space-times of more general theories of gravity. We use all the standard --- Bekenstein's universal lower bound on the entropy transition, the highly damped quasi-normal modes and reduced phase-space quantization --- approaches to derive the spectra. In particular, the three approaches show that the Bekenstein-like spectra for the horizon entropy is a robust result. Our results confirm the suggestion made relatively recently by an independent fourth argument by Kothawala et al [1].
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In this work we generalize the results for the entropy spectra typically derived for black holes in general relativity to a generic horizon within the spherically symmetric (asymptotically flat and non-flat) space-times of more general theories of gravity. | contribution 1.00 | 0.90 | 0.14 | asserted 0.95 |
| s1 | We use all the standard --- Bekenstein's universal lower bound on the entropy transition, the highly damped quasi-normal modes and reduced phase-space quantization --- approaches to derive the spectra. | method 0.99 | 0.89 | 0.05 | asserted 0.99 |
| s2 | In particular, the three approaches show that the Bekenstein-like spectra for the horizon entropy is a robust result. | result 0.70 | 0.86 | 0.67 | asserted 1.00 |
| s3 | Our results confirm the suggestion made relatively recently by an independent fourth argument by Kothawala et al [1]. | interpretation 0.54 | 0.53 | 0.19 | asserted 0.98 |
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The paper
Original abstract
In this work we generalize the results for the entropy spectra typically derived for black holes in general relativity to a generic horizon within the spherically symmetric (asymptotically flat and non-flat) space-times of more general theories of gravity. We use all the standard --- Bekenstein's universal lower bound on the entropy transition, the highly damped quasi-normal modes and reduced phase-space quantization --- approaches to derive the spectra. In particular, the three approaches show that the Bekenstein-like spectra for the horizon entropy is a robust result. Our results confirm the suggestion made relatively recently by an independent fourth argument by Kothawala et al [1].
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How the literature uses it
1 arXiv paper cite this in 1 sentence
Papers citing it
Cites it as support 1 paper
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This indeed has provided the correct black-hole entropy spectrum like other more rigorous semiclassical quantization approaches [ref] .
An approach to the quantization of black-hole quasi-normal modes · Introduction · 0.97
What it cites · 54 sentences without a confident label
Builds on 5 papers
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Therefore, as mentioned before, (since cosmological constant is included) we can apply the quantization from [ref] to quantize entropy of the deSitter cosmological horizon, or even (considering the interior region inside the Cauchy horizon), to the inner Cauchy horizon of the R-N black hole.
Spectrum of Charged Black Holes - The Big Fix Mechanism Revisited · Discussion of the results · 0.89
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Therefore, as mentioned before, (since cosmological constant is included) we can apply the quantization from [ref] to quantize entropy of the deSitter cosmological horizon, or even (considering the interior region inside the Cauchy horizon), to the inner Cauchy horizon of the R-N black hole.
Quantum Mechanics of Charged Black Holes · Discussion of the results · 0.89
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Therefore, as mentioned before, (since cosmological constant is included) we can apply the quantization from [ref] to quantize entropy of the deSitter cosmological horizon, or even (considering the interior region inside the Cauchy horizon), to the inner Cauchy horizon of the R-N black hole.
Discrete Spectra of Charged Black Holes · Discussion of the results · 0.89
Uses the method or tool of 7 papers
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Imposing the periodicity condition on the action [ref] one can provide a transformation of variables: [equation] and [equation] For this transformation to be canonical, as shown in [ref] , direct calculation implies that the following must hold: [equation] Now consider theory in which $M$ corresponds to some reasonably defined mass, then [ref] means $E$ is from the definition related to the entropy of a horizon and some theory of gravity, in particular [equation] Then one can easily observe: [equation] with the spectrum of the harmonic oscillator: [equation] This spectrum describes deviation of entropy from entropy of an extremal state.
Quantum Mechanics of Charged Black Holes · Quantization in the Euclidean sector · 0.84
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Imposing the periodicity condition on the action [ref] one can provide a transformation of variables: [equation] and [equation] For this transformation to be canonical, as shown in [ref] , direct calculation implies that the following must hold: [equation] Now consider theory in which $M$ corresponds to some reasonably defined mass, then [ref] means $E$ is from the definition related to the entropy of a horizon and some theory of gravity, in particular [equation] Then one can easily observe: [equation] with the spectrum of the harmonic oscillator: [equation] This spectrum describes deviation of entropy from entropy of an extremal state.
Spectrum of Charged Black Holes - The Big Fix Mechanism Revisited · Quantization in the Euclidean sector · 0.84
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Imposing the periodicity condition on the action [ref] one can provide a transformation of variables: [equation] and [equation] For this transformation to be canonical, as shown in [ref] , direct calculation implies that the following must hold: [equation] Now consider theory in which $M$ corresponds to some reasonably defined mass, then [ref] means $E$ is from the definition related to the entropy of a horizon and some theory of gravity, in particular [equation] Then one can easily observe: [equation] with the spectrum of the harmonic oscillator: [equation] This spectrum describes deviation of entropy from entropy of an extremal state.
Discrete Spectra of Charged Black Holes · Quantization in the Euclidean sector · 0.84
Cites as support 3 papers
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Therefore we claim that the results of [ref] , when pushed to their consequences, support the basic conclusion of this paper.
Spectrum of Charged Black Holes - The Big Fix Mechanism Revisited · Discussion of the results · 0.96
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Therefore we claim that the results of [ref] , when pushed to their consequences, support the basic conclusion of this paper.
Quantum Mechanics of Charged Black Holes · Discussion of the results · 0.96
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Therefore we claim that the results of [ref] , when pushed to their consequences, support the basic conclusion of this paper.
Discrete Spectra of Charged Black Holes · Discussion of the results · 0.96
Cites as background 16 papers
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* Bekenstein's original argument about the universality (independence on BH parameters) of the lower bound on the BH entropy/area transition [ref] . * Argument via asymptotically highly damped BH quasi-normal modes [ref] . * Direct quantization techniques typically applied to a reduced phase space of the black hole parameters [ref] .
Black Holes: Classical Properties, Thermodynamics and Heuristic Quantization · Introduction · 0.85
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* Bekenstein's original argument about the universality (independence on BH parameters) of the lower bound on the BH entropy/area transition [ref] . * Argument via asymptotically highly damped BH quasi-normal modes [ref] . * Direct quantization techniques typically applied to a reduced phase space of the black hole parameters [ref] .
Bohr's Correspondence Principle and The Area Spectrum of Quantum Black Holes · Introduction · 0.85
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* Bekenstein's original argument about the universality (independence on BH parameters) of the lower bound on the BH entropy/area transition [ref] . * Argument via asymptotically highly damped BH quasi-normal modes [ref] . * Direct quantization techniques typically applied to a reduced phase space of the black hole parameters [ref] .
Quantum Mechanics of Charged Black Holes · Introduction · 0.85
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