Mass and charge fluctuations and black hole entropy

Chatterjee, Ashok; Majumdar, Parthasarathi

doi:10.1103/physrevd.71.024003

Cited by 65 publications

(64 citation statements)

References 21 publications

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“…The correction to B-H entropy of black hole attracts researcher's attention. Various method has been used to discuss the correction value to black hole B-H entropy [32][33][34][35][36][37][38][39][40][41][42][43][44][45]. Many researchers think that the expression of the correction to B-H entropy of the black hole is…”

Section: Introductionmentioning

confidence: 99%

Generalized Uncertainty Relation and Hawking Radiation of the Black Hole

et al. 2009

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Recently, there has been much attention devoted to the correction to the black hole radiation spectrum and the quantum corrections to Bekenstein-Hawking entropy. In particular, many researchers have expressed a vested interest in the coefficient of the logarithmic term of the black hole entropy correction term. In this paper, we calculate the radiation spectrum of arbitrary dimension Schwarzschild black hole after considering the generalized uncertainty principle. The correction value of Bekenstein-Hawking entropy is derived.

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Section: Introductionmentioning

confidence: 99%

Generalized Uncertainty Relation and Hawking Radiation of the Black Hole

et al. 2009

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“…These corrections can appear in the black hole entropy in loop quantum gravity (LQG) [12,13,14,15,16,17,18,19,20,21,22]; they can also be due to thermal equilibrium fluctuation, quantum fluctuation, or mass and charge fluctuations [20,23,24,25,26,27,28,71,72]. We refer to e.g.…”

Section: Introductionmentioning

confidence: 99%

Entropy-Corrected Holographic Dark Energy

Hao

2009

Commun. Theor. Phys.

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The holographic dark energy (HDE) is now an interesting candidate of dark energy, which has been studied extensively in the literature. In the derivation of HDE, the black hole entropy plays an important role. In fact, the entropy-area relation can be modified due to loop quantum gravity or other reasons. With the modified entropy-area relation, we propose the so-called "entropy-corrected holographic dark energy" (ECHDE) in the present work. We consider many aspects of ECHDE and find some interesting results. In addition, we briefly consider the so-called "entropy-corrected agegraphic dark energy" (ECADE).

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“…Also since the original version of this manuscript, it has been suggested [51] that the grand-canonical analysis of [26] may be invalidated as follows: For a classically neutral or almost neutral black hole (our regime of interest), the relative charge fluctuation "blows up" since ∆Q/Q → ∞ as Q → 0. [Actually, the problem occurs because < m >→ 0, since our partition function (7) is directly expressed in terms of the quantum numbers n and m.] It is then argued that this divergence would invalidate the small fluctuation (Gaussian) approximation, which was used to evaluate the partition function.…”

Section: Addendummentioning

confidence: 99%

A comment on black hole entropy or does nature abhor a logarithm?

Medved

2004

Class. Quantum Grav.

105

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There has been substantial interest, as of late, in the quantum-corrected form of the Bekenstein-Hawking black hole entropy. The consensus viewpoint is that the leading-order correction should be a logarithm of the horizon area; however, the value of the logarithmic prefactor remains a point of notable controversy. Very recently, Hod has employed statistical arguments that constrain this prefactor to be a non-negative integer. In the current paper, we invoke some independent considerations to argue that the "best guess" for the prefactor might simply be zero. Significantly, this value complies with the prior prediction and, moreover, seems suggestive of some fundamental symmetry. I. MOTIVATIONIt has long been accepted that black holes possess an intrinsic entropy which (for at least a wide class of models) can be determined by way of the famous Bekenstein-Hawking area law [1,2]; that is,where S BH is the entropy in question and A is the cross-sectional area (in Planck units) of the black hole horizon. Here and throughout, all fundamental constants are set equal to unity. Moreover, we will focus on the physically realistic case of only four uncompactified spacetime dimensions, as well as the case of a black hole that is neutral and static modulo quantum fluctuations (although many of our statements have more general applicability). Also, we will always assume the semi-classical regime of a macroscopically large black hole or A >> 1. Further note that the above relation is, in spite of the implied presence ofh (in the denominator), strictly a classical one. Although the black hole area law initially followed from thermodynamic considerations (e.g., protecting the second law of thermodynamics in the presence of a black hole [1]), it is 1

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Mass and charge fluctuations and black hole entropy

Cited by 65 publications

References 21 publications

Generalized Uncertainty Relation and Hawking Radiation of the Black Hole

Generalized Uncertainty Relation and Hawking Radiation of the Black Hole

Entropy-Corrected Holographic Dark Energy

A comment on black hole entropy or does nature abhor a logarithm?

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