Black Hole Entropy: Certain Quantum Features

Majumdar, Parthasarathi

doi:10.1142/9789812777386_0298

Cited by 1 publication

(1 citation statement)

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“…Our outcome of b = 0, although somewhat conjectural, does immediately satisfy a non-trivial consistency check; namely, it complies with Hod's statistical constraint that the prefactor be a non-negative integer [13]. Moreover, if one interprets the well-known holographic principle [42] in its most literal form (so that A/4 is a strict upper bound on the black hole entropy), then a non-positive value of b would necessarily be favoured [43]. This realization suggests that zero is, in fact, the unique choice of prefactor that is consistent with both the holographic principle and statistical mechanics.…”

Section: Discussionmentioning

confidence: 60%

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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Section: Discussionmentioning

confidence: 60%