Black-hole entropy in loop quantum gravity

By K. Meissner. 2004

830 citations recorded by the source corpus.

We calculate the black-hole entropy in loop quantum gravity as a function of the horizon area and provide the exact formula for the leading and sub-leading terms. By comparison with the Bekenstein–Hawking formula, we uniquely fix the value of the ‘quantum of area’ in the theory.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/9564b1becac99a9362b77856e0f5f07661ea7c67

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Citations in the corpus

On the classification of asymptotic quasinormal frequencies for $d$-dimensional black holes and quantum gravity (2004, background): “Yet another problem has recently emerged directly within loop quantum gravity [86, 87].”
Black hole entropy from the SU(2)-invariant formulation of type I isolated horizons (2010, background): “In loop quantum gravity the first computations (valid for physical black holes) were based on general considerations and the fact that the area spectrum in the theory is discrete [9].”
Introduction to loop quantum gravity and spin foams (2004, background): “[A])] is a gauge invariant cylindrical function. Unitary irreducible representation matrices of spin j will be denoted by j Πmm′ for −j≤ m,m′ ≤ j. The cylindrical function Wj γ[A] := Tr[ j Π (he[A])] (76) is the simplest example of spin network function41,42,43,44. This function is represented as on”
Gravity and the Thermodynamics of Horizons (2003, background): “One gets the correct numerical factor (only) if γ = ln N/2π √ 2 where N = 2 or N = 3 depending on whether the gauge group SU(2) or SO(3) is used in the theory (Ashtekar et al., 1998, 2000; Krasnov, 1998; Rovelli, 1996).”
Introduction to Loop Quantum Cosmology (2011, background): “238 [148] from the computation of the entropy of non-rotating black-hole isolated horizons [7, 8, 148].”
Logarithmic corrections to Schwarzschild and other non-extremal black hole entropy in different dimensions (2012, methodology): “This gives An alternative computation of the corrections to the Schwarzschild black hole entropy in loop quantum gravity, based on the U(1) Chern-Simons theory, has been given in [31, 34–36].”
Black-hole entropy from quantum geometry (2004, background): “The issue was raised in works by Krasnov [4] and Rovelli [ 5 ].”
Isolated and Dynamical Horizons and Their Applications (2004, background): “For example if, as in the early treatments [145, 33, 138, 139, 113, 114] one ignores the horizon boundary conditions and the resulting Chern-Simons term in the symplectic structure, one would find that S∆ is proportional to √ ao.”
Loop Quantum Gravity (2003, neutral): “[140] K.”
Gravity and the quantum (2004, background): “entropy. This discussion is based on work of Ashtekar, Baez, Bojowald, Corichi, Domagala, Krasnov, Lewandowski and Meissner, much of which was motivated by earlier work of Krasnov, Rovelli and others [38,46,47]. As explained in the Introduction, since mid-seventies, a key question in the subject has”
Loop quantum gravity: an outside view (2005, background): “the horizon would imply a prediction for the value of the parameter γ. Unfortunately, the results obtained so far disagree; for instance, [36] obtains γ= ln2 π √ 3 , whereas a more recent calculation [83, 84] gives γ= 0.23753295.... We suspect that the ﬁnal word has not yet been spoken on this subje”
Hawking radiation as tunneling through the quantum horizon (2005, background): “) Hence, the canonical correction is more than sufficient to compensate for the Loop Quantum Gravity prediction of α = −1/2 [27].”