1997/10/01 by Abhay Ashtekar, A. Ashtekar, John C. Baez +5 · 25 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Black hole thermodynamics #Classical mechanics #Cosmology and Gravitation Theories #Entropy (arrow of time) #Extremal black hole #Immirzi parameter #Loop quantum gravity #Mathematical physics #Noncommutative and Quantum Gravity Theories #Physics #Quantum #Quantum gravity #Quantum mechanics #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevlett.80.904
published as Phys.Rev.Lett. 80 (1998) 904-907 · Revtex, 8 pages, 1 figure
arxiv created 1997/10/01 · openalex publication_date 1998/02/02 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
A ``black hole sector'' of nonperturbative canonical quantum gravity is introduced. The quantum black hole degrees of freedom are shown to be described by a Chern-Simons field theory on the horizon. It is shown that the entropy of a large nonrotating black hole is proportional to its horizon area. The constant of proportionality depends upon the Immirzi parameter, which fixes the spectrum of the area operator in loop quantum gravity; an appropriate choice of this parameter gives the Bekenstein-Hawking formula S\phantom\rule0ex0ex=\phantom\rule0ex0exA/4\ensuremathℓP2. With the same choice of the Immirzi parameter, this result also holds for black holes carrying electric or dilatonic charge, which are not necessarily near extremal.