2003/02/28 by Andrés Gomberoff, Andres Gomberoff, Claudio Teitelboim · 2 citations
Mathematics · Physics and Astronomy · #Angular momentum #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Black hole (networking) #Boundary (topology) #Boundary value problem #Classical mechanics #Cosmological constant #Cosmology and Gravitation Theories #De Sitter universe #Hamiltonian (control theory) #Horizon #Mathematical analysis #Mathematical physics #Mathematics #Physics #Quantum mechanics #Rotating black hole #Universe #de Sitter–Schwarzschild metric #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.67.104024
published as Phys.Rev. D67 (2003) 104024 · 9 pages. References added
arxiv created 2003/04/02 · openalex publication_date 2003/05/29 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The action and the thermodynamics of a rotating black hole in the presence of a positive cosmological constant are analyzed. Since there is no spatial infinity, one must bring in, instead, a platform where the parameters characterizing the thermodynamic ensemble are specified. In the present treatment the platform in question is taken to be one of the two horizons, which is considered as a boundary. If the boundary is taken to be the cosmological horizon one deals with the action and thermodynamics of the black hole horizon. Conversely, if one takes the black hole horizon as the boundary, one deals with the action and thermodynamics of the cosmological horizon. The two systems are different. Their energy and angular momenta are equal in magnitude but have opposite sign. In either case, the energy and the angular momentum are obtained as surface terms on the boundary, according to the standard Hamiltonian procedure. The temperature and the rotational chemical potential are also expressed in terms of magnitudes on the boundary. If, in the resulting expressions, one continues the cosmological constant to negative values, the black hole thermodynamic parameters defined on the cosmological horizon coincide with those calculated at spatial infinity in the asymptotically anti--de Sitter case.