2010/03/31 by Leo Rodriguez, Tuna Yildirim · 4 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #hep-th
paper · pdf · doi:10.1088/0264-9381/27/15/155003
published as 2010 Class. Quantum Grav. 27 155003 · 18 pages, references added, accepted in IOP's Classical and Quantum Gravity.
arxiv created 2010/05/10 · openalex publication_date 2010/06/11 · arxiv updated 2010/06/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/30
We construct a two-dimensional CFT, in the form of a Liouville theory, in the near-horizon limit of four- and three-dimensional black holes. The near-horizon CFT assumes two-dimensional black hole solutions first introduced by Christensen and Fulling (1977 Phys. Rev. D 15 2088–104) and expanded to a greater class of black holes via Robinson and Wilczek (2005 Phys. Rev. Lett. 95 011303). The two-dimensional black holes admit a Diff( S 1 ) subalgebra, which upon quantization in the horizon limit becomes Virasoro with calculable central charge. This charge and the lowest Virasoro eigen-mode reproduce the correct Bekenstein–Hawking entropy of the four- and three-dimensional black holes via the known Cardy formula (Blöte et al 1986 Phys. Rev. Lett. 56 742; Cardy 1986 Nucl. Phys. B 270 186). Furthermore, the two-dimensional CFT's energy–momentum tensor is anomalous. However, in the horizon limit the energy–momentum tensor becomes holomorphic equaling the Hawking flux of the four- and three-dimensional black holes. This encoding of both entropy and temperature provides a uniformity in the calculation of black hole thermodynamic and statistical quantities for the non-local effective action approach.