2017/03/31 by S. Sadeghian, M. H. Vahidinia
Physics and Astronomy · #Black Holes and Theoretical Physics #Computer science #Cosmology and Gravitation Theories #Quantum Chromodynamics and Particle Interactions #hep-th
paper · pdf · doi:10.1103/physrevd.96.044004
published as Phys. Rev. D 96, 044004 (2017) · 27 pages, 2 figures
openalex publication_date 2017/08/04 · arxiv created 2017/08/06 · arxiv updated 2017/08/09 · openalex created_date 2017/08/17 · openalex updated_date 2026/08/05
We consider two solutions of Einstein-\mathrm\ensuremathΛ theory which admit the extremal vanishing horizon (EVH) limit, odd-dimensional multispinning Kerr black hole (in the presence of cosmological constant) and cosmological soliton. We show that the near horizon EVH geometry of Kerr has a three-dimensional maximally symmetric subspace whose curvature depends on rotational parameters and the cosmological constant. In the Kerr-dS case, this subspace interpolates between AdS3, three-dimensional flat and dS3 by varying rotational parameters, while the near horizon of the EVH cosmological soliton always has a dS3. The feature of the EVH cosmological soliton is that it is regular everywhere on the horizon. In the near EVH case, these three-dimensional parts turn into the corresponding locally maximally symmetric spacetimes with a horizon: Kerr-dS3, flat space cosmology or BTZ black hole. We show that their thermodynamics match with the thermodynamics of the original near EVH black holes. We also briefly discuss the holographic two-dimensional CFT dual to the near horizon of EVH solutions.