1998/12/31 by O. B. Zaslavskii, O B Zaslavskii
Physics and Astronomy · #Black Holes and Theoretical Physics #Noncommutative and Quantum Gravity Theories #Quantum Electrodynamics and Casimir Effect #gr-qc #hep-th
paper · pdf · doi:10.1088/0264-9381/17/2/315
published as Class.Quant.Grav. 17 (2000) 497-512 · 27 pages, REVTeX 3.0. Expanded from previous version. Title somewhat changed. Qualitative explanation of effects of strong quantum backreaction on geometry suggested in terms of induced cosmological constant. Stressed that if this constant is positive, solutions found can be considered as quantum versions of charged Nariai one. Accepted for publication in Class. Quant. Grav
arxiv created 1999/11/24 · openalex publication_date 2000/01/07 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
We consider the class of metrics that can be obtained from those of non-extreme black holes by limiting transitions to the extreme state such that the near-horizon geometry expands into a whole manifold. These metrics include, in particular, the Rindler and Bertotti-Robinson spacetimes. The general formula for the entropy of massless radiation valid either for black hole or for acceleration horizons is derived. It is argued that, as a black hole horizon in the limit under consideration turns into an acceleration one, the thermodynamic entropy S q of quantum radiation is due to the Unruh effect entirely and S q = 0 exactly. The contribution to the quasilocal energy from a given curved spacetime is equal to zero and the only non-vanishing term stems from a reference metric. In the variation procedure necessary for the derivation of the general first law, the metric on a horizon surface changes along with the boundary one, and the account for gravitational and matter stresses is an essential ingredient of the first law. This law confirms the property S q = 0. The quantum-corrected geometry of the Bertotti-Robinson spacetime is found and it is argued that backreaction of quantum fields mimics the effect of the cosmological constant eff and can drastically change the character of spacetime depending on the sign of eff - for instance, turn AdS 2 × S 2 into dS 2 × S 2 or Rindler 2 × S 2 . The latter two solutions can be thought of as the quantum versions of the cold and ultracold limits of the Reissner-Nordstrom-de Sitter metric.