2016/02/01 by Andrea Addazi, Salvatore Capozziello · 2 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Black hole (networking) #Black hole thermodynamics #Degenerate energy levels #Event horizon #Extremal black hole #Hawking radiation #Horizon #Quantum Electrodynamics and Casimir Effect #Semiclassical physics #White hole #astro-ph.HE #de Sitter–Schwarzschild metric #gr-qc #hep-th
paper · pdf · doi:10.1142/s0217732316500541
9 pages, to appear in Mod. Phys. Lett. A
arxiv created 2016/02/01 · openalex publication_date 2016/03/11 · arxiv updated 2016/04/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The semiclassical effects of anti-evaporating black holes can be discussed in the framework of f(R) gravity. In particular, the Bousso–Hawking–Nojiri–Odinstov anti-evaporation instability of degenerate Schwarzschild–de Sitter black holes (the so-called Nariai spacetime) leads to a dynamical increasing of black hole horizon in f(R) gravity. This phenomenon causes the following transition: emitting marginally trapped surfaces (TS) become space-like surfaces before the effective Bekenstein–Hawking emission time. As a consequence, Bousso–Hawking thermal radiation cannot be emitted in an anti-evaporating Nariai black hole. Possible implications in cosmology and black hole physics are also discussed.