2014/04/30 by Yiyang Zhang, Yiwei Zhu, Leonardo Modesto +1 · 1 citation
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #General relativity #Gravitational collapse #Noncommutative and Quantum Gravity Theories #Numerical relativity #Primordial black hole #Quantum Electrodynamics and Casimir Effect #Ring singularity #Singularity #Spacetime #White hole #astro-ph.HE #gr-qc
paper · pdf · doi:10.1140/epjc/s10052-015-3311-2
published as Eur.Phys.J.C75:96,2015 · 14 pages, 9 figures. v2: refereed version
openalex publication_date 2015/02/01 · arxiv created 2015/02/12 · arxiv updated 2015/02/27 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Starting from the Oppenheimer–Snyder model, we know how in classical general relativity the gravitational collapse of matter forms a black hole with a central spacetime singularity. It is widely believed that the singularity must be removed by quantum-gravity effects. Some static quantum-inspired singularity-free black hole solutions have been proposed in the literature, but when one considers simple examples of gravitational collapse the classical singularity is replaced by a bounce, after which the collapsing matter expands for ever. We may expect three possible explanations: (i) the static regular black hole solutions are not physical, in the sense that they cannot be realized in Nature, (ii) the final product of the collapse is not unique, but it depends on the initial conditions, or (iii) boundary effects play an important role and our simple models miss important physics. In the latter case, after proper adjustment, the bouncing solution would approach the static one. We argue that the “correct answer” may be related to the appearance of a ghost state in de Sitter spacetimes with super Planckian mass. Our black holes have indeed a de Sitter core and the ghost would make these configurations unstable. Therefore we believe that these black hole static solutions represent the transient phase of a gravitational collapse but never survive as asymptotic states.