2003/03/31 by T. Hirayama, Takayuki Hirayama, Bob Holdom +1 · 9 citations
Mathematics · Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Black hole (networking) #Boundary (topology) #Charged black hole #Classical mechanics #Computer science #Cosmology and Gravitation Theories #Euclidean distance matrix #Euclidean domain #Euclidean geometry #Euclidean space #Extremal black hole #General relativity #Geometry #Horizon #Mathematical analysis #Mathematics #Nonsingular black hole models #Physics #Theoretical physics #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.68.044003
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 68(4) (American Physical Society) · 14 pages with figures, version to appear in PRD
arxiv created 2003/07/22 · openalex publication_date 2003/08/05 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The search for regular black hole solutions in classical gravity leads us to consider a core of Euclidean signature in the interior of a black hole. Solutions of Lorentzian and Euclidean general relativity match in such a way that energy densities and pressures of an isotropic perfect fluid form are everywhere finite and continuous. Although the weak energy condition cannot be satisfied for these solutions in general relativity, it can be when higher derivative terms are added. A numerical study shows how the transition becomes smoother in theories with more derivatives. As an alternative to the Euclidean core, we also discuss a closely related time dependent orbifold construction with a smooth space-like boundary inside the horizon.