Classical Signature Change in the Black Hole Topology

Details Classical Signature Change in the Black Hole Topology Classical Signature Change in the Black Hole Topology

1999-07-09

arxiv.org/abs/gr-qc/9907042v2

Int.J.Mod.Phys. D6 (1997) 211-238

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

LaTeX, 19 pages, 11 Figures. Replacement - only change is following comment: For a pdf version with the figures embedded, see

Scientific paper

Investigations of classical signature change have generally envisaged applications to cosmological models, usually a Friedmann-Lemaitre-Robertson-Walker model. The purpose has been to avoid the inevitable singularity of models with purely Lorentzian signature, replacing the neighbourhood of the big bang with an initial, singularity free region of Euclidean signture, and a signature change. We here show that signature change can also avoid the singularity of gravitational collapse. We investigate the process of re-birth of Schwarzschild type black holes, modelling it as a double signature change, joining two universes of Lorentzian signature through a Euclidean region which provides a `bounce'. We show that this process is viable both with and without matter present, but realistic models -- which have the signature change surfaces hidden inside the horizons -- require non-zero density. In fact the most realistic models are those that start as a finite cloud of collapsing matter, surrounded by vacuum. We consider how geodesics may be matched across a signature change surface, and conclude that the particle `masses' must jump in value. This scenario may be relevant to Smolin's recent proposal that a form of natural selection operates on the level of universes, which favours the type of universe we live in.

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