Modelling the Evaporation of Non-singular Black Holes

Abstract

We present a model for studying the formation and evaporation of non-singular (quantum corrected) black holes. The model is based on a generalized form of the dimensionally reduced, spherically symmetric Einstein--Hilbert action and includes a suitably generalized Polyakov action to provide a mechanism for radiation back-reaction. The equations of motion describing self-gravitating scalar field collapse are derived in local form both in null co--ordinates and in Painleve--Gullstrand (flat slice) co--ordinates. They provide the starting point for numerical studies of complete spacetimes containing dynamical horizons that bound a compact trapped region. Such spacetimes have been proposed in the past as solutions to the information loss problem because they possess neither an event horizon nor a singularity. Since the equations of motion in our model are derived from a diffeomorphism invariant action they preserve the constraint algebra and the resulting energy momentum tensor is manifestly conserved.

14 pages, 0 figures, references and acknowledgements added, final version to appear in PRD

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Cited by in corpus (6)

• Notes on non-singular models of black holes
• Towards a Non-singular Paradigm of Black Hole Physics
• Quantum radiation from a sandwich black hole
• Hawking-like radiation and the density matrix for an infalling observer during gravitational collapse
• Regular black holes from pure gravity in four dimensions
• Anomaly induced quantum correction to charged black holes; geometry and thermodynamics