A Quantum Model of Schwarzschild Black Hole Evaporation

Abstract

We construct a one-loop effective metric describing the evaporation phase of a Schwarzschild black hole in a spherically symmetric null-dust model. This is achieved by quantising the Vaidya solution and by chosing a time dependent quantum state. This state describes a black hole which is initially in thermal equilibrium and then the equilibrium is switched off, so that the black hole starts to evaporate, shrinking to a zero radius in a finite proper time. The naked singularity appears, and the Hawking flux diverges at the end-point. However, a static metric can be imposed in the future of the end-point. Although this end-state metric cannot be determined within our construction, we show that it cannot be a flat metric.

arXiv comment14 pages, Latex, 2 figures

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Cited by in corpus (5)

• Metric Fluctuation Corrections to Hawking Radiation
• One-Loop Effective Action for Spherical Scalar Field Collapse
• One-loop corrections for Schwarzschild black hole via 2D dilaton gravity
• General Solution for Self-Gravitating Spherical Null Dust
• One-loop Effective Action for a Generic 2D Dilaton Gravity Theory