Semiclassical quantisation of space-times with apparent horizons

Abstract

Coherent or semiclassical states in canonical quantum gravity describe the classical Schwarzschild space-time. By tracing over the coherent state wavefunction inside the horizon, a density matrix is derived. Bekenstein-Hawking entropy is obtained from the density matrix, modulo the Immirzi parameter. The expectation value of the area and curvature operator is evaluated in these states. The behaviour near the singularity of the curvature operator shows that the singularity is resolved. We then generalise the results to space-times with spherically symmetric apparent horizons.

52 pages, 4 figures

References in corpus (2)

• Black hole entropy in Loop Quantum Gravity
• Counting a black hole in Lorentzian product triangulations

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