Abstract
We model the gravitational collapse of heavy massive shells including its main quantum corrections. Among these corrections, quantum improvements coming from Quantum Einstein Gravity are taken into account, which provides us with an effective quantum spacetime. Likewise, we consider dynamical Hawking radiation by modeling its back-reaction once the horizons have been generated. Our results point towards a picture of gravitational collapse in which the collapsing shell reaches a minimum non-zero radius (whose value depends on the shell initial conditions) with its mass only slightly reduced. Then, there is always a rebound after which most (or all) of the mass evaporates in the form of Hawking radiation. Since the mass never concentrates in a single point, no singularity appears.
Highlights
It is expected that a large enough object would collapse classically until a horizon forms
We assume that the spacetime is split in two different regions M = M+ ∪ M− with a common spherically symmetric timelike boundary Σ = ∂M+ ∩ ∂M− corresponding to the thin shell
We consider Hawking radiation coming out from an improved black hole satisfying M > Mcr thanks to the tunneling process occurring both in the outer and in the inner horizons
Summary
It is expected that a large enough object would collapse classically until a horizon forms. We assume that the spacetime is split in two different regions M = M+ ∪ M− with a common spherically symmetric timelike boundary Σ = ∂M+ ∩ ∂M− corresponding to the thin shell We choose for the exterior region an effective improved solution coming from Quantum Einstein Gravity that incorporates quantum corrections to the classical solution It does so by taking into account the effect of virtual gravitons. This will provide us with the shell evolution equation which will allow us to analyze its different attractive and repulsive contributions.
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