Abstract
Quantum resolutions of the space-time singularity at the end of gravitational collapse may provide hints towards the properties of a final theory of Quantum-Gravity. The mechanism by which the singularity is avoided and replaced by a bounce depends on the specific behaviour of gravity in the strong field and may have implications for the geometry of the space-time also in the weak field. In the last few decades, several scenarios for black hole bounces have been proposed and I shall argue that the times are now mature to ask the question of whether such bounces can be observed in astrophysical phenomena.
Highlights
IntroductionThe search for a viable theory of Quantum-Gravity (QG) has been ongoing for several decades [1]
The search for a viable theory of Quantum-Gravity (QG) has been ongoing for several decades [1].It is widely accepted that General Relativity (GR) is not a complete theory and that it needs modifications in the high energy regime [2]
QG modifications to the geometrical side of Einstein’s equations are treated as an effective energy-momentum tensor [13]. This allows to solve the usual set of field equations of GR for an effective matter source that takes into account QG effects
Summary
The search for a viable theory of Quantum-Gravity (QG) has been ongoing for several decades [1]. The energy scales at which QG becomes relevant are well beyond what is presently achievable in particle accelerators [4], there exist other proposed experiments that do not require high energy particle physics that may provide results in the future (see, for example, [5]) These may run into difficulties due to the weakness of the gravitational field at low energy regimes. In the bouncing scenarios, the removal of the singularity implies that there is not a time after which the geometry can be described by a black hole solution This affects the nature of the horizon, which can not be the usual event horizon, and may have implications for the weak field regions of the space-time.
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