Black hole evaporation: a paradigm

By Abhay Ashtekar, M. Bojowald. 2005

285 citations recorded by the source corpus.

A paradigm describing black hole evaporation in non-perturbative quantum gravity is developed by combining two sets of detailed results: (i) resolution of the Schwarzschild singularity using quantum geometry methods and (ii) time evolution of black holes in the trapping and dynamical horizon frameworks. Quantum geometry effects introduce a major modification in the traditional spacetime diagram of black hole evaporation, providing a possible mechanism for recovery of information that is classically lost in the process of black hole formation. The paradigm is developed directly in the Lorentzian regime and necessary conditions for its viability are discussed. If these conditions are met, much of the tension between expectations based on spacetime geometry and structure of quantum theory would be resolved.

Subfields: Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/cc03487a382f4bb66257abde59cfca9208615229

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In Atomic and Molecular Physics, and Optics

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In Statistical and Nonlinear Physics

Citations in the corpus

Quantum extension of the Kruskal spacetime (2018, unknown): “[47]).”
Loop Quantum Cosmology (2005, background): “This allows one to see if the different ingredients and effects of a loop quantization fit together in a complete picture, which so far seems to be the case [14, 159, 13, 76, 57].”
Some uniqueness results for dynamical horizons (2005, methodology): “Since their area is known [9, 10, 25, 26] to grow during collapse and decrease because of Hawking radiation, one could use the MTTs to analyze the formation and evaporation of black holes [5].”
Loop quantization of the Schwarzschild interior revisited (2015, background): “It is only with that more complete description that one might hope to give meaning to the ‘effective spacetime’ that arises from the solution to our effective equations, in terms of the Ashtekar-Bojowald paradigm [24].”
Black holes in general relativity (2009, methodology): “At a technical level the main difference is that Hayward prefers to work with trapping horizons [20], while Ashtekar and Bojowald prefer to work with dynamical horizo s [19].”
Gravity and the quantum (2004, background): “loss [ 51 ]. Furthermore, the semi-classical considerations are not simply dismissed; they turn out to be valid in certain space-time regions and under certain approximations.”
Quantum-gravity effects outside the horizon spark black to white hole tunneling (2014, background): “The possibility of such a Planck star phenomenology has been considered by numerous authors [3–13].”
An apologia for firewalls (2013, background): “[75] for a recent discussion) and other ideas such as [76] that lead to information being recovered only long after the Page time are similarly incompatible with AdS/CFT; these would otherwise be an alternative to the firewall.”
FUNDAMENTAL STRUCTURE OF LOOP QUANTUM GRAVITY (2005, background): “One may further study the ”end state” of the gravitational colla pse of matter fields inside a black hole [54][103] and black hole evaporation [9].”
White holes as remnants: a surprising scenario for the end of a black hole (2018, background): “But the scenario presented here turns out to be consistent with general expectations that are both in the AdS/CFT community (see for instance [51, 52]) and in the quantum gravity community (see for instance the ‘paradigm’ [14]).”