Abstract
Gravitational backgrounds, such as black holes, AdS, de Sitter and inflationary universes, should be viewed ascomposite of Nsoft constituent gravitons. It then follows that such systems are close to quantum criticality of graviton Bose-gas to Bose-liquidtransition.Generic properties of the ordinary metric description, including geodesic motion orparticle-creation in the background metric, emerge as the large-N limit of quantum scattering of constituent longitudinal gravitons.We show that this picture correctly accountsfor physics of large and small black holes in AdS, as well as reproduces well-known inflationarypredictions for cosmological parameters. However, it anticipates new effects not captured by the standard semi-classical treatment. In particular, we predict observable corrections thatare sensitive to the inflationary history way beyond last 60 e-foldings. We derive an absolute upper bound on the number of e-foldings, beyond which neither de Sitter nor inflationary Universe can be approximated by a semi-classical metric. However, they could in principle persist in a new type of quantum eternity state. We discuss implications of this phenomenon for the cosmological constant problem.
Highlights
Generic properties of the ordinary metric description, including geodesic motion or particlecreation in the background metric, emerge as the large-N limit of quantum scattering of constituent longitudinal gravitons. We show that this picture correctly accounts for physics of large and small black holes in AdS, as well as reproduces well-known inflationary predictions for cosmological parameters
We derive an absolute upper bound on the number of e-foldings, beyond which neither de Sitter nor inflationary Universe can be approximated by a semi-classical metric
In what follows we adopt the key concept of [1, 2]: Gravitational systems, such as black holes, AdS, de Sitter or other cosmological spaces represent composite entities of microscopic quantum constituent gravitons of wave-length set by the characteristic classical size R of the system
Summary
Before proceeding to AdS and Inflationary spaces, we wish to briefly review some ingredients of our black hole quantum portrait [1, 2] that will be useful later for drawing analogies as well as differences with other spaces. The constituents can be chosen to be arbitrarily weakly-coupled by taking their wave-length large From this perspective it is hard to expect anything dramatic as long as their number is below the black hole formation threshold N α−1. The entanglement effect is impossible to capture in the standard semi-classical description since in this case N = ∞ and generation of entanglement takes infinite time. We shall discuss this effect in more details below when we shall make the study of a similar effect for the inflationary Universe. This detailed construction might provide the clue — from the graviton condensate point of view — to unveil the black hole inner geometry
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