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\({\mathcal {H}}\)olographic \({\mathcal {N}}\)aturalness and \({\mathcal {C}}\)osmological \({\mathcal {R}}\)elaxation

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Abstract

We rediscuss the main Cosmological Problems as illusions originated from our ignorance of the hidden information holographically stored in vacuo. The Cosmological vacuum state is full of a large number of dynamical quantum hairs, dubbed hairons, which dominate the Cosmological Entropy. We elaborate on the Cosmological Constant (CC) problem, in both the dynamical and time-constant possibilities. We show that all dangerous quantum mixings between the CC and the Planck energy scales are exponentially suppressed as an entropic collective effect of the hairon environment. As a consequence, the dark energy scale is UV insensitive to any Planckian corrections. On the other hand, the inflation scale is similarly stabilized from any radiative effects. In the case of the Dark energy, we show the presence of a holographic entropic attractor, favoring a time variation of \(\Lambda \rightarrow 0\) in future rather than a static CC case, i.e., the \(w>-1\) Dynamical DE is favored over a CC or a \(w<-1\) phantom cosmology. In both the inflation and dark energy sectors, we elaborate on the Trans-Planckian problem, in relation with the recently proposed Trans-Planckian Censorship Conjecture (TCC). We show that the probability for any sub-Planckian wavelength modes to survive after inflation is completely negligible as a holographic wash-out mechanism. In other words, the hairons provide for a holographic decoherence of the transplanckian modes in a holographic scrambling time. This avoids the TCC strong bounds on the Inflaton and DE potentials.

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This manuscript has associated data in a data repository. [Authors’ comment: I state that the research datas of this paper are deposited in publicly available repositories.]

Notes

  1. See Ref. [2] for a review on the CC problem.

  2. Interesting discussions on implications on the Primordial Black Hole production in the early Universe can be found in Refs. [10, 11]

  3. Possible quantum hairs were discussed by many authors as a way-out to the Black Hole information paradox, e.g., see Refs. [15,16,17,18,19,20,21,22,23,24,25,26,27].

  4. See also recent discussions of the \(\mathcal {HN}\) in contest of particle physics [28] and topological aspects [29].

  5. The HN paradigm is flowing in continuity with many intuitions and approaches proposed in literature before in Refs. [30,31,32,33,34,35,36,37,38,39,40,41,42,43,44,45,46,47,48,49,50,51,52,53,54,55,56,57].

  6. A dynamical relaxation mechanism can be considered in a string-theory holographic setup as in Ref. [67].

  7. See Refs. [68,69,70, 70,71,72,73] for a panoramic view on the problem of phantom cosmology and singularities.

  8. See also Ref. [9] for stronger TCC bounds on the tensor-to-scalar ratio r parameter of inflation.

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Acknowledgements

We wish to thank S. Pi for valuable comments on these aspects.

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  1. Center for Theoretical Physics, College of Physics Science and Technology, Sichuan University, Chengdu, 610065, China

    Andrea Addazi

  2. INFN Sezione Roma Tor Vergata, 00133, Rome, Italy

    Andrea Addazi

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Addazi, A. \({\mathcal {H}}\)olographic \({\mathcal {N}}\)aturalness and \({\mathcal {C}}\)osmological \({\mathcal {R}}\)elaxation. Eur. Phys. J. Plus 135, 940 (2020). https://doi.org/10.1140/epjp/s13360-020-00933-4

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