Hubble tension bounds the GUP and EUP parameters

Aghababaei, S.; Moradpour, H.; Vagenas, Elias C.

doi:10.48550/arxiv.2109.14826

Cited by 3 publications

(6 citation statements)

References 52 publications

(86 reference statements)

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“…In this case, there is a surprising accidental cancelation of the parameters so that Σ = 0 and a minimum length scale does not appear in scattering processes. 2 Renormalisable theories possess no natural scale, whereas non-renormalisable theories contain an intrinsic scale which is then used as a cut-off to define the effective field theory and its range of validity. For lengths below this scale, the effective field theory breaks down and ultraviolet phenomena cannot be described without a ultraviolet completion.…”

Section: Length Scale In Scatteringsmentioning

confidence: 99%

Horizon quantum mechanics and the inner side of black holes

Casadio

Giusti

Giugno

et al. 2022

The Fifteenth Marcel Grossmann Meeting

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The idea that gravity can act as a regulator of ultraviolet divergences is almost a century old and has inspired several approaches to quantum gravity. In fact, a minimum Planckian length can be shown to emerge from the nonlinear dynamics of gravity in the effective field theory approach to gravitational scatterings at Planckian energies. A simple quantum description of the gravitational collapse of a ball of dust supports the conclusion that such a length scale is indeed dynamical and matter inside black holes forms extended cores of macroscopic size. The geometry of these quantum black holes can be described by coherent states which cannot contain modes of arbitrarily short wavelength, compatibly with a matter core of finite size. Therefore, the classical central singularity is not realised, yet the expected general relativistic behaviour can be recovered in the weak-field region outside the horizon with good approximation. Deviations from classical general relativistic solutions are still present and form quantum hair which modify the thermodynamical description of black holes. These quantum black holes also avoid the presence of inner (Cauchy) horizons, since the effective energy density and pressures are integrable, as required by quantum physics, and not as regular as in classical physics.

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Section: Length Scale In Scatteringsmentioning

confidence: 99%

Horizon quantum mechanics and the inner side of black holes

Casadio

Giusti

Giugno

et al. 2022

The Fifteenth Marcel Grossmann Meeting

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“…By resorting to the standard Heisenberg uncertainty principle at cosmological scales [46,47] as well as some of its generalized versions as semi-classical approaches to quantum gravity (QG) [48], further interesting ideas for solving the HT have been brought forward, too. Taking QG into account can be relevant, as quantum fluctuations were produced during the Planck epoch, which, after propagating through spacetime, generated primordial fluctuations in the inflationary era.…”

Section: Introductionmentioning

confidence: 99%

Hubble tension as a guide for refining the early Universe: Cosmologies with explicit local Lorentz and diffeomorphism violation

Khodadi¹,

Schreck²

2023

Preprint

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This paper is dedicated to assessing modified cosmological settings based on the gravitational Standard-Model Extension (SME). Our analysis rests upon the Hubble tension (HT), which is a discrepancy between the observational determination of the Hubble parameter via data from the Cosmic Microwave Background (CMB) and Type Ia supernovae, respectively. While the latter approach is model-independent, the former highly depends on the model used to describe the physics of the early Universe. Motivated by the HT, we take into account two recently introduced cosmological models as test frameworks of the pre-CMB era. These settings involve local Lorentz and diffeomorphism violation parameterized by nondynamical SME background fields s 00 and s ij , respectively. We aim at explaining the tension in the measured results of the cosmic expansion rate in early and late epochs by resorting to these two modified cosmologies as potential descriptions of the pre-CMB era. As long as the HT does not turn out to be a merely systematic effect, it can serve as a criterion for exploring regions of the parameter space in certain pre-CMB new-physics candidates such as SME cosmologies. By setting extracted limits on SME coefficients into perspective with already existing bounds in the literature, we infer that none of the aforementioned models are suitable pre-CMB candidates for fixing the HT. In this way, new physics arising from the particular realizations of Lorentz and diffeomorphism violation studied in this article does not explain the HT. Our paper exemplifies how to exploit this discrepancy as a novel possibility of refining our description of the early Universe.

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“…The Heisenberg principle, considered at cosmological scales, has been adopted [1] to address the so-called Hubble tension [2][3][4][5][6][7][8][9][10][11] taking into account the differences between kinematic and dynamical measurements of the Hubble-Lemaître constant 1 H 0 . Here, we want to investigate if the Heisenberg principle has other roles at cosmological scales and if there are implications for fundamental physics.…”

mentioning

confidence: 99%

“…The distance of 8.4 Gpc falls into the radius of the observable universe 8 , that is the cosmological region causally connected by light. We can now reinterpret λ H as the Heisenberg radius, the cosmological length beyond which the indeterminacy principle prevails 9 .…”

mentioning

confidence: 99%

“…For a flat universe, Ω k = 0, the luminosity distance is (1 + z) times the comoving distance, achieving thereby extremely large values for increasing z. 9 McCrea [49] used the term uncertainty for pointing out the consequences of the finitude of the speed of light on the observability of the universe and did not address the Heisenberg principle in any manner. In [50][51][52], the origin of probability in cosmology, the relations to inflation, the boundaries of knowledge are addressed.…”

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confidence: 99%

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The Heisenberg limit at cosmological scales

Spallicci,

Benetti,

Capozziello

2021

Preprint

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For an observation time equal to the universe age, the Heisenberg principle fixes the value of the smallest measurable mass at mH = 1.35 × 10 −69 kg and prevents to probe the masslessness for any particle using a balance. The corresponding reduced Compton length to mH is λH, and represents the length limit beyond which masslessness cannot be proved using a metre ruler. In turns, λH is equated to the luminosity distance dH which corresponds to a red shift zH. When using the Concordance-Model parameters, we get dH = 8.4 Gpc and zH = 1.3. Remarkably, dH falls quite short to the radius of the observable universe. According to this result, tensions in cosmological parameters could be nothing else but due to comparing data inside and beyond zH. Finally, in terms of quantum quantities, the expansion constant H0 reveals to be one order of magnitude above the smallest measurable energy, divided by the Planck constant.

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Hubble tension bounds the GUP and EUP parameters

Cited by 3 publications

References 52 publications

Horizon quantum mechanics and the inner side of black holes

Horizon quantum mechanics and the inner side of black holes

Hubble tension as a guide for refining the early Universe: Cosmologies with explicit local Lorentz and diffeomorphism violation

The Heisenberg limit at cosmological scales

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