Primordial inflation and present-day cosmological constant from extra dimensions

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Abstract

A semiclassical gravitation model is outlined which makes use of the Casimir energy density of vacuum fluctuations in extra compactified dimensions to produce the present-day cosmological constant as ρΛ ∼ M8/M4 p, where M p is the Planck scale and M is the weak interaction scale. The model is based on (4 + D)-dimensional gravity, with D = 2 extra dimensions with radius b(t) curled up at the ADD length scale b0 = Mp/M2 ∼ 0.1 mm. Vacuum fluctuations in the compactified space perturb b0 very slightly, generating a small present-day cosmological constant. The radius of the compactified dimensions is predicted to be b0 ≈ k1/40.09 mm (or equivalently M ≈ 2.4 TeV/k1/8), where the Casimir energy density is k/b4. Primordial inflation of our three-dimensional space occurs as in the cosmology of the ADD model as the inflaton b(t), which initially is on the order of 1/M ∼ 10-17 cm, rolls down its potential to b0.

Original languageEnglish (US)
Pages (from-to)21-25
Number of pages5
JournalPhysics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics
Volume524
Issue number1-2
DOIs
StatePublished - Jan 3 2002

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flux density
gravitation
vacuum
radii
cosmology

Keywords

  • Cosmological constant
  • Extra dimensions
  • Inflationary cosmology

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

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title = "Primordial inflation and present-day cosmological constant from extra dimensions",
abstract = "A semiclassical gravitation model is outlined which makes use of the Casimir energy density of vacuum fluctuations in extra compactified dimensions to produce the present-day cosmological constant as ρΛ ∼ M8/M4 p, where M p is the Planck scale and M is the weak interaction scale. The model is based on (4 + D)-dimensional gravity, with D = 2 extra dimensions with radius b(t) curled up at the ADD length scale b0 = Mp/M2 ∼ 0.1 mm. Vacuum fluctuations in the compactified space perturb b0 very slightly, generating a small present-day cosmological constant. The radius of the compactified dimensions is predicted to be b0 ≈ k1/40.09 mm (or equivalently M ≈ 2.4 TeV/k1/8), where the Casimir energy density is k/b4. Primordial inflation of our three-dimensional space occurs as in the cosmology of the ADD model as the inflaton b(t), which initially is on the order of 1/M ∼ 10-17 cm, rolls down its potential to b0.",
keywords = "Cosmological constant, Extra dimensions, Inflationary cosmology",
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N2 - A semiclassical gravitation model is outlined which makes use of the Casimir energy density of vacuum fluctuations in extra compactified dimensions to produce the present-day cosmological constant as ρΛ ∼ M8/M4 p, where M p is the Planck scale and M is the weak interaction scale. The model is based on (4 + D)-dimensional gravity, with D = 2 extra dimensions with radius b(t) curled up at the ADD length scale b0 = Mp/M2 ∼ 0.1 mm. Vacuum fluctuations in the compactified space perturb b0 very slightly, generating a small present-day cosmological constant. The radius of the compactified dimensions is predicted to be b0 ≈ k1/40.09 mm (or equivalently M ≈ 2.4 TeV/k1/8), where the Casimir energy density is k/b4. Primordial inflation of our three-dimensional space occurs as in the cosmology of the ADD model as the inflaton b(t), which initially is on the order of 1/M ∼ 10-17 cm, rolls down its potential to b0.

AB - A semiclassical gravitation model is outlined which makes use of the Casimir energy density of vacuum fluctuations in extra compactified dimensions to produce the present-day cosmological constant as ρΛ ∼ M8/M4 p, where M p is the Planck scale and M is the weak interaction scale. The model is based on (4 + D)-dimensional gravity, with D = 2 extra dimensions with radius b(t) curled up at the ADD length scale b0 = Mp/M2 ∼ 0.1 mm. Vacuum fluctuations in the compactified space perturb b0 very slightly, generating a small present-day cosmological constant. The radius of the compactified dimensions is predicted to be b0 ≈ k1/40.09 mm (or equivalently M ≈ 2.4 TeV/k1/8), where the Casimir energy density is k/b4. Primordial inflation of our three-dimensional space occurs as in the cosmology of the ADD model as the inflaton b(t), which initially is on the order of 1/M ∼ 10-17 cm, rolls down its potential to b0.

KW - Cosmological constant

KW - Extra dimensions

KW - Inflationary cosmology

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