Single field inflationary models with non-compact Kaluza–Klein theory

2015

Can. J. Phys.

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Using a new kind of 5D Ricci-flat canonical metric, we obtain by a static foliation an effective 4D Schwarzschild -de Sitter hypersurface. We examine some particular initial conditions that could be responsible for the inflationary expansion of the early universe, which could be driven by the explosion of a white hole (WH). The zeroth-order spectrum outside the WH describes quantum fluctuations, which for a scale invariant power spectrum, can be expressed in terms of the cosmological constant, or the square mass of the WH.Résumé : À partir d'un nouveau type de métrique canonique plate de Ricci en 5D, nous obtenons par foliation statique une hypersurface effective de Schwarzschild -de Sitter en 4D. Nous examinons quelques conditions initiales particulières qui pourraient être responsables de l'inflation de l'univers jeune, entrainée par l'explosion d'un trou blanc. Le spectre de puissance d'ordre zéro à l'extérieur du trou blanc décrit des fluctuations quantiques que, pour un spectre de puissance invariant d'échelle, on peut exprimer en fonction de la constance cosmologique ou du carré de la masse du trou blanc.[Traduit par le Rédaction]

Section: Motivationmentioning

confidence: 99%

Inflation as a white hole explosion from a 5D vacuum

Anabitarte

2015

Can. J. Phys.

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“…A more detailed explanation can be found in [28]. This space will be a 5D extension of a 4D de Sitter spacetime, which is very relevant to inflationary cosmology, and is given by a 5D (canonical Riemann-flat) metric with a line element [29] …”

Section: Electrodynamics a Riemann-flat Extended De Sitter Spacetimementioning

confidence: 99%

Seminal magnetic fields from inflato-electromagnetic inflation

Membiela

2012

Eur. Phys. J. C

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We extend some previous attempts to explain the origin and evolution of primordial magnetic fields during inflation induced from a 5D vacuum. We show that the usual quantum fluctuations of a generalized 5D electromagnetic field cannot provide us with the desired magnetic seeds. We show that special fields without propagation on the extra non-compact dimension are needed to arrive to appreciable magnetic strengths. We also identify a new magnetic tensor field Bij in this kind of extra dimensional theories. Our results are in very good agreement with observational requirements, in particular from TeV Blazars and CMB radiation limits we obtain that primordial cosmological magnetic fields should be close to scale invariance.

“…To describe a 3D spatially isotropic and homogeneous universe, which is Ricci flat: R A BCD = 0 and describes a 5D vacuum: G AB = 0, we shall consider the background metric [12]…”

Section: Introduction and Overview Of The 5d Formalismmentioning

confidence: 99%

Cosmological expansion governed by a scalar field from a 5D vacuum

2006

Physics Letters B

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We consider a single field governed expansion of the universe from a five dimensional (5D) vacuum state. Under an appropiate change of variables the universe can be viewed in a effective manner as expanding in 4D with an effective equation of state which describes different epochs of its evolution. In the example here worked the universe fistly describes an inflationary phase, followed by a decelerated expansion. Thereafter, the universe is accelerated and describes a quintessential expansion to finally, in the future, be vacuum dominated.Comment: version accepted in Phys. Lett.