Stiff-matter solitons in cosmology

Pullin, Jorge

doi:10.1007/bf00658832

Cited by 1 publication

(2 citation statements)

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“…Comparing (36) and ( 38) with (30) we see that IR perturbations do not yield a scale invariant spectrum once they cross the Hubble horizon. Independent of the initial vacuum choice, a logarithmic and an oscillatory correction are present.…”

Section: Discussionmentioning

confidence: 93%

“…Deep inside the Hubble horizon the spectrum of fluctuations is scale invariant according to (30), but due to IR fluctuations entering during the holographic phase, the spectrum becomes k-dependent according to (36) or (38) (even inside the Hubble horizon). For the oscillatory effects to be invisible in the CMBR, a period of inflation after the p = ρ phase has to last for a sufficient number of e-foldings.…”

Section: Discussionmentioning

confidence: 99%

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Perturbations in a holographic universe and in other stiff fluid cosmologies

Battefeld

Easson

2004

Phys. Rev. D

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We examine the generation and evolution of perturbations in a universe dominated by a fluid with stiff equation of state p = ρ. The recently proposed Holographic Universe is an example of such a model. We compute the spectrum of scalar and tensor perturbations, without relying on a microphysical description of the p = ρ fluid. The spectrum is scale invariant deep inside the Hubble horizon. In contrast, infrared perturbations that enter the Hubble horizon during the stiff fluid dominated (holographic) phase yield oscillatory and logarithmic terms in the power spectrum. We show that vector perturbations grow during the stiff fluid dominated epoch and may result in a turbulent and anisotropic Universe at the end of the holographic phase. Therefore, the required period of inflation following the holographic phase cannot be much shorter than that required in standard inflationary models.PACS numbers: 98.80.Cq.

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Section: Discussionmentioning

confidence: 93%