Endolymph pH in the Inner Ear of Guinea Pigs.

Tsujikawa, Satoshi; Yamashita, Toshio; Cho, Hisayuki; Kumazawa, Tadami; Vosteen, K. H.

doi:10.5631/jibirin.85.1651

Cited by 7 publications

(8 citation statements)

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“…Indeed it is to this class of models to which one must turn for a scenario, which not only gives rise to quintessential-inflation, but also satisfies all other observational constraints -particularly those on the spectral index and the scalar to tensor ratio placed by WMAP+SDSS [4,55]. It is well known that steep inflation in the RS scenario comes into conflict with observations [56] while GB brane world can rescue these models [57]. Indeed, it appears that steep inflation in GB models which commences at an intermediate energy scale between RS and GB regimes -can be easily reconciled with observations [57].…”

Section: Discussionmentioning

confidence: 99%

Quintessential inflation on the brane and the relic gravity wave background

2004

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Quintessential inflation describes a scenario in which both inflation and dark energy (quintessence) are described by the same scalar field. In conventional braneworld models of quintessential inflation gravitational particle production is used to reheat the universe. This reheating mechanism is very inefficient and results in an excessive production of gravity waves which violate nucleosynthesis constraints and invalidate the model. We describe a new method of realizing quintessential inflation on the brane in which inflation is followed by 'instant preheating' . The larger reheating temperature in this model results in a smaller amplitude of relic gravity waves which is consistent with nucleosynthesis bounds. The relic gravity wave background has a 'blue' spectrum at high frequencies and is a generic byproduct of successful quintessential inflation on the brane.

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Section: Discussionmentioning

confidence: 99%

Quintessential inflation on the brane and the relic gravity wave background

2004

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“…Further, the time parameter can be eliminated from the obtained time dependence of (F (t) − F (t = 0))/ √ 2C and X(t) by numerically evaluating both the quantities at same values of t from which we subsequently obtain the X-dependence the quantity (F (X) − F (X 0 ))/ √ 2C. Now recall standard theories of homogeneous inflation [48,49]. There the potential energy of a homogeneous scalar field φ, usually called inflaton (described by Lagrangians with canonical kinetic terms), leads to the exponential expansion of the universe.…”

Section: The K-essence Scalar Field Model and Its Contact With Obmentioning

confidence: 99%

The k-essence scalar field in the context of Supernova Ia observations

2012

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A k-essence scalar field model having (non canonical) Lagrangian of the form L = −V (φ)F (X) where X = 1 2 g µν ∇µφ∇νφ with constant V (φ) is shown to be consistent with luminosity distanceredshift data observed for type Ia Supernova. For constant V (φ), F (X) satisfies a scaling relation which is used to set up a differential equation involving the Hubble parameter H, the scale factor a and the k-essence field φ. H and a are extracted from SNe Ia data and using the differential equation the time dependence of the field φ is found to be: φ(t) ∼ λ0 + λ1t + λ2t 2 . The constants λi have been determined. The time dependence is similar to that of the quintessence scalar field (having canonical kinetic energy) responsible for homogeneous inflation. Furthermore, the scaling relation and the obtained time dependence of the field φ is used to determine the X-dependence of the function F (X).

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“…For a minimally coupled scalar field model, a number of studies have been done for reconstructing the potential for this scalar field in a model independent way by using observational data [11]. Recently Tsujikawa has studied the reconstruction of the potential function V (φ) in the k-essence Lagrangian once one assumes a certain form for the kinetic energy function F (X) [12]. But until now, there is no attempt in the literature to reconstruct in a model independent way the function F (X) in the k-essence Lagrangian.…”

Section: Introductionmentioning

confidence: 99%

Reconstructing k-essence

Sen

2006

J. Cosmol. Astropart. Phys.

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We present a model independent method of reconstructing the Lagrangian for the k-essence field driving the present acceleration of the universe. We consider the simplest k-essence model for which the potential is constant. Later we use three parametrizations for the Hubble parameter H(z), consistent with recent the SN1a data, to yield the Lagrangian F . Our reconstruction program does not generate any physically realistic Lagrangian for models that allow phantom crossing, whereas models without phantom crossing, yield well behaved Lagrangians.PACS numbers: 98.80.Es, 98.70.Vc

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Endolymph pH in the Inner Ear of Guinea Pigs.

Cited by 7 publications

References 0 publications

Quintessential inflation on the brane and the relic gravity wave background

Quintessential inflation on the brane and the relic gravity wave background

The k-essence scalar field in the context of Supernova Ia observations

Reconstructing k-essence

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