Reconstructing a model of quintessential inflation

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dc.creatorNeupane, Ishwaree P.
dc.date2007-06-19
dc.date2008-05-31
dc.date.accessioned2026-07-07T11:56:59Z
dc.date.available2026-07-07T11:56:59Z
dc.descriptionWe present an explicit cosmological model where inflation and dark energy both could arise from the dynamics of the same scalar field. We present our discussion in the framework where the inflaton field $ϕ$ attains a nearly constant velocity $m_P^{-1} |dϕ/dN|\equiv α+β\exp(βN)$ (where $N\equiv \ln a$ is the e-folding time) during inflation. We show that the model with $|α|<0.25$ and $β<0$ can easily satisfy inflationary constraints, including the spectral index of scalar fluctuations ($n_s=0.96\pm 0.013$), tensor-to-scalar ratio ($r<0.28$) and also the bound imposed on $Ω_ϕ$ during the nucleosynthesis epoch ($Ω_ϕ(1 {\rm MeV})<0.1$). In our construction, the scalar field potential always scales proportionally to the square of the Hubble expansion rate. One may thereby account for the two vastly different energy scales associated with the Hubble parameters at early and late epochs. The inflaton energy could also produce an observationally significant effective dark energy at a late epoch without violating local gravity tests.
dc.description18 pages, 7 figures; added refs, published version
dc.identifierhttps://arxiv.org/abs/0706.2654
dc.identifierhttp://arxiv.org/abs/0706.2654
dc.identifierClass.Quant.Grav.25:125013,2008
dc.identifierdoi:10.1088/0264-9381/25/12/125013
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205727
dc.subjectHigh Energy Physics - Theory
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Phenomenology
dc.titleReconstructing a model of quintessential inflation
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