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dc.contributor.authorHaro Cases, Jaume
dc.contributor.authorAmorós Torrent, Jaume
dc.contributor.authorPan, Supriya
dc.contributor.otherUniversitat Politècnica de Catalunya. Departament de Matemàtiques
dc.date.accessioned2016-09-12T12:07:40Z
dc.date.available2016-09-12T12:07:40Z
dc.date.issued2016-04-12
dc.identifier.citationHaro, J., Amoros, J., Pan, S. Simple inflationary quintessential model. "PHYSICAL REVIEW D", 12 Abril 2016, vol. 93, núm. 8.
dc.identifier.issn2470-0010
dc.identifier.urihttp://hdl.handle.net/2117/89829
dc.description.abstractIn the framework of a flat Friedmann-Lemaitre-Robertson-Walker geometry, we present a nongeodesically past complete model of our Universe without the big bang singularity at finite cosmic time, describing its evolution starting from its early inflationary era up to the present accelerating phase. We found that a hydrodynamical fluid with nonlinear equation of state could result in such scenario, which after the end of this inflationary stage, suffers a sudden phase transition and enters into the stiff matter dominated era, and the Universe becomes reheated due to a huge amount of particle production. Finally, it asymptotically enters into the de Sitter phase concluding the present accelerated expansion. Using the reconstruction technique, we also show that this background provides an extremely simple inflationary quintessential potential whose inflationary part is given by the well-known 1-dimensional Higgs potential, i.e., a double well inflationary potential, and the quintessential one by an exponential potential that leads to a deflationary regime after this inflation, and it can depict the current cosmic acceleration at late times. Moreover the Higgs potential leads to a power spectrum of the cosmological perturbations which fit well with the latest Planck estimations. Further, we compared our viable potential with some known inflationary quintessential potential, which shows that our quintessential model, that is, the Higgs potential combined with the exponential one, is an improved version of them because it contains an analytic solution that allows us to perform all analytic calculations. Finally, we have shown that the introduction of a nonzero cosmological constant simplifies the potential considerably with an analytic behavior of the background which again permits us to evaluate all the quantities analytically.
dc.language.isoeng
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.subjectÀrees temàtiques de la UPC::Matemàtiques i estadística
dc.subject.lcshcosmology
dc.subject.otherEmergent universe
dc.subject.otherparticle-production
dc.subject.othercosmology
dc.subject.otherfields
dc.subject.otherscenario
dc.subject.otherflatness
dc.subject.othercreation
dc.subject.otherhorizon
dc.titleSimple inflationary quintessential model
dc.typeArticle
dc.subject.lemacCosmologia
dc.contributor.groupUniversitat Politècnica de Catalunya. EDP - Equacions en Derivades Parcials i Aplicacions
dc.contributor.groupUniversitat Politècnica de Catalunya. GEOMVAP - Geometria de Varietats i Aplicacions
dc.identifier.doi10.1103/PhysRevD.93.084018
dc.description.peerreviewedPeer Reviewed
dc.rights.accessOpen Access
drac.iddocument18544198
dc.description.versionPostprint (author's final draft)
upcommons.citation.authorHaro, J., Amoros, J., Pan, S.
upcommons.citation.publishedtrue
upcommons.citation.publicationNamePHYSICAL REVIEW D
upcommons.citation.volume93
upcommons.citation.number8


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