Cosmological Perturbations in Phantom Dark Energy Models
dc.contributor.author | Albarran, Imanol | |
dc.contributor.author | Bouhmadi López, Mariam | |
dc.contributor.author | Morais, Joao | |
dc.date.accessioned | 2018-12-14T19:19:07Z | |
dc.date.available | 2018-12-14T19:19:07Z | |
dc.date.issued | 2017-03-06 | |
dc.identifier.citation | Universe 3(1) : (2017) // Article ID 22 | es_ES |
dc.identifier.issn | 2218-1997 | |
dc.identifier.uri | http://hdl.handle.net/10810/30389 | |
dc.description.abstract | The CDM paradigm, characterised by a constant equation of state w = -1 for dark energy, is the model that better fits observations. However, the same observations strongly support the possibility of a dark energy content where the corresponding equation of state is close to but slightly smaller than -1. In this regard, we focus on three different models where the dark energy content is described by a perfect fluid with an equation of state which can evolve or not. The three proposals show very similar behaviour at present, while the asymptotic evolution of each model drives the Universe to different abrupt events known as (i) Big Rip; (ii) Little Rip (LR); and (iii) Little Sibling of the Big Rip. With the aim of comparing these models and finding possible imprints in their predicted matter distribution, we compute the matter power spectrum and the growth rate fs. We conclude that the model which induces a LR seems to be favoured by observations. | es_ES |
dc.description.sponsorship | The work of I. A. was supported by a Santander-Totta fellowship "Bolsas de Investigacao Faculdade de Ciencias (UBI) - Santander Totta". The work of M.B.-L. is supported by the Portuguese Agency "Fundacao para a Ciencia e Tecnologia" through an Investigador FCT Research contract, with reference IF/01442/2013/CP1196/CT0001. She also wishes to acknowledge the partial support from the Basque government Grant No. IT592-13 (Spain) and FONDOS FEDER under grant FIS2014-57956-P (Spanish government). This research work is partially supported by the grant UID/MAT/00212/2013. J.M. is thankful to UPV/EHU for a PhD fellowship and acknowledges the support from the Basque government Grant No. IT592-13 (Spain) and FONDOS FEDER, under grant FIS2014-57956-P (Spanish Government). The authors acknowledge the COST Action CA15117 (CANTATA). | es_ES |
dc.language.iso | eng | es_ES |
dc.publisher | MDPI | es_ES |
dc.rights | info:eu-repo/semantics/openAccess | es_ES |
dc.rights.uri | http://creativecommons.org/licenses/by/3.0/es/ | * |
dc.subject | dark energy | es_ES |
dc.subject | cosmological perturbations | es_ES |
dc.subject | cosmic singularities | es_ES |
dc.title | Cosmological Perturbations in Phantom Dark Energy Models | es_ES |
dc.type | info:eu-repo/semantics/article | es_ES |
dc.rights.holder | © 2017 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license ( http://creativecommons.org/licenses/by/4.0/). | es_ES |
dc.rights.holder | Atribución 3.0 España | * |
dc.relation.publisherversion | https://www.mdpi.com/2218-1997/3/1/22 | es_ES |
dc.identifier.doi | 10.3390/universe3010022 | |
dc.departamentoes | Física teórica e historia de la ciencia | es_ES |
dc.departamentoeu | Fisika teorikoa eta zientziaren historia | es_ES |
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Except where otherwise noted, this item's license is described as © 2017 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license ( http://creativecommons.org/licenses/by/4.0/).