Growth of Structure in the Szekeres Class-II Inhomogeneous Cosmological Models and the Matter-Dominated Era

dc.contributor.ISNI0000 0001 2874 3832 (Ishak-Boushaki, M)
dc.contributor.authorIshak-Boushaki, Mustaphaen_US
dc.contributor.authorPeel, Austinen_US
dc.contributor.utdAuthorIshak-Boushaki, Mustaphaen_US
dc.contributor.utdAuthorPeel, Austinen_US
dc.date.accessioned2014-02-26T21:42:03Z
dc.date.available2014-02-26T21:42:03Z
dc.date.created2012-04-03en_US
dc.date.issued2012-04-03en_US
dc.description.abstractThis study belongs to a series devoted to using the Szekeres inhomogeneous models in order to develop a theoretical framework where cosmological observations can be investigated with a wider range of possible interpretations. While our previous work addressed the question of cosmological distances versus redshift in these models, the current study is a start at looking into the growth rate of large-scale structure. The Szekeres models are exact solutions to Einstein's equations that were originally derived with no symmetries. We use here a formulation of the Szekeres models that is due to Goode and Wainwright, who considered the models as exact perturbations of a Friedmann-Lemaître- Robertson-Walker (FLRW) background. Using the Raychaudhuri equation we write, for the two classes of the models, exact growth equations in terms of the under/overdensity and measurable cosmological parameters. The new equations in the overdensity split into two informative parts. The first part, while exact, is identical to the growth equation in the usual linearly perturbed FLRW models, while the second part constitutes exact nonlinear perturbations. We integrate numerically the full exact growth rate equations for the flat and curved cases. We find that for the matter-dominated cosmic era, the Szekeres growth rate is up to a factor of three to five stronger than the usual linearly perturbed FLRW cases, reflecting the effect of exact Szekeres nonlinear perturbations. We also find that the Szekeres growth rate with an Einstein-de Sitter background is stronger than that of the well-known nonlinear spherical collapse model, and the difference between the two increases with time. This highlights the distinction when we use general inhomogeneous models where shear and a tidal gravitational field are present and contribute to the gravitational clustering. Additionally, it is worth observing that the enhancement of the growth found in the Szekeres models during the matter-dominated era could suggest a substitute to the argument that dark matter is needed when using FLRW models to explain the enhanced growth and resulting large-scale structures that we observe today.en_US
dc.identifier.bibliographicCitationIshak, M., and A. Peel. 2012. "Growth of structure in the Szekeres class-II inhomogeneous cosmological models and the matter-dominated era." Physical Review D - Particles, Fields, Gravitation and Cosmology 85(8), doi:10.1103/PhysRevD.85.083502en_US
dc.identifier.issn1550-7998en_US
dc.identifier.issue8en_US
dc.identifier.urihttp://hdl.handle.net/10735.1/3073
dc.identifier.volume85en_US
dc.relation.urihttp://dx.doi.org/10.1103/PhysRevD.85.083502
dc.rights© 2012 American Physical Societyen_US
dc.sourcePhysical Review D - Particles, Fields, Gravitation and Cosmology
dc.subjectGravitational collapseen_US
dc.subjectDark energy (Astronomy)en_US
dc.subjectNaked singularities (Cosmology)en_US
dc.subjectExpanding universeen_US
dc.titleGrowth of Structure in the Szekeres Class-II Inhomogeneous Cosmological Models and the Matter-Dominated Eraen_US
dc.typeTexten_US
dc.type.genreArticleen_US

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