Growth of Structure in the Szekeres Class-II Inhomogeneous Cosmological Models and the Matter-Dominated Era
| dc.contributor.ISNI | 0000 0001 2874 3832 (Ishak-Boushaki, M) | |
| dc.contributor.author | Ishak-Boushaki, Mustapha | en_US |
| dc.contributor.author | Peel, Austin | en_US |
| dc.contributor.utdAuthor | Ishak-Boushaki, Mustapha | en_US |
| dc.contributor.utdAuthor | Peel, Austin | en_US |
| dc.date.accessioned | 2014-02-26T21:42:03Z | |
| dc.date.available | 2014-02-26T21:42:03Z | |
| dc.date.created | 2012-04-03 | en_US |
| dc.date.issued | 2012-04-03 | en_US |
| dc.description.abstract | This 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-LemaƮtre- 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.bibliographicCitation | Ishak, 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.85.083502 | en_US |
| dc.identifier.issn | 1550-7998 | en_US |
| dc.identifier.issue | 8 | en_US |
| dc.identifier.uri | http://hdl.handle.net/10735.1/3073 | |
| dc.identifier.volume | 85 | en_US |
| dc.relation.uri | http://dx.doi.org/10.1103/PhysRevD.85.083502 | |
| dc.rights | Ā© 2012 American Physical Society | en_US |
| dc.source | Physical Review D - Particles, Fields, Gravitation and Cosmology | |
| dc.subject | Gravitational collapse | en_US |
| dc.subject | Dark energy (Astronomy) | en_US |
| dc.subject | Naked singularities (Cosmology) | en_US |
| dc.subject | Expanding universe | en_US |
| dc.title | Growth of Structure in the Szekeres Class-II Inhomogeneous Cosmological Models and the Matter-Dominated Era | en_US |
| dc.type | Text | en_US |
| dc.type.genre | Article | en_US |