Scale-invariant Perturbation of the Friedmann Universe
| dc.creator | Abdalla, E. | |
| dc.creator | Mohayaee, Roya | |
| dc.date | 1997-06-17 | |
| dc.date | 1998-11-13 | |
| dc.date.accessioned | 2026-07-07T08:58:27Z | |
| dc.date.available | 2026-07-07T08:58:27Z | |
| dc.description | We use de Vaucouleurs' power-law density-distance relation, to study a hierarchical perturbation of the Friedmann universe. We solve the Einstein equation and obtain the density contrast and the amplification factor for the perturbation. It is shown that, scale-invariant inhomogeneities decay in Einstein-de-Sitter universe. On the contrary, in an open universe, the inhomogeneities grow. For low values of $Ω$, amplification peaks sharply and the fluctuations can grow by up to a factor of $10^{13}$ from the recombination to the present time. Our analysis of the closed universe further confirms that, unlike the common belief that perturbations grow faster with increasing $Ω$, scale-invariant perturbations amplify with decreasing $Ω$. This result is consistent with the very low density expected for a hierarchical universe. | |
| dc.description | extended version with new diagrams and discussions | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9706181 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9706181 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/147328 | |
| dc.subject | Astrophysics | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.subject | High Energy Physics - Theory | |
| dc.title | Scale-invariant Perturbation of the Friedmann Universe | |
| dc.type | text |