1997/06/17 by Élcio Abdalla, Abdalla, E., Roya Mohayaee +1
Physics and Astronomy · #Astrophysics (astro-ph) #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #General Relativity and Quantum Cosmology (gr-qc) #High Energy Physics - Theory (hep-th)
paper · pdf · doi:10.48550/arxiv.astro-ph/9706181
openalex publication_date 1997/06/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 1013 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.