On "Observational Constraints on Power-Law Cosmologies"
| dc.creator | Meetu, Sethi | |
| dc.creator | Annu, Batra | |
| dc.creator | Daksh, Lohiya | |
| dc.date | 1999-03-05 | |
| dc.date.accessioned | 2026-07-07T02:30:41Z | |
| dc.date.available | 2026-07-07T02:30:41Z | |
| dc.description | "Power Law Cosmologies" are defined by their growth of the cosmological scale factor as $ t^α$ regardless of the matter content or cosmological epoch. Constraints from the current age of the Universe and from the high redshift supernovae data require ``large'' $α$ ($\approx 1$). We reinforce this by latest available observations. Such a large $α$ is also consistent with the right amount of helium and the lowest observed metallicity in the universe for a model with the baryon entropy ratio $\approx 8.1\times 10^{-9}$. | |
| dc.description | Plain Tex File, 4 postscript figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9903084 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9903084 | |
| dc.identifier | Phys.Rev. D60 (1999) 108301 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/13898 | |
| dc.subject | Astrophysics | |
| dc.title | On "Observational Constraints on Power-Law Cosmologies" | |
| dc.type | text |