Cosmic inventory of energy densities: issues and concerns
| dc.creator | Padmanabhan, T. | |
| dc.date | 2001-12-26 | |
| dc.date.accessioned | 2026-07-25T17:03:00Z | |
| dc.description | The dynamics of our universe is characterised by the density parameters for cosmological constant ($Ω_V$), nonbaryonic darkmatter($Ω_{\rm wimp}$), radiation ($Ω_R$) and baryons ($Ω_B$). To these parameters -- which describe the smooth background universe -- one needs to add at least another dimensionless number ($\sim 10^{-5}$) characterising the strength of primordial fluctuations in the gravitational potential, in order to ensure formation of structures by gravitational instability. I discuss several issues related to the description of the universe in terms of these numbers and argue that we do not yet have a fundamental understanding of these issues. | |
| dc.description | Based on the invited talk at the XIII Rencontres de Blois - Frontiers of the Universe, June 17-23,2001 | |
| dc.identifier | https://arxiv.org/abs/gr-qc/0112068 | |
| dc.identifier | http://arxiv.org/abs/gr-qc/0112068 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/45287 | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.subject | Astrophysics | |
| dc.subject | High Energy Physics - Theory | |
| dc.title | Cosmic inventory of energy densities: issues and concerns | |
| dc.type | text |