Hostname: page-component-848d4c4894-xfwgj Total loading time: 0 Render date: 2024-07-01T07:40:56.133Z Has data issue: false hasContentIssue false

The “still point” cosmology

Published online by Cambridge University Press:  26 May 2016

Ivan I. Shevchenko*
Affiliation:
Pulkovo Observatory, Russian Academy of Sciences, Pulkovskoje ave. 65/1, St. Petersburg 196140, Russia. Email: iis@gao.spb.ru

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Recent results on supernovae as standard candles (Riess et al. 1998; Perlmutter et al. 1999) and on CMB anisotropy (Lineweaver 1998) indicate that ΩM ≍ 0.3-0.4, Ωv ≍ 0.6-0.7, ΩM + Ωv ≍ 1. By definition, ΩM = ρMcr, ΩV = ρvcr, where ρM is the matter density, ρv is the vacuum density; the critical density ρcr = 3H2/8πG; H is the Hubble parameter, G is the gravitational constant. In the standard Friedmann-Lemaître cosmologies, these results seriously constrain the non-dimensional cosmological constant (as defined below): Δ ≫ 1, meaning that the Universe expands forever. If a scalar field is present, the future evolution may be different.

Type
Part XII: Poster Papers
Copyright
Copyright © Astronomical Society of the Pacific 2005 

References

Dolgov, A. D., Zel'dovich, Ya. B. & Sashimi, M. V. 1988, Cosmology of the Early Universe (Moscow Univ.: Moscow) (in Russian).Google Scholar
Lineweaver, C. H. 1998, ApJ, 505, L69.Google Scholar
Perlmutter, V. S. et al. 1999, ApJ, 517, 565.Google Scholar
Riess, A. G. et al. 1998, AJ, 116, 1009.Google Scholar
Shevchenko, I. I. 1993, Astrophys. and Space Sci., 202, 45.Google Scholar