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The “still point” cosmology

Published online by Cambridge University Press:  26 May 2016

Ivan I. Shevchenko
Ivan I. Shevchenko*
Affiliation:
Pulkovo Observatory, Russian Academy of Sciences, Pulkovskoje ave. 65/1, St. Petersburg 196140, Russia. Email: [email protected]

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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 = ρM/ρcr, ΩV = ρv/ρcr, 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
Information
Symposium - International Astronomical Union , Volume 201: New Cosmological Data and the Values of the Fundamental Parameters , 2005 , pp. 514 - 515
Copyright
Copyright © Astronomical Society of the Pacific 2005 

References

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