Towards classification of simple dark energy cosmological models

Details Towards classification of simple dark energy cosmological models Towards classification of simple dark energy cosmological models

2006-08-20

arxiv.org/abs/gr-qc/0608098v1

ECONFC0602061:18,2006; Int.J.Geom.Meth.Mod.Phys.4:313,2007

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

10 pages, 2 figures, the paper presented at 42nd Karpacz Winter School of Theoretical Physics: Ladek, Poland, 6-11 Feb 2006

Scientific paper

10.1142/S0219887807002016

We characterize a class of simple FRW models filled by both dark energy and dark matter in notion of a single potential function of the scale factor $a(t)$; $t$ is the cosmological time. It is representing potential of fictitious particle - Universe moving in 1-dimensional well $V(a)$ which the positional variable mimics the evolution of the Universe. Then the class of all dark energy models (called a multiverse) can be regarded as a Banach space naturally equipment in the structure of the Sobolev metric. In this paper we explore notion of $C^{1}$ metric introduced in the multiverse which measure distance between any two dark energy models. If we choose cold dark matter as a reference one then we can find how so far apart are different models offering explanation of present accelerating expansion phase of the Universe. We consider both models with dark energy (models with the generalized Chaplygin gas, models with variable coefficient equation of state $w_{X}=\frac{p_{X}}{\rho_{X}}$ parameterized by redshift $z$, models with phantom matter) as well as models basing on some modification of the Friedmann equation (Cardassian models, Dvali-Gabadadze-Porati brane models). We argue that because observational data still favor the $\Lambda$CDM model all reasonable dark energy models should belong to the nearby neighborhood of this model.

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