Phantom crossing, equation-of-state singularities, and local gravity constraints in f(R) models

Details Phantom crossing, equation-of-state singularities, and local gravity constraints in f(R) models Phantom crossing, equation-of-state singularities, and local gravity constraints in f(R) models

2007-05-03

arxiv.org/abs/0705.0396v3

Phys.Lett.B660:125-132,2008

Astronomy and Astrophysics

Astrophysics

8 pages, 3 figures, version to appear in Physics Letters B

Scientific paper

10.1016/j.physletb.2007.12.041

We identify the class of f(R) dark energy models which have a viable cosmology, i.e. a matter dominated epoch followed by a late-time acceleration. The deviation from a LambdaCDM model (f=R-Lambda) is quantified by the function m=Rf_{,RR}/f_{,R}. The matter epoch corresponds to m(r=-1) simeq +0 (where r=-Rf_{,R}/f) while the accelerated attractor exists in the region 01, i.e. within reach of observations. If we add local gravity constraints, the bound on m becomes very stringent, with m several orders of magnitude smaller than unity in the region whose density is much larger than the present cosmological density. The representative models that satisfy both cosmological and local gravity constraints take the asymptotic form m(r)=C(-r-1)^p with p>1 as r approaches -1.

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