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

• Verfasst von: Amendola, Luca [VerfasserIn]
• Verfasst von: Tsujikawa, Shinji [VerfasserIn]
• Titel: Phantom crossing, equation-of-state singularities, and local gravity constraints in f(R) models
• Verf.angabe: Luca Amendola, Shinji Tsujikawa
• Umfang: 8 S.
• Fussnoten: Gesehen am 15.11.2017
• Titel Quelle: Enthalten in: Physics letters / B
• Jahr Quelle: 2008
• Band/Heft Quelle: 660(2008), 3, S. 125-132
• ISSN Quelle: 1873-2445
• DOI: doi:10.1016/j.physletb.2007.12.041
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1565362799

Abstract

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 ΛCDM model (f=R−Λ) is quantified by the function m=Rf,RR/f,R. The matter epoch corresponds to m(r=−1)≃+0 (where r=−Rf,R/f) while the accelerated attractor exists in the region 0⩽m<1. We find that the equation of state wDE of all such “viable” f(R) models exhibits two features: wDE diverges at some redshift zc and crosses the cosmological constant boundary (“phantom crossing”) at a redshift zb smaller than zc. Using the observational data of Supernova Ia and Cosmic Microwave Background, we obtain the constraint m<O(0.1) and we find that the phantom crossing could occur at zb≳1, 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.