Conditions for the cosmological viability of f(R) dark energy models

• Verfasst von: Amendola, Luca [VerfasserIn]
• Titel: Conditions for the cosmological viability of f(R) dark energy models
• Verf.angabe: Luca Amendola, INAF/Osservatorio Astronomico di Roma, Via Frascati 33, 00040 Monte Porzio Catone (Roma), Italy ; Radouane Gannouji and David Polarski, LPTA, Universite Montpellier II, CNRS, 34095 Montpellier Cedex 05, France ; Shinji Tsujikawa, Department of Physics, Gunma National College of Technology, Gunma 371-8530, Japan
• Fussnoten: Gesehen am 15.11.2017
• Titel Quelle: Enthalten in: Physical review / D
• Jahr Quelle: 2007
• Band/Heft Quelle: 75(2007,08) Artikel-Nummer 083504, 22 Seiten
• ISSN Quelle: 1550-2368
• ISSN Quelle: 1089-4918
• DOI: doi:10.1103/PhysRevD.75.083504
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1565367154

Abstract

We derive the conditions under which dark energy models whose Lagrangian densities f are written in terms of the Ricci scalar R are cosmologically viable. We show that the cosmological behavior of f(R) models can be understood by a geometrical approach consisting of studying the m(r) curve on the (r,m) plane, where m≡Rf,RR/f,R and r≡−Rf,R/f with f,R≡df/dR. This allows us to classify the f(R) models into four general classes, depending on the existence of a standard matter epoch and on the final accelerated stage. The existence of a viable matter-dominated epoch prior to a late-time acceleration requires that the variable m satisfies the conditions m(r)≈+0 and dm/dr>−1 at r≈−1. For the existence of a viable late-time acceleration we require instead either (i) m=−r−1, (√3−1)/2<m≤1 and dm/dr<−1 or (ii) 0<m≤1 at r=−2. These conditions identify two regions in the (r,m) space, one for the matter era and the other for the acceleration. Only models with an m(r) curve that connects these regions and satisfies the requirements above lead to an acceptable cosmology. The models of type f(R)=αR−n and f=R+αR−n do not satisfy these conditions for any n>0 and n<−1 and are thus cosmologically unacceptable. Similar conclusions can be reached for many other examples discussed in the text. In most cases the standard matter era is replaced by a cosmic expansion with scale factor a∝t1/2. We also find that f(R) models can have a strongly phantom attractor but in this case there is no acceptable matter era.