Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
f(R) gravity >No. 10Sf(R)2ô 2f(R) gravityf(R)=R: General Relativity[Nojiri and Odintsov, Phys. Rept. 505, 59 (2011) [arXiv:1011.0544 [gr-qc]];Int. J. Geom. Meth. Mod. Phys. 4, 115 (2007) [arXiv:hep-th/0601213]][Capozziello and Francaviglia, Gen. Rel. Grav. 40, 357 (2008)][Sotiriou and Faraoni, Rev. Mod. Phys. 82, 451 (2010)][De Felice and Tsujikawa, Living Rev. Rel. 13, 3 (2010)]< Gravitational field equation >f 0 (R)=df(R)/dR: Covariant d'Alembertian: Covariant derivative operator
・In the flat FLRW background, gravitational field equations readú eff , p eff,: Effective energydensity andNo. 11pressure from theterm f(R) à RExample:öf(R)=R à 2(n+1)Rn[Carroll, Duvvuri, Trodden and Turner,Phys. Rev. D 70, 043528 (2004)]・ö : Mass scale, n : Constant Second term becomea ∝ t q (2n+1)(n+1), q =important as R decreases.n+2If q>1 , accelerated2(n+2)w eff = à 1+ 3(2n+1)(n+1) expansion can be realized.(For n =1, q =2 and w eff = à 2/3 .)
- Page 1: Equation of state for dark energyin
- Page 4 and 5: (1) General relativistic approach
- Page 6 and 7: m à:mMMDistanceestimator::Apparent
- Page 9: Canonical scalar field >⎧S þ =
- Page 13 and 14: Models of f(R) gravity (examples) >
- Page 15 and 16: Data fitting of w(z) >zw(z)=w 0 + w
- Page 17 and 18: w DEw DE = à 1< Cosmological evolu
- Page 19 and 20: II. Future crossing of the phantom
- Page 21 and 22: Future evolutions of 1+w DE as func
- Page 23 and 24: III. Equation of state for dark ene
- Page 25 and 26: Combined f(T) theory >No. 25u(> 0):
- Page 27 and 28: A. Non-local gravity< Action >g =de
- Page 29 and 30: ・In the flat FLRW space-time, we
- Page 31 and 32: ・The finite-time future singulari
- Page 33 and 34: ・We estimate the present valueof
- Page 35 and 36: Future evolutions of H as functions
- Page 37 and 38: ・・In the future ( ), the crossi
- Page 39 and 40: Conditions for the viability of f(R
- Page 41 and 42: We solve Equations (1) and (2) by i
- Page 43 and 44: Equation of state for (the componen
- Page 45 and 46: No. 32We consider only non-relativi
- Page 47 and 48: Gravitational field equations in th
- Page 49: ・By using and ,No. 39・We take a
- Page 52 and 53: Future crossing of the phantom divi
- Page 54 and 55: B. Relations between the model para
- Page 56 and 57: IV. Effective equation of state for
- Page 58 and 59: (2) Extension of gravitational theo
・In the flat FLRW background, gravitational field equations readú eff , p eff,: Effective energydensity andNo. 11pressure from theterm f(R) à RExample:öf(R)=R à 2(n+1)Rn[Carroll, Duvvuri, Trodden and Turner,<strong>Phys</strong>. <strong>Rev</strong>. D 70, 043528 (2004)]・ö : Mass scale, n : Constant Second term becomea ∝ t q (2n+1)(n+1), q =important as R decreases.n+2If q>1 , accelerated2(n+2)w eff = à 1+ 3(2n+1)(n+1) expansion can be realized.(For n =1, q =2 and w eff = à 2/3 .)
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