Tsujikawa, Phys. Rev. D 77, 023507 (2008)

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Canonical scalar field >⎧S þ = ⎭ d 4 √x à gâà 1 g ö÷ ã∂ 2 ö þ∂ ÷ þ à V(þ)No. 9g =det(g ö÷ )V(þ)þ : Scalar field: Potential of þ・ For a homogeneous scalar field þ = þ(t) :ú þ = 2 1 þ ç 2 + V(þ), P þ = 2 1 þ ç 2 à V(þ)Pw þ = þ þ= ç 2 à2V(þ)úþ þ ç 2 +2V(þ)þ ç 2 ü V(þ)w þ ùà1If , .Accelerated expansion can be realized.
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 10 and 11: f(R) gravity >No. 10Sf(R)2ô 2f(R)
Page 12 and 13: Conditions for the viability of f(R
Page 14 and 15: Crossing of the phantom divide >・
Page 16 and 17: ・ It is known that in several via
Page 18 and 19: We explicitly demonstrate that the
Page 20 and 21: Gravitational field equations in th
Page 22 and 23: Hu-Sawicki modelStarobinsky’s mod
Page 24 and 25: No. 24*・: Gravitational field equ
Page 26 and 27: IV. Effective equation of state for
Page 28 and 29: Gravitational field equation >No. 2
Page 30 and 31: ・It is known that the finite-time
Page 32 and 33: We examine the asymptotic behavior
Page 34 and 35: V. Summary・ We have discussed mod
Page 36 and 37: Hu-Sawicki modelStarobinsky’s mod
Page 38 and 39: ・・Hw eff = à 1 à 32H ç2(a)(b
Page 40 and 41: Flat Friedmann-Lema tre-Robertson-W
Page 42 and 43: Combining Equations (3) and (4), we
Page 44 and 45: No. 31: Gravitational field equatio
Page 46 and 47: Gravitational field equation >No. 3
Page 48 and 49: A. Finite-time future singularities
Page 51 and 52: Other model >・No. 18Appleby-Batty
Page 53 and 54: ・・We examine the behavior of ea
Page 55 and 56: B. Estimation of the current value
Page 57 and 58: (1) General relativistic approach
Page 59 and 60:
・ DGP braneworld scenario[Dvali,
Page 61 and 62:
(4) Solar system constraintsf(R) gr
Page 63 and 64:
Ω DE Ω m Ω rNo. 19< Cosmological
Page 65 and 66:
Conclusions of Sec. III >・・・W
Page 67 and 68:
Continuity equation:No. 44・ We de
Page 69 and 70:
Continuity equation:No. 39・ We de
Page 71 and 72:
does not cross the phantom divide l
Page 73 and 74:
Cosmological evolutions of Ω DE ,
Page 75 and 76:
Backup Slides A
Page 77 and 78:
(5) Existence of a matter-dominated
Page 79 and 80:
Data fitting of w(z)No. 22(2) >From
Page 81 and 82:
・For most observational probes (e
Page 83 and 84:
Future evolutions of S as functions
Page 85 and 86:
S ∝ H à2H・ Since , the oscilla
Page 87 and 88:
No. 16< (b). Logarithmic f(T) theor
Page 89 and 90:
(c). Combined f(T) theory >No. 16
Page 91 and 92:
Combined f(T) theory >No. 48u : Con
Page 93 and 94:
C. Relations between the model para
Page 95 and 96:
Appendix A
Page 97 and 98:
S = 4GA:Bekenstein-Hawking horizon
Page 99 and 100:
Remarks >(a) The qualitative result
Page 101 and 102:
Numerical results >Models of (i), (
Page 103 and 104:
No. A-20・Models of (i), (ii), (ii
Page 105 and 106:
・Our results are not sensitive to
Page 107 and 108:
Second law of thermodynamics in equ
Page 109 and 110:
Backup Slides B
Page 111 and 112:
Baryon acoustic oscillation (BAO) >
Page 113 and 114:
・No. BS-B4In the flat FLRW backgr
Page 115 and 116:
(7) Free of curvature singularities
Page 117 and 118:
We reconstruct an explicit model of
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Tsujikawa, Phys. Rev. D 77, 023507 (2008)

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