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Equation of state for dark energyin
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(1) General relativistic approach
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m à:mMMDistanceestimator::Apparent
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Canonical scalar field >⎧S þ =
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・In the flat FLRW background, gra
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Models of f(R) gravity (examples) >
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Data fitting of w(z) >zw(z)=w 0 + w
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w DEw DE = à 1< Cosmological evolu
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II. Future crossing of the phantom
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Future evolutions of 1+w DE as func
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III. Equation of state for dark ene
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Combined f(T) theory >No. 25u(> 0):
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A. Non-local gravity< Action >g =de
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・In the flat FLRW space-time, we
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・The finite-time future singulari
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・We estimate the present valueof
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Future evolutions of H as functions
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・・In the future ( ), the crossi
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Conditions for the viability of f(R
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We solve Equations (1) and (2) by i
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Equation of state for (the componen
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No. 32We consider only non-relativi
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Gravitational field equations in th
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・By using and ,No. 39・We take a
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Future crossing of the phantom divi
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B. Relations between the model para
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IV. Effective equation of state for
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- Page 60 and 61: Conditions for the viability of f(R
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- Page 64 and 65: Conclusions of Sec. II >・We have
- Page 66 and 67: Conclusions of Sec. IV >No. 64・
- Page 68 and 69: ・We assume the flat FLRW space-ti
- Page 70 and 71: No. 45p =0.001p =0.01p = à 0.1p =0
- Page 72 and 73: (b). Logarithmic f(T) theory >No. 4
- Page 74 and 75: The best-fit values >No. 42The mini
- Page 76 and 77: (4) Solar system constraintsf(R) gr
- Page 78 and 79: (4) Stability of the late-time de S
- Page 80 and 81: Data fitting of w(z) (3) >No. B-7Fr
- Page 82 and 83: Bekenstein-Hawking entropy on the a
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- Page 86 and 87: (a). Exponential f(T) theory >No. 1
- Page 88 and 89: (c). Combined f(T) theory >No. 16
- Page 90 and 91: p : Constantú Mand P M : Energy de
- Page 92 and 93: IV. Effective equation of state for
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- Page 100 and 101: Cosmological evolutions of , and in
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- Page 104 and 105: No. A-21・・ By examining the cos
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- Page 112 and 113: 5-year WMAP data on >・ For the fl
- Page 114 and 115: Appendix B
- Page 116 and 117: Recent work >No. B-3[Martinelli, Me
- Page 118: (5) Existence of a matter-dominated