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

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No. A-21・・ By examining the cosmological evolutions of andw DE as functions of the redshift z for the models, wehave found that is close to its initial valueof .y H・This is because in the higher z regime, the universe is inthe phantom phase ( w DE < à 1) and therefore, ú DE andy H increase (since ), whereas in the lower zregime, the universe is in the non-phantom (quintessence)phase ( w DE > à 1 ) and hence they decrease.Consequently, the above two effects cancel out.
・Our results are not sensitive to the initial values ofand .No. A-22z 0・The initial condition ofisdue to that the f(R) gravity models at z = z 0 should bevery close to the ΛCDM model, in which.
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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
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
Page 60 and 61: Conditions for the viability of f(R
Page 62 and 63: (5) Existence of a matter-dominated
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
Page 84 and 85: Hu-Sawicki modelStarobinsky’s mod
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
Page 94 and 95: ・It is known that the finite-time
Page 96 and 97: Other models >No. A-10・Appleby-Ba
Page 98 and 99: w effNo. A-13< Cosmological evoluti
Page 100 and 101: Cosmological evolutions of , and in
Page 102 and 103: Initial conditions >Models of (i),
Page 106 and 107: No. A-23
Page 108 and 109: Second law of thermodynamics >[KB a
Page 110 and 111: Residuals for the best fit to a fla
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
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Tsujikawa, Phys. Rev. D 77, 023507 (2008)

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