Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Other models >No. A-10・Appleby-Battye model [Appleby and Battye, Phys. Lett. B 654, 7 (2007)]f AB (R)= R 2+ 1 2b1log [ cosh(b 1 R) à tanh(b 2 ) sinh(b 1 R) ]b 1 (> 0), b 2: Constant parametersCf. Power-law modelf(R)=R à öR vö(> 0): Constant parameter[Amendola, Gannouji, Polarski and Tsujikawa,Phys. Rev. D 75, 083504 (2007)][Li and Barrow, Phys. Rev. D 75, 084010 (2007)]0
S = 4GA:Bekenstein-Hawking horizon entropyin the Einstein gravityNo. A-11・・:Wald entropy in modified gravitytheories: Area of the apparent horizonWald introduced a horizon entropy associated with aNoether charge in the context of modified gravity theories.This is equivalent to S ê = A/(4G eff ).S êThe Wald entropy is a local quantity defined in terms ofquantities on the bifurcate Killing horizon.More specifically, it depends on the variation of theLagrangian density of gravitational theories withrespect to the Riemann tensor.G eff = G/FS ê: Effective gravitational coupling
- 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
- 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 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 104 and 105: No. A-21・・ By examining the cos
- 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
S = 4GA:Bekenstein-Hawking horizon entropyin the Einstein gravityNo. A-11・・:Wald entropy in modified gravitytheories: Area of the apparent horizonWald introduced a horizon entropy associated with aNoether charge in the context of modified gravity theories.This is equivalent to S ê = A/(4G eff ).S êThe Wald entropy is a local quantity defined in terms ofquantities on the bifurcate Killing horizon.More specifically, it depends on the variation of theLagrangian density of gravitational theories withrespect to the Riemann tensor.G eff = G/FS ê: Effective gravitational coupling
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