Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
No. A-23
Second law of thermodynamics in equilibriumdescription >We consider the same temperature of the universeoutside and inside the apparent horizon.< Gibbs equation >No. A-17[KB and Geng, JCAP 1006, 014 (2010)]< Second law of thermodynamics >< Condition >As long as R>0 , the second law of thermodynamicscan be met in both non-phantom ( H ç < 0 , w eff > à 1 )and phantom ( H ç > 0, w eff < à 1 ) phases.Cf. [Gong, Wang and Wang, JCAP 0701, 024 (2007)][Jamil, Saridakis and Setare, Phys. Rev. D 81, 023007 (2010)]
- 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 104 and 105: No. A-21・・ By examining the cos
- 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
Second law of thermodynamics in equilibriumdescription >We consider the same temperature of the universeoutside and inside the apparent horizon.< Gibbs equation >No. A-17[KB and Geng, JCAP 1006, 014 (2010)]< Second law of thermodynamics >< Condition >As long as R>0 , the second law of thermodynamicscan be met in both non-phantom ( H ç < 0 , w eff > à 1 )and phantom ( H ç > 0, w eff < à 1 ) phases.Cf. [Gong, Wang and Wang, JCAP 0701, 024 (2007)][Jamil, Saridakis and Setare, <strong>Phys</strong>. <strong>Rev</strong>. D 81, 023007 (2010)]
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