Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Appendix B
(7) Free of curvature singularities・ Existence of relativistic stars[Frolov, Phys. Rev. Lett. 101, 061103 (2008)]No. B-2[Kobayashi and Maeda, Phys. Rev. D 78, 064019 (2008)][Kobayashi and Maeda, Phys. Rev. D 79, 024009 (2009)]< Model with satisfying the condition (7) >F MJWQ (R)ë>0, R ã > 0 : Constants[Miranda, Joras, Waga and Quartin, Phys. Rev. Lett. 102, 221101 (2009)]Cf. [de la Cruz-Dombriz, Dobado and Maroto, Phys. Rev. Lett. 103, 179001 (2009)]
- 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 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 116 and 117: Recent work >No. B-3[Martinelli, Me
- Page 118: (5) Existence of a matter-dominated
(7) Free of curvature singularities・ Existence of relativistic stars[Frolov, <strong>Phys</strong>. <strong>Rev</strong>. Lett. 101, 061103 (<strong>2008</strong>)]No. B-2[Kobayashi and Maeda, <strong>Phys</strong>. <strong>Rev</strong>. D 78, 064019 (<strong>2008</strong>)][Kobayashi and Maeda, <strong>Phys</strong>. <strong>Rev</strong>. D 79, 024009 (2009)]< Model with satisfying the condition (7) >F MJWQ (R)ë>0, R ã > 0 : Constants[Miranda, Joras, Waga and Quartin, <strong>Phys</strong>. <strong>Rev</strong>. Lett. 102, 221101 (2009)]Cf. [de la Cruz-Dombriz, Dobado and Maroto, <strong>Phys</strong>. <strong>Rev</strong>. Lett. 103, 179001 (2009)]
Change language