Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Data fitting of w(z) (3) >No. B-7From [Zhao, Xia, Feng and Zhang,Int. J. Mod. Phys. D 16, 1229 (2007)[arXiv:astro-ph/0603621]]68%Best-fitconfidence level95% confidence level157 “gold” SN Ia data set+WMAP 3-year data+SDSSwith/without dark energy perturbations.
・For most observational probes (except the SNLSdata), a low Ω 0m prior (0.2 < Ω 0m < 0.25) leads toan increased probability (mild trend) for the crossingof the phantom divide.Ω 0m : Current density parameter of matterNo. B-6[Nesseris and L. Perivolaropoulos, JCAP 0701, 018 (2007)]
- Page 29 and 30: ・In the flat FLRW space-time, we
- Page 31 and 32: ・The finite-time future singulari
- Page 33 and 34: ・We estimate the present valueof
- Page 35 and 36: Future evolutions of H as functions
- Page 37 and 38: ・・In the future ( ), the crossi
- Page 39 and 40: Conditions for the viability of f(R
- Page 41 and 42: We solve Equations (1) and (2) by i
- Page 43 and 44: Equation of state for (the componen
- 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 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 114 and 115: Appendix B
- Page 116 and 117: Recent work >No. B-3[Martinelli, Me
- Page 118: (5) Existence of a matter-dominated
Data fitting of w(z) (3) >No. B-7From [Zhao, Xia, Feng and Zhang,Int. J. Mod. <strong>Phys</strong>. D 16, 1229 (2007)[arXiv:astro-ph/0603621]]68%Best-fitconfidence level95% confidence level157 “gold” SN Ia data set+WMAP 3-year data+SDSSwith/without dark energy perturbations.
Change language