Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
V. Summary・ We have discussed modified gravitational theories inorder to explain the current accelerated expansion ofthe universe, so-called dark energy problem.・ We have investigated the equation of state for dark energyin f(R) gravity as well as f(T) theory.w DEw DE = à 1The future crossings of the phantom divide lineare the generic feature in the existingviable f(R) gravity models.No. 34・The crossing of the phantom divide line can berealized in the combined f(T) theory.We have studied the effective equation of state for theuniverse when the finite-time future singularities occurin non-local gravity.
Future evolutions of H as functions of z >No. 23Exponential gravity modelOscillatory behavior:ñH(z=à1)H0‘f’ denotes the valueat the final stagez = à 1.:Present value of theHubble parameter
- Page 1: Equation of state for dark energyin
- Page 4 and 5: (1) General relativistic approach
- Page 6 and 7: m à:mMMDistanceestimator::Apparent
- Page 9 and 10: Canonical scalar field >⎧S þ =
- Page 11 and 12: ・In the flat FLRW background, gra
- Page 13 and 14: Models of f(R) gravity (examples) >
- Page 15 and 16: Data fitting of w(z) >zw(z)=w 0 + w
- Page 17 and 18: w DEw DE = à 1< Cosmological evolu
- Page 19 and 20: II. Future crossing of the phantom
- Page 21 and 22: Future evolutions of 1+w DE as func
- Page 23 and 24: III. Equation of state for dark ene
- Page 25 and 26: Combined f(T) theory >No. 25u(> 0):
- Page 27 and 28: A. Non-local gravity< Action >g =de
- Page 29 and 30: ・In the flat FLRW space-time, we
- Page 31 and 32: ・The finite-time future singulari
- Page 33: ・We estimate the present valueof
- 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 80 and 81: Data fitting of w(z) (3) >No. B-7Fr
- Page 82 and 83: Bekenstein-Hawking entropy on the a
Future evolutions of H as functions of z >No. 23Exponential gravity modelOscillatory behavior:ñH(z=à1)H0‘f’ denotes the valueat the final stagez = à 1.:Present value of theHubble parameter
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