Tsujikawa, Phys. Rev. D 77, 023507 (2008)

More documents

Recommendations

Info

・ It is known that in several viable f(R) gravity models,the crossing of the phantom divide can occur in thepast.(i) Hu-Sawicki model[Hu and Sawicki, Phys. Rev. D 76, 064004 (2007)][Martinelli, Melchiorri and Amendola, Phys. Rev. D 79, 123516 (2009)]Cf. [Nozari and Azizi, Phys. Lett. B 680, 205 (2009)](ii) Starobinsky’s model(iv) Exponential gravity modelCf.[Motohashi, Starobinsky and Yokoyama, Prog. Theor.Phys. 123, 887 (2010); Prog. Theor. Phys. 124, 541 (2010)][Linder, Phys. Rev. D 80, 123528 (2009)][KB, Geng and Lee, JCAP 1008, 021 (2010) arXiv:1005.4574 [astro-ph.CO]]Appleby-Battye modelNo. 16[Appleby, Battye and Starobinsky, JCAP 1006, 005 (2010)]
w DEw DE = à 1< Cosmological evolution of in the exponentialgravity model > From [KB, Geng and Lee, JCAP 1008, 021 (2010)].No. 17w DE (z =0)=à 0.93(< à 1/3)f E (R)=Crossingin the pastCrossing of thephantom divide
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: Data fitting of w(z) >zw(z)=w 0 + w
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 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 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 114 and 115:
Appendix B
Page 116 and 117:
Recent work >No. B-3[Martinelli, Me
Page 118:
(5) Existence of a matter-dominated
show all

Tsujikawa, Phys. Rev. D 77, 023507 (2008)

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?