Tsujikawa, Phys. Rev. D 77, 023507 (2008)
Tsujikawa, Phys. Rev. D 77, 023507 (2008) Tsujikawa, Phys. Rev. D 77, 023507 (2008)
(1) General relativistic approach・ Cosmological constant・ Scalar fields:X matter, Quintessence, Phantom, K-essence,Tachyon. f(R)・ Fluid: Chaplygin gas(2) Extension of gravitational theory・ f(R) gravity・ Scalar-tensor theories・ Ghost condensates: Arbitrary function of the Ricci scalar[Capozziello, Cardone, Carloniand Troisi, Int. J. Mod. Phys. D12, 1969 (2003)][Carroll, Duvvuri, Trodden and Turner, Phys. Rev. D 70,043528 (2004)][Nojiri and Odintsov, Phys. Rev. D 68, 123512 (2003)]R[Arkani-Hamed, Cheng, Luty and Mukohyama,JHEP 0405, 074 (2004)]G : Gauss-Bonnet termf(G) T : torsion scalar[Dvali, Gabadadze and Porrati, Phys.Lett B 485, 208 (2000)]・ Higher-order curvature term ・ gravity・ DGP braneworld scenario・ Non-local gravity [Deser and Woodard, Phys. Rev. Lett. 99, 111301 (2007)]・ f(T) gravity[Bengochea and Ferraro, Phys. Rev. D 79, 124019 (2009)]・ Galileon gravity[Linder, Phys. Rev. D 81, 127301 (2010) [Erratum-ibid. D 82, 109902 (2010)]][Nicolis, Rattazzi and Trincherini, Phys. Rev. D 79,064036 (2009)]No. 4
Flat Friedmann-Lema tre-Robertson-Walker (FLRW)space-time >a (t)No. 5: Scale factor< Equation for a(t) with a perfect fluid >ä = àô 2 ( 1+3w)úa 6w ñ úP: Equation of state (EoS)T ö÷ =diag(ú, P, P, P)ú : Energy densityP : Pressureä > 0 : Accelerated expansionw
- Page 1: Equation of state for dark energyin
- 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 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
(1) General relativistic approach・ Cosmological constant・ Scalar fields:X matter, Quintessence, Phantom, K-essence,Tachyon. f(R)・ Fluid: Chaplygin gas(2) Extension of gravitational theory・ f(R) gravity・ Scalar-tensor theories・ Ghost condensates: Arbitrary function of the Ricci scalar[Capozziello, Cardone, Carloniand Troisi, Int. J. Mod. <strong>Phys</strong>. D12, 1969 (2003)][Carroll, Duvvuri, Trodden and Turner, <strong>Phys</strong>. <strong>Rev</strong>. D 70,043528 (2004)][Nojiri and Odintsov, <strong>Phys</strong>. <strong>Rev</strong>. D 68, 123512 (2003)]R[Arkani-Hamed, Cheng, Luty and Mukohyama,JHEP 0405, 074 (2004)]G : Gauss-Bonnet termf(G) T : torsion scalar[Dvali, Gabadadze and Porrati, <strong>Phys</strong>.Lett B 485, 208 (2000)]・ Higher-order curvature term ・ gravity・ DGP braneworld scenario・ Non-local gravity [Deser and Woodard, <strong>Phys</strong>. <strong>Rev</strong>. Lett. 99, 111301 (2007)]・ f(T) gravity[Bengochea and Ferraro, <strong>Phys</strong>. <strong>Rev</strong>. D 79, 124019 (2009)]・ Galileon gravity[Linder, <strong>Phys</strong>. <strong>Rev</strong>. D 81, 127301 (2010) [Erratum-ibid. D 82, 109902 (2010)]][Nicolis, Rattazzi and Trincherini, <strong>Phys</strong>. <strong>Rev</strong>. D 79,064036 (2009)]No. 4
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