Nikolaos Tetradis
Nikolaos Tetradis Nikolaos Tetradis
Hierarchy of scalesFor subhorizon perturbations with momenta k ≫ H = ȧ/a, thelinear analysis predicts |δ⃗v| ∼ (k/H)Φ ∼ (H/k)(δρ/¯ρ).We assume the hierarchy of scales: Φ, δφ/¯φ ≪ |δ⃗v| ≪ δρ/¯ρ 1.As we are dealing with subhorizon perturbations, we assumethat the spatial derivatives of Φ, δφ, δ⃗v dominate over their timederivatives. We also assume that a spatial derivative acting on Φ,δφ or δ⃗v increases the position of that quantity in the hierarchy byone level: ⃗ ∇Φ is comparable to Hδ⃗v, while ∇ 2 Φ is comparable toH 2 δρ/¯ρ.F. Saracco, M. Pietroni, N. T., V. Pettorino, G. RobbersarXiv:0911.5396[astro-ph], Phys. Rev. D 82: 023528 (2010)N. Tetradis University of AthensThe inhomogeneity of the Universe and the cosmological model
Equations of motion for several non-relativistic speciesThe evolution of the homogeneous background is described byH 2 = 1 [ ∑a2¯ρ i + 1 ˙¯φ 2 + a 2 U(¯φ) ] ≡ 1 323 a2 ρ toti=1,2˙¯ρ i + 3H¯ρ i = − β i˙¯φ¯ρi⎛¨¯φ + 2H ˙¯φ = − a2⎝ dUdφ (¯φ) − ∑with ρ tot ≡ ∑ i¯ρ i + ˙¯φ2 /(2a 2 ) + U(¯φ).i=1,2β i ¯ρ i⎞⎠,For the CDM we set β 1 = β, while for BM, because of strongobservational constraints , we set β 2 = 0.N. Tetradis University of AthensThe inhomogeneity of the Universe and the cosmological model
- Page 2: Figure: 2MASS Galaxy Catalog (more
- Page 5 and 6: Standard frameworkBasic assumptions
- Page 7 and 8: Our approachAll the information abo
- Page 9 and 10: Luminosity distance and redshiftCon
- Page 11 and 12: Observer and source at random posit
- Page 13 and 14: A similar problem in brane cosmolog
- Page 15 and 16: Basic relationsAction∫S =d 4 x
- Page 17 and 18: Static spherically symmetric config
- Page 19 and 20: Compact astrophysical objects made
- Page 21 and 22: Astrophysical objects made of neutr
- Page 23 and 24: Sloan Digital Sky Survey (2005)Figu
- Page 25: Ansatz for the metricds 2 = a 2 (τ
- Page 29 and 30: Time renormalization group (Pietron
- Page 31 and 32: The non-zero components of the effe
- Page 33 and 34: In this way we obtain∂ η P ab (k
- Page 35 and 36: 7Density-Density Power Spectra at z
- Page 37 and 38: 1.7BAO Power Spectra at z=0 (β=0.1
- Page 39 and 40: wz0.40.60.81.01.41.62 4 6 8 10 zFig
- Page 41 and 42: ∆k i k i,lin0.0150.0100.005(2)0.0
- Page 43 and 44: Growing neutrino quintessence i , q
- Page 45: ConclusionsThe inhomogeneities in t
Equations of motion for several non-relativistic speciesThe evolution of the homogeneous background is described byH 2 = 1 [ ∑a2¯ρ i + 1 ˙¯φ 2 + a 2 U(¯φ) ] ≡ 1 323 a2 ρ toti=1,2˙¯ρ i + 3H¯ρ i = − β i˙¯φ¯ρi⎛¨¯φ + 2H ˙¯φ = − a2⎝ dUdφ (¯φ) − ∑with ρ tot ≡ ∑ i¯ρ i + ˙¯φ2 /(2a 2 ) + U(¯φ).i=1,2β i ¯ρ i⎞⎠,For the CDM we set β 1 = β, while for BM, because of strongobservational constraints , we set β 2 = 0.N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
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