Nikolaos Tetradis

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OutlineEffect of inhomogeneities on the average expansionA similar problem in brane cosmologyLarge-scale structures in quintessence cosmologyNon-linear spectrum of matter perturbations1 Coupled quintessence2 Variable equation of state3 Growing neutrino quintessenceConclusionsN. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
Standard frameworkBasic assumptions: Homogeneity and isotropyds 2 = −dt 2 + a 2 (t)δ ij dx i dx j(ȧ ) 2= 8πGa 3 ρäa = − 4πG (ρ + 3p)3Inhomogeneities can be treated as small perturbations of thisbackgroundIndications for the acceleration of the cosmological expansion1 Distant supernovae2 Power spectrum of the galaxy distribution3 Cosmic microwave backgroundFor acceleration: p < −ρ/3N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
Page 2: Figure: 2MASS Galaxy Catalog (more
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 and 26: Ansatz for the metricds 2 = a 2 (τ
Page 27 and 28: Equations of motion for several non
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

Nikolaos Tetradis

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