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10000 1000 100 10 1 0.001 0.01 k/h M pc −1 0.1 1 Perturbationevolution 10 1e-06 1e-05 0.0001 0.001 0.01 CDM density Figure6.4: The evolution of allCDM density perturbation modes is shown. The axes arethe sameas infig. 6.3. The oscillations, which arepresent at recombination (neither super horizon nor dampedaway)causeanimprintin theCDMandthus occurin thepower spectrum ofthe matter density distributionofthe universe. a 0.1 1 38 6.3 The Evolution of Perturbations
6 The cmbeasy program 39 1e+20 1e+15 1e+10 100000 1 1e-05 Dgγ Dg b Dgc Densityperturbations 1e-10 1e-08 1e-07 1e-06 1e-05 0.0001 0.001 0.01 0.1 1 1 0.01 0.0001 1e-06 1e-08 1e-10 1e-07 1e-06 1e-05 0.0001 0.001 0.01 0.1 1 a Potential a Ψ Φ 1e+20 1e+15 1e+10 100000 1 1e-05 1e-10 Vγ Vb Vc Velocityperturbations 1e-15 1e-08 1e-07 1e-06 1e-05 0.0001 0.001 0.01 0.1 1 1e+06 10000 100 1 0.01 0.0001 1e-06 1e-08 1e-10 a Zoom of Perturbations Vγ Dgγ Ψ Φ Vb Vc Dg b Dgc 0.01 0.1 Figure6.5: Breakdownofperturbation evolution The perturbation has a momentum scale of k=428.0h M pc −1 , corresponding to an extension ofλ=14.7h −1 kpc. The plots are of the same type as in figure 6.2 except thezoom-plot inthe lower-right. Note that the absolutevalue ofthe perturbation variablesisplotted because they changetheir signs(even CDM),yielding toafrayed plot. Obviously thephoton velocity V γ grows,whichcauses a successivedragof theother variables: First D gγ, thenΨ&Φ, V b, V c, D g b and D gc grownearly unlimited. It israther unphysicalthat V γ isgrowingafterrecombination. Maybethe weakcouplingapproximationofbaryons andphotons breaks downat highk. a
Page 1: Structure Formation in the Universe
Page 5 and 6: Contents 1 Introduction 5 2 Equival
Page 7: 1 Introduction At high energies the
Page 10 and 11: 1. Spacetime is endowed with a symm
Page 12 and 13: One can see, that the differentials
Page 14 and 15: 3.5 The Connection 3.5.1 Geometric
Page 16 and 17: 3.7 Torsion andCurvature The Torsio
Page 18 and 19: It is an important property that th
Page 20 and 21: One concludes that the space of con
Page 22 and 23: 4.4 ScalefactorandRedshift For simp
Page 24 and 25: 4.6 The FriedmannEquations Summing
Page 26 and 27: 4.7.1 Values ofthedensityparameters
Page 28 and 29: 4.8 Inflation Inflation, first intr
Page 30 and 31: 10 1 1e+12 1e+10 1e+08 1e+06 10000
Page 32 and 33: With this metric, the velocity pert
Page 34 and 35: 5.2 InitialConditions According to
Page 36 and 37: CDM density perturbation today. Unf
Page 38 and 39: 100000 10000 1000 100 10 1 Dgγ Dg
Page 42 and 43: timesteps 1e+09 1e+08 1e+07 1e+06 1
Page 44 and 45: Performing on the other hand a Four
Page 46 and 47: α(Ω b,Ω c)=0.8873 andβ(Ω b,
Page 49 and 50: 8 The search for a cutoff Now the q
Page 51 and 52: 8 The searchfor a cutoff 49 ∆ 2 (
Page 53 and 54: Figure8.4: Luminosityfunction ofgal
Page 55: λ0/m Inflation aRH Radiation domin
Page 59 and 60: Descriptions Acbar: Arcminute Cosmo
Page 61 and 62: Bibliography [1] Clifford M. Will,
Page 63: [48] Simon P. Driver, Paul D. Allen

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