| frequently used symbols. preface 1 introduction 1.1 this book 1.2 the universe we see 1.3 overview: from cosmological inflation to large-scale structure 1.4 notes on examples 2 the hot big bang cosmology 2.1 the expanding universe 2.2 epochs 2.3 scales 2.4 the cosmic microwave background 2.5 ingredients for a model of the universe 2.6 history of our universe examples 3 inflation 3.1 motivation for inflation 3.2 inflation in the abstract 3.3 scalar fields in cosmology 3.4 slow-roll inflation .3.5 exact solutions 3.6 hamilton-jacobi formulation of inflation 3.7 inflationary attractor 3.8 reheating: recovering the hot big bang 3.9 thermal inflation examples 4 simplest model for the origin of structure i 4.1 introduction 4.2 sequence of events 4.3 oaussian perturbations 4.4 density perturbation: newtonian treatment 4.5 the baryon density contrast: newtonian treatmem 4.6 cosmological perturbation theory 4.7 evolution equations 4.8 outside the horizon 4.9 peculiar velocity in the relativistic domain examples 5 simplest model for the origin of structure ii 5.1 from horizon entry to galaxy formation 5.2 the cosmic microwave background anisotropy 5.3 polarization 5.4 reionization examples 6 extensions to the simplest model 6.1 modifying the cold dark matter hypothesis 6.2 acdm model 6.3 open cdm model 6.4 fine tuning issues 6.5 gravitational waves 6.6 isocurvature perturbations examples 7 scalar fields and the vacuum fluctuation 7.1 classical scalar field 7.2 quantized free scalar field in flat space-time 7.3 several scalar fields 7.4 vacuum fluctuation of inflaton field 7.5 spectrum of the primordial curvature perturbation 7.6 beyond the slow-roll approximation 7.7 gravitational waves 7.8 generating an isocurvature perturbation 7.9 a multicomponent inflaton? examples 8 building and testing models of inflation 8.1 overview 8.2 form of the scalar field potential 8.3 single-field models 8.4 hybrid inflation models.. 8.5 the spectral index as a discriminator 8.6 models from extended theories of gravity 8.7 open inflation models examples 9 the cosmic microwave background 9.1 large angles and the cosmic background explorer (cobe) satellite 9.2 degree-scale observations and acoustic oscillations 9.3 aspects of microwave anisotropy satellites examples l0 galaxy motions and clustering 10.1 clustering of galaxies 10.2 galaxy velocities examples 11 the quasi-linear regime 11.1 gravitational collapse 11.2 press-schechter theory 11.3 theory of peaks 11.4 numerical simulations 11.5 applications of press-schechter theory 11.6 reionization of the universe examples 12 putting observations together 12.1 observations 12.2 critical-density models 12.3 low-density models 12.4 other options 12.5 summary 13 outlook for the future 14 advanced topic: cosmological perturbation theory 14.1 special relativity 14.2 fluid flow in special relativity 14.3 special relativity using genetic coordinates 14.4 general relativity 14.5 cosmological perturbations 14.6 evolution of the perturbations examples 15 advanced topic: diffusion and freestreaming 15.1 matter 15.2 gas dynamics in flat space-time 15.3 gas dynamics in the perturbed universe 15.4 multipoles and the boltzmann hierarchy 15.5 polarization 15.6 initial conditions and the transfer functions examples appendix: constants and parameters numerical solutions and hints for selected examples references index... |
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