The Young Universe von Richard Taillet

<p><i>The Young Universe</i> presents four major physical and astrophysical themes related to these extreme phases of the primordial universe. In particular, it presents the physics of the primordial plasma and the concepts of quantum and particle physics necessary to describe this extreme state.</p><p>It discusses the cosmological background radiation and explores inflation, an extremely rapid expansion phase that is believed to have occurred very early in cosmological history and to have shaped our present universe. The book also provides a synthesis of the dark matter problem.</p>

Richard Taillet is an astrophysicist at the LAPTh in Annecy, France and Professor at the Université Savoie Mont Blanc, Chambéry, France.

Chapter 1 A Thermal History of the Universe and Primordial Nucleosynthesis1Pierre SALATI1.1 A quick overview 21.1.1 A useful refresher of the FriedmannLemaître model 21.1.2 The major events of the Big Bang 51.2 Gamows ylem 101.2.1 Introductory remarks 101.2.2 Numerical density 141.2.3 Energy density and pressure 161.2.4 Entropy density 171.2.5 Effective degrees of freedom of the ylem 191.2.6 Numerical developments 201.3 Cooling kinetics 221.3.1 Planck mass 221.3.2 Relation between scale factor and temperature 241.3.3 Relation between cosmic time and temperature 251.4 Thermal decoupling of neutrinos 291.4.1 The concept of cross-section 291.4.2 Thermal equilibrium breaking 331.4.3 The neutrinic fossil radiation 361.4.4 The Cowsik and McClelland limit 381.5 Primordial nucleosynthesis 411.5.1 Transmutation between protons and neutrons 421.5.2 Breaking of the neutronproton equilibrium 461.5.3 The formation of deuterium 511.5.4 The cooking of light elements 541.6 Chemical decoupling of heavy particles 601.6.1 Evolutionary equation 621.6.2 Approximate solution 631.6.3 Relic density 671.6.4 The Lee and Weinberg limit 691.7 Dissipation of the primordial fog 711.7.1 Sahas equilibrium 721.7.2 Photoionization and recombination of neutral hydrogen 751.7.3 Lyman-alpha line and atomic resonance 781.7.4 The three-level atom model 821.7.5 Recombination of the primordial plasma and residual ionization 851.8 References 89Chapter 2 Cosmological Microwave Background93Julien LESGOURGUES2.1 Introduction 932.1.1 Last scattering surface 932.1.2 CMB anisotropies 942.1.3 Conventions 962.2 Revisiting the Thomson scattering 962.2.1 Scattering rate 962.2.2 Optical depth 972.2.3 Visibility function 982.2.4 Diffusion length 992.3 Linear cosmological perturbations 1002.3.1 Why linear perturbations? 1002.3.2 Classification of perturbations 1002.3.3 Comoving Fourier space 1032.3.4 Linearized Einstein equation 1052.3.5 Species present in the standard cosmological model 1062.3.6 General equations of motion 1072.4 Formal description of temperature anisotropies 1082.4.1 Photon propagation 1082.4.2 Temperature anisotropy in a given direction 1132.5 Stochastic theory of cosmological perturbations 1172.5.1 Initial conditions 1182.5.2 Power spectrum and transfer functions 1232.5.3 Spectrum of temperature anisotropies 1272.6 Physics of temperature anisotropies 1312.6.1 Line-of-sight integral in Fourier space 1312.6.2 Perturbation evolution 1372.6.3 Contributions to the temperature spectrum 1422.6.4 Dependency on cosmological parameters 1502.7 Other contributions and observables 1562.7.1 Overview of CMB polarization 1562.7.2 CMB gravitational lensing 1592.7.3 Overview of the role of gravitational waves 1602.7.4 Astrophysical foreground 1612.7.5 Spectral distortions 1622.8 CBM observations 1622.8.1 Current observations 1622.8.2 Future observations 1692.9 References 170Chapter 3 Cosmological Inflation173Sébastien RENAUX-PETEL3.1 Overview 1733.2 Introduction 1753.2.1 Shortcomings of the Hot Big Bang model 1753.2.2 The mechanism of inflation 1793.3 Single-field slow-roll inflation 1843.3.1 Homogeneous dynamics 1843.3.2 Dynamics of fluctuations 1893.4 The physics of inflation beyond toy models 2153.4.1 Ultraviolet sensitivity 2163.4.2 Multifield effects 2223.5 Primordial non-Gaussianities 2363.5.1 Overview 2363.5.2 Determining primordial non-Gaussianities 2393.5.3 Non-Gaussian shapes 2433.6 Conclusion 2533.7 References 255Chapter 4 Dark Matter259Richard TAILLET4.1 Introduction 2594.1.1 Subject presentation 2594.1.2 Brief historical overview 2604.1.3 Current interest in the subject 2614.1.4 Warning 2614.1.5 Summary of evidence in favor of dark matter 2614.2 At the galaxy scale 2624.2.1 Introduction 2624.2.2 Spiral galaxy rotation curves 2634.2.3 Velocity dispersion in elliptical galaxies 2664.2.4 Application to the gravitational case 2694.2.5 Dwarf spheroid galaxies 2714.2.6 Our Galaxy 2724.2.7 Density profiles 2744.3 At the galaxy cluster scale 2764.3.1 Velocity dispersion 2764.3.2 Hot gas X-ray 2764.3.3 Gravitational lenses 2774.3.4 The SunyaevZeldovich effect 2784.4 Cosmology 2794.4.1 Geometry of the universe 2794.4.2 Primordial nucleosynthesis 2824.4.3 The formation of large structures 2824.5 The nature of dark matter 2914.5.1 Baryonic candidates 2914.5.2 Gravity microlensing 2944.5.3 Particles 3034.6 Detection 3154.6.1 Direct detection 3154.6.2 Indirect detection 3214.6.3 Clumps 3264.7 Modified dynamics and gravity 3294.7.1 MOND theory 3294.7.2 The Bullet Cluster 3304.8 Conclusion 3324.9 References 332List of Authors 335Index 337

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