Inflationary cosmology has been developed over the last 20 years to remedy serious
shortcomings in the standard hot big bang model of the universe.Taking an original
approach, this textbook explains the basis of modern cosmology and shows where
the theoretical results come from.
The book is divided into two parts: the first deals with the homogeneous and
isotropic model of the universe, while the second part discusses howinitial inhomogeneities
can explain the observed structure of the universe. Analytical treatments
of traditionally highly numerical topics – such as primordial nucleosynthesis, recombination
and cosmic microwave background anisotropy – are provided, and
inflation and quantum cosmological perturbation theory are covered in great detail.
The reader is brought to the frontiers of current cosmological research by the
discussion of more speculative ideas.
This is an ideal textbook both for advanced students of physics and astrophysics
and for those with a particular interest in theoretical cosmology. Nearly every
formula in the book is derived from basic physical principles covered in undergraduate
courses. Each chapter includes all necessary background material and no prior
knowledge of general relativity and quantum field theory is assumed.
Viatcheslav Mukhanov is Professor of Physics and Head of the Astroparticle
Physics and Cosmology Group at the Department of Physics, Ludwig-
Maximilians-Universit¨at M¨unchen, Germany. Following his Ph.D. at the Moscow
Physical-Technical Institute, he conducted research at the Institute for Nuclear
Research, Moscow, between 1982 and 1991. From 1992, he was a lecturer at
Eidgen¨ossische Technische Hochschule (ETH) in Z¨urich, Switzerland, until his appointment
atLMUin 1997. His current research interests include cosmic microwave
background fluctuations, inflationary models, string cosmology, the cosmological
constant problem, dark energy, quantum and classical black holes, and quantum
cosmology. He also serves on the editorial boards of leading research journals in
these areas.
In 1980–81, Professor Mukhanov and G. Chibisov discovered that quantum
fluctuations could be responsible for the large-scale structure of the universe. They
calculated the spectrum of fluctuations in a model with a quasi-exponential stage
of expansion, later known as inflation. The predicted perturbation spectrum is in
very good agreement with measurements of the cosmic microwave background
fluctuations. Subsequently, Professor Mukhanov developed the quantum theory
of cosmological perturbations for calculating perturbations in generic inflationary
models. In 1988, he was awarded the Gold Medal of the Academy of Sciences of
the USSR for his work on this theory.
Contents
Foreword by Professor Andrei Linde page xi
Preface xiv
Acknowledgements xvi
Units and conventions xvii
PartI Homogeneous isotropic universe 1
1 Kinematics and dynamics of an expanding universe 3
1.1 Hubble law 4
1.2 Dynamics of dust in Newtonian cosmology 8
1.2.1 Continuity equation 9
1.2.2 Acceleration equation 9
1.2.3 Newtonian solutions 10
1.3 From Newtonian to relativistic cosmology 13
1.3.1 Geometry of an homogeneous, isotropic space 14
1.3.2 The Einstein equations and cosmic evolution 19
1.3.3 Friedmann equations 22
1.3.4 Conformal time and relativistic solutions 24
1.3.5 Milne universe 27
1.3.6 De Sitter universe 29
2 Propagation of light and horizons 37
2.1 Light geodesics 37
2.2 Horizons 38
2.3 Conformal diagrams 41
2.4 Redshift 55
2.4.1 Redshift as a measure of time and distance 58
2.5 Kinematic tests 60
2.5.1 Angular diameter–redshift relation 60
2.5.2 Luminosity–redshift relation 64
2.5.3 Number counts 66
2.5.4 Redshift evolution 67
3 The hot universe 69
3.1 The composition of the universe 69
3.2 Brief thermal history 72
3.3 Rudiments of thermodynamics 74
3.3.1 Maximal entropy state, thermal spectrum,
conservation laws and chemical potentials 75
3.3.2 Energy density, pressure and the equation of state 79
3.3.3 Calculating integrals 82
3.3.4 Ultra-relativistic particles 85
3.3.5 Nonrelativistic particles 88
3.4 Lepton era 89
3.4.1 Chemical potentials 92
3.4.2 Neutrino decoupling and electron–positron annihilation 94
3.5 Nucleosynthesis 97
3.5.1 Freeze-out of neutrons 98
3.5.2 “Deuterium bottleneck” 104
3.5.3 Helium-4 108
3.5.4 Deuterium 112
3.5.5 The other light elements 117
3.6 Recombination 120
3.6.1 Helium recombination 120
3.6.2 Hydrogen recombination: equilibrium consideration 122
3.6.3 Hydrogen recombination: the kinetic approach 123
4 The very early universe 131
4.1 Basics 132
4.1.1 Local gauge invariance 133
4.1.2 Non-Abelian gauge theories 135
4.2 Quantum chromodynamics and quark–gluon plasma 138
4.2.1 Running coupling constant and asymptotic freedom 141
4.2.2 Cosmological quark–gluon phase transition 146
4.3 Electroweak theory 150
4.3.1 Fermion content 151
4.3.2 “Spontaneous breaking” of U(1) symmetry 153
4.3.3 Gauge bosons 154
4.3.4 Fermion interactions 158
4.3.5 Fermion masses 160
4.3.6 CP violation 162
4.4 “Symmetry restoration” and phase transitions 165
4.4.1 Effective potential 165
4.4.2 U(1) model 170
4.4.3 Symmetry restoration at high temperature 173
4.4.4 Phase transitions 174
4.4.5 Electroweak phase transition 176
4.5 Instantons, sphalerons and the early universe 180
4.5.1 Particle escape from a potential well 180
4.5.2 Decay of the metastable vacuum 184
4.5.3 The vacuum structure of gauge theories 190
4.5.4 Chiral anomaly and nonconservation of the
fermion number 196
4.6 Beyond the Standard Model 199
4.6.1 Dark matter candidates 203
4.6.2 Baryogenesis 210
4.6.3 Topological defects 216
5 Inflation I: homogeneous limit 226
5.1 Problem of initial conditions 226
5.2 Inflation: main idea 229
5.3 How can gravity become “repulsive”? 233
5.4 How to realize the equation of state p ≈ −ε 235
5.4.1 Simple example: V = 12
m2ϕ2. 236
5.4.2 General potential: slow-roll approximation 241
5.5 Preheating and reheating 243
5.5.1 Elementary theory 244
5.5.2 Narrow resonance 245
5.5.3 Broad resonance 249
5.5.4 Implications 255
5.6 “Menu” of scenarios 256
Part II Inhomogeneous universe 263
6 Gravitational instability in Newtonian theory 265
6.1 Basic equations 266
6.2 Jeans theory 267
6.2.1 Adiabatic perturbations 269
6.2.2 Vector perturbations 270
6.2.3 Entropy perturbations 270
6.3 Instability in an expanding universe 271
6.3.1 Adiabatic perturbations 273
6.3.2 Vector perturbations 275
6.3.3 Self-similar solution 275
6.3.4 Cold matter in the presence of radiation or dark energy 276
6.4 Beyond linear approximation 279
6.4.1 Tolman solution 281
6.4.2 Zel’dovich solution 283
6.4.3 Cosmic web 286
7 Gravitational instability in General Relativity 289
7.1 Perturbations and gauge-invariant variables 290
7.1.1 Classification of perturbations 291
7.1.2 Gauge transformations and gauge-invariant variables 292
7.1.3 Coordinate systems 295
7.2 Equations for cosmological perturbations 297
7.3 Hydrodynamical perturbations 299
7.3.1 Scalar perturbations 299
7.3.2 Vector and tensor perturbations 309
7.4 Baryon–radiation plasma and cold dark matter 310
7.4.1 Equations 311
7.4.2 Evolution of perturbations and transfer functions 314
8 Inflation II: origin of the primordial inhomogeneities 322
8.1 Characterizing perturbations 323
8.2 Perturbations on inflation (slow-roll approximation) 325
8.2.1 Inside the Hubble scale 327
8.2.2 The spectrum of generated perturbations 329
8.2.3 Why do we need inflation? 332
8.3 Quantum cosmological perturbations 334
8.3.1 Equations 335
8.3.2 Classical solutions 337
8.3.3 Quantizing perturbations 340
8.4 Gravitational waves from inflation 348
8.5 Self-reproduction of the universe 352
8.6 Inflation as a theory with predictive power 354
9 Cosmic microwave background anisotropies 356
9.1 Basics 357
9.2 Sachs–Wolfe effect 360
9.3 Initial conditions 363
9.4 Correlation function and multipoles 365
9.5 Anisotropies on large angular scales 367
9.6 Delayed recombination and the finite thickness effect 369
9.7 Anisotropies on small angular scales 374
9.7.1 Transfer functions 374
9.7.2 Multipole moments 377
9.7.3 Parameters 379
9.7.4 Calculating the spectrum 382
9.8 Determining cosmic parameters 385
9.9 Gravitational waves 391
9.10 Polarization of the cosmic microwave background 395
9.10.1 Polarization tensor 396
9.10.2 Thomson scattering and polarization 398
9.10.3 Delayed recombination and polarization 400
9.10.4 E and B polarization modes and correlation functions 402
9.11 Reionization 407
Bibliography 410
Expanding universe (Chapters 1 and 2) 410
Hot universe and nucleosynthesis (Chapter 3) 411
Particle physics and early universe (Chapter 4) 412
Inflation (Chapters 5 and 8) 414
Gravitational instability (Chapters 6 and 7) 416
CMB fluctuations (Chapter 9) 417
Index 419
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