现代宇宙学
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作者（英）都德尔逊 著
出版社世界图书出版公司
ISBN9787506291996
出版时间2008-10
版次1
装帧平装
开本16开
纸张胶版纸
页数440页
定价55元
上书时间2024-07-31
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基本信息
书名:现代宇宙学
定价：55元
作者:（英）都德尔逊 著
出版社：世界图书出版公司
出版日期：2008-10-01
ISBN：9787506291996
字数：
页码：440
版次：1
装帧：平装
开本：24开
商品重量：
编辑推荐
作者简介：Scott Dodelson is Head of the Theoretical Astrophysics Group at Fermilab and Associate Professor in the Department of Astronomy and Astrophysics at the University of Chicago.He received his Ph.D. from Columbia University and was a research fellow at Harvard before coming to Fermilab and Chicago. He is the author of more than seventy papers on cosmology, most of which focused on the cosmic microwave background and the large scale structure of the universe. Dodelson is a theoretical cosmologist, but has worked with several experiments, including the Sloan Digital Sky Survey and the Python and MSAM anisotropy experiments.
内容提要
There are two aspects of cosmology today that make it more alluring than ever. First, there is an enormous amount of data. To give just one example of how rapidly our knowledge of the structure of the universe is advancing, consider galaxy surveys which map the sky. In 1985, the state-of-the-art survey was the one carried out by the Center for Astrophysics; it consisted of the positions of 1100 galaes. Today, the Sloan Digital Sky Survey and the Two Degree Field between them have recorded the 3D positions of half a million galaes.
目录
1 The Standard Model and Beyond 1.1 The Expanding Universe 1.2 The Hubble Diagram 1.3 Big Bang Nucleosynthesis 1.4 The Cosmic Microwave Background 1.5 Beyond the Standard Model 1.6 Summary Exercises2 The Smooth, Expanding Universe 2.1 General Relativity 2.1.1 The Metric 2.1.2 The Geodesic Equation 2.1.3 Einstein Equations 2.2 Distances 2.3 Evolution of Energy 2.4 Cosmic Inventory 2.4.1 Photons 2.4.2 Baryons 2.4.3 Matter 2.4.4 Neutrinos 2.4.5 Dark Energy 2.4.6 Epoch of Matter-Radiation Equality 2.5 Summary Exercises3 Beyond Equilibrium 3.1 Boltzmann Equation for Annihilation 3.2 Big Bang Nucleosynthesis 3.2.1 Neutron Abundance 3.2.2 Light Element Abundances 3.3 Recombination 3.4 Dark Matter 3.5 Summary Exercises4 The Boltzmann Equations 4.1 The Boltzmann Equation for the Harmonic Oscillator 4.2 The Collisionless Boltzmann Equation for Photons 4.2.1 Zero-Order Equation 4.2.2 First-Order Equation 4.3 Collision Terms: Compton Scattering 4.4 The Boltzmann EqUation for Photons 4.5 The Boltzmann Equation for Cold Dark Matter 4.6 The Boltzmann Equation for Baryons 4.7 Summary Exercises5 Einstein Equations 5.1 The Perturbed Ricci Tensor and Scalar 5.1.1 Christoffel Symbols 5.1.2 Ricci Tensor 5.2 Two Components of the Einstein Equations 5.3 Tensor Perturbations 5.3.1 Christoffel Symbols for Tensor Perturbations 5.3.2 Ricci Tensor for Tensor Perturbations 5.3.3 Einstein Equations for Tensor Perturbations 5.4 The Decomposition Theorem 5.5 From Gauge to Gauge 5.6 Summary Exercises6 Initial Conditions 6.1 The Einstein-Boltzmann Equations at Early Times 6.2 The Horizon 6.3 Inflation 6.3.1 A Solution to the Horizon Problem 6.3.2 Pressure 6.3.3 Implementation with a Scalar Field 6.4 Gravity Wave Production 6.4.1 Quantizing the Harmonic Oscillator 6.4.2 Tensor Perturbations 6.5 Scalar Perturbations 6.5.1 Scalar Field Perturbations around a Smooth Background 6.5.2 Super-Horizon Perturbations 6.5.3 Spatially Flat Slicing 6.6 Summary and Spectral Indices Exercises7 Inhomogeneities 7.1 Prelude 7.1.1 Three Stages of Evolution 7.1.2 Method 7.2 Large Scales 7.2.1 Super-horizon Solution 7.2.2 Through Horizon Crossing 7.3 Small Scales 7.3.1 Horizon Crossing 7.3.2 Sub-horizon Evolution 7.4 Numerical Results and Fits 7.5 Growth Function 7.6 Beyond Cold Dark Matter 7.6.1 Baryons 7.6.2 Massive Neutrinos 7.6.3 Dark Energy Exercises8 Anisotropies 8.1 Overview 8.2 Large-Scale Anisotropies 8.3 Acoustic Oscillations 8.3.1 Tightly Coupled Limit of the Boltzmann Equations 8.3.2 Tightly Coupled Solutions 8.4 Diffusion Damping 8.5 Inhomogeneities to Anisotropies 8.5.1 Free Streaming 8.5.2 The Cl's 8.6 The Anisotropy Spectrum Today 8.6.1 Sachs-Wolfe Effect 8.6.2 Small Scales 8.7 Cosmological Parameters 8.7.1 Curvature 8.7.2 Degenerate Parameters 8.7.3 Distinct Imprints Exercises9 Probes of Inhomogeneities 9.1 Angular Correlations 9.2 Peculiar Velocities 9.3 Direct Measurements of Peculiar Velocities 9.4 Redshift Space Distortions 9.5 Galaxy Clusters Exercises10 Weak Lensing and Polarization 10.1 Gravitational Distortion of Images 10.2 GeodesiCs and Shear 10.3 Ellipticity as an Estimator of Shear 10.4 Weak Lensing Power Spectrum 10.5 Polarization: The Quadrupole and the Q/U DecompositioI 10.6 Polarization from a Single Plane Wave 10.7 Boltzmann Solution 10.8 Polarization Power Spectra 10.9 Detecting Gravity Waves Exercises11 Analysis 11.1 The Likelihood Function 11.1.1 Simple Example 11.1.2 CMB Likelihood 11.1.3 Galaxy Surveys 11.2 Signal Covariance Matrix 11.2.1 CMB Window Functions 11.2.2 Examples of CMB Window Functions 11.2.3 Window Functions for Galaxy Surveys 11.2.4 Summary 11.3 Estimating the Likelihood Function 11.3.1 Karhunen-Loeve Techniques 11.3.2 Optimal Quadratic Estimator 11.4 The Fisher Matrix: Limits and Applications 11.4.1 CMB 11.4.2 Galaxy Surveys 11.4.3 Forecasting 11.5 Mapmaking and Inversion 11.6 Systematics 11.6.1 Foregrounds 11.6.2 Mode Subtraction ExercisesA Solutions to Selected ProblemsB Numbers B.1 Physical Constants B.2 Cosmological ConstantsC Special Functions C.1 Legendre Polynomials C.2 Spherical Harmonics C.3 Spherical Bessel Functions C.4 Fourier Transforms C.5 MiscellaneousD SymbolsBibliographyIndex
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