商品簡介
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 galaxies. Today, the Sloan Digital Sky Survey and the Two Degree Field between them have recorded the 3D positions of half a million galaxies.現代觀測技術正迅速革新我們對宇宙物理圖像的認識。本書系統地介紹了現代宇宙學的最新進展。從平坦均勻的宇宙（可以用弗裡德曼―羅伯遜―沃克度規描述）開始，講解了暗能量的處理過程，宇宙大爆炸的核合成，重組和暗物質，然後介紹了對平坦均勻宇宙的擾動：宇宙的演化和愛因斯坦―玻爾茲曼方程組，原始膨脹和現代宇宙的形成，以及觀測結果如宇宙微波背景的各向異性，紅移扭曲和弱透鏡化現象等。本書對宇宙微波背景的聲學峰結構，以及用來探測原始引力波的偏振的E/B分解都有較詳細的討論，還包含了一個長的章節專門介紹對日益龐大的宇宙觀測數據進行現代分析的技術。每章後都附有該章總結和相關文獻。通過學習，讀者可以獲得從事現代宇宙學研究必須的知識和方法。
本書的特色：（1）講解了現代宇宙學的理論基礎，處理方法和具體解釋，闡明了當前在宇宙學研究中的深刻思想；（2）涵蓋了過去十年中在宇宙學研究中的重大進展；（3）包括了上百幅很有特色的教學圖片。
作者簡介：Scott Dodelson：美國費米國家實驗室理論天體物理研究組負責人和芝加哥大學天文和天體物理學系教授。在哥倫比亞大學獲博士學位。進入費米國家實驗室和芝加哥大學前在哈佛大學做研究員。在宇宙論方面發表了七十多篇論文，其中大部分是關於宇宙的微波背景和大尺度結構。
讀者對象：理論物理、天文物理和宇宙學等專業的高年級本科生、研究生和相關專業的科研人員。
目次：標準模型及其它；平坦擴張的宇宙；遠離平衡態；波爾茲曼方程；愛因斯坦方程；初始條件；多樣性；各項異性；多樣性的探測；弱透鏡化和偏振；分析；附錄A：部分習題解答；附錄B：常數；附錄C：特殊函數；附錄D：符號；參考文獻；索引。
目次
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
Exercises
2 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
Exercises
3 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
Exercises
4 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
Exercises
5 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
Exercises
6 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 Negative 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
Exercises
7 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
Exercises
8 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 Cls
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
Exercises
9 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
Exercises
10 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
Exercises
11 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
Exercises
A Solutions to Selected Problems
B Numbers
B.1 Physical Constants
B.2 Cosmological Constants
C Special Functions
C.1 Legendre Polynomials
C.2 Spherical Harmonics
C.3 Spherical Bessel Functions
C.4 Fourier Transforms
C.5 Miscellaneous
D Symbols
Bibliography
Index
