現(xiàn)代宇宙學

前言

The Men of the Great Assembly had three sayings: "Be patient before reachinga decision; Enable many students to stand on their own; Make a fence around yourteaching."Ethics of the Fathers 1:1There 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 rapidlyour knowledge of the structure of the universe is advancing, consider galaxy surveyswhich map the sky. In 1985, the state-of-the-art survey was the one carried out bythe Center for Astrophysics; it consisted of the positions of 1100 galaxies. Today, theSloan Digital Sky Survey and the Two Degree Field between them have recordedthe 3D positions of half a million galaxies.The other aspect of modern cosmology which distinguishes it from previousefforts to understand the universe is that we have developed a consistent theoret-ical framework which agrees quantitatively with the data. These two features arethe secret of the excitement in modern cosmology: we have a theory which makespredictions, and these predictions can be tested by observations. Understanding what the theory is and what predictions it makes is not trivial.First, many of the predictions are statistical. We don't predict that there should bea hot spot in the cosmic microwave background （CMB） at RA = 15h, dec= 27~~~~.Rather, predictions are about the distribution and magnitude of hot and cold spots.Second, these predictions, and the theory on which they are based, involve lots ofsteps, many arguments drawn from a broad range of physics. For example, wewill see that the distribution of hot and cold spots in the CMB depends on quan-tum mechanics, general relativity, fluid dynamics, and the interaction of light withmatter. So we will indeed follow the first dictum of the Men of the Great Assem-bly and be patient before coming to judgment. Indeed, the fundamental measuresof structure in the universe——the power spectra of matter and radiation——agreeextraordinary well with the current cosmological theory, but we won't have thetools to understand this agreement completely until Chapters 7 and 8. Sober mindshave always knows that it pays to be patient before pronouncing judgment on ideasas lofty as those necessary to understand our Universe. The modern twist on this"Be patient" theme is that we need to set up the framework （in this case Chapters.

內(nèi)容概要

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 galaxies. Today, the Sloan Digital Sky Survey and the Two Degree Field between them have recorded the 3D positions of half a million galaxies.

作者簡介

作者：(英國)都德爾遜 (Scott Dodelson)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(fā)表了七十多篇論文，其中大部分是關于宇宙的微波背景和大尺度結(jié)構(gòu)。目次：標準模型及其它；平坦擴張的宇宙；遠離平衡態(tài)；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(shù)；附錄C：特殊函數(shù)；附錄D：符號；參考文獻；索引。讀者對象：理論物理、天文物理和宇宙學等專業(yè)的高年級本科生、研究生和相關專業(yè)的科研人員。

書籍目錄

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  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  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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《現(xiàn)代宇宙學》的特色：（1）講解了現(xiàn)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。

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