宇宙膨脹和大尺度結構

《宇宙膨脹和大尺度結構》是2009年世界圖書出版公司出版的一本圖書，作者是安德魯等。

基本介紹

• 書名：宇宙膨脹和大尺度結構
• 作者：(英國)安德魯 (Andrew R.liddle) (英國)David H.lyth
• 原版名稱：Cosmological Inflation and Large-scale Structure
• ISBN：9787506292788
• 頁數： 400頁 
• 出版社：世界圖書出版公司
• 出版時間：2009年1月1日
• 裝幀：平裝 
• 開本：16
• 叢書名：經典英文物理教材系列
• 正文語種：簡體中文, 英語
• 條形碼：9787506292788
• 尺寸：25.6x18.2x2 cm
• 重量：739g
• 版次：第1版

內容簡介

《宇宙膨脹和大尺度結構》主要內容：The 1990s have seen substantial consolidation of theoretical cosmology, coupled with dramatic observational advances, including the emergence of an entirely new field of observational astronomy - the study of irregularities in the cosmic microwave background radiation. A key idea of modern cosmology is cosmological inflation, which is a possible theory for the origin of all structures in the Universe, including ourselves! The time is ripe for a new book describing this field of research.

目錄

Frequently used symbols

Preface

1 INTRODUCTION

1.1 This book

1.2 The Universe we see

1.3 Overview: From cosmological inflation to large-scale structure

1.4 Notes on examples

2 THE HOT BIG BANG COSMOLOGY

2.1 The expanding Universe

2.2 Epochs

2,3 Scales

2.4 The cosmic microwave background

2,5 Ingredients for a model of the Universe

2.6 History of our Universe

Examples

3 INFLATION

3.1 Motivation for inflation

3.2 Inflation in the abstract

3.3 Scalar fields in cosmology

3.4 Slow-roll inflation

3.5 Exact solutions

3.6 Hamilton-Jacobi formulation of inflation

3.7 Inflationary attractor

3.8 Reheating: Recovering the Hot Big Bang

3.9 Thermal inflation

Examples

4 SIMPLEST MODEL FOR THE ORIGIN OF STRUCTURE I

4.1 Introduction

4.2 Sequence of events

4.3 Gaussian perturbations

4.4 Density perturbation: Newtonian treatment

4.5 The Baryon density contrast: Newtonian treatment

4.6 Cosmological perturbation theory

4.7 Evolution equations

4.8 Outside the horizon

4.9 Peculiar velocity in the relativistic domain

Examples

5 SIMPLEST MODEL FOR THE ORIGIN OF STRUCTURE H

5.1 From horizon entry to galaxy formation

5.2 The cosmic microwave background anisotropy

5.3 Polarization

5.4 Reionization

Examples

6 EXTENSIONS TO THE SIMPLEST MODEL

6.1 Modifying the cold dark matter hypothesis

6.2 ACDM model

6.3 Open CDM model

6.4 Fine tuning issues

6.5 Gravitational waves

6.6 Isocurvature perturbations

Examples

7 SCALAR FIELDS AND THE VACUUM FLUCTUATION

7.1 Classical scalar field

7.2 Quantized free scalar field in fiat space-time

7.3 Several scalar fields

7.4 Vacuum fluctuation of inflaton field

7.5 Spectrum of the primordial curvature perturbation

7.6 Beyond the slow-roll approximation

7.7 Gravitational waves

7.8 Generating an isocurvature perturbation

7.9 A multicomponent inflaton?

Examples

8 BUILDING AND TESTING MODELS OF INFLATION

8.1 Overview

8.2 Form of the scalar field potential

8.3 Single-field models

8.4 Hybrid inflation models

8.5 The spectral index as a discriminator

8.6 Models from extended theories of gravity

8.7 Open inflation models

Examples

9 THE COSMIC MICROWAVE BACKGROUND

9.1 Large angles and the cosmic background explorer (COBE) satellite

9.2 Degree-scale observations and acoustic oscillations

9.3 Aspects of microwave anisotropy satellites

Examples

10 GALAXY MOTIONS AND CLUSTERING

10.1 Clustering of galaxies

10.2 Galaxy velocities

Examples

11 TIlEQUASI-LINEARREGIME

11．1 Gravitational collapse

1 1．2 Press-5；chechter theory

1 1．3 Theory of peaks

1 1．4 Nlimetical simulations

1 1．5 App~~cafions of Press-Schechter theory

11．6 Reionizafion ofthe Universe

Examples

12 PUTING OBSERVATIONS TOGETHER

12．1 Observations

12．2 Critical—density models

12．3 Low-density models

12．4 Other options

12．5 Summary

13 oUTLooK FoR THE FUTURE

14 ADVANCED TOPIC：CoSMoLoGICAL PERTURBATION THEORY

14．1 Special relativity

14．2 Fluid flow in special relativity

14．3 Special relativity using generic coordinates

14．4 General relativity

14．5 Cosmological perturbations

14．6 Evolution of the perturbations

Examples

15 ADVANCED TOPIC：DIFFUSIoN AND FREESTREAMING

15．1 Matter

15．2 Gas dynamics in fiat space—time

15．3 Gas dynamics in the perturbed Universe

15．4 Multipoles and the Boltzmann hierarchy

15．5 Polarization

15．6 Initial conditionsandthetransferfuncfions

Examples

Appendix：Constants and parameters

Numerical solutions and hintsfor selected examples

References

Index