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宇宙膨胀和大尺度结构 |
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基本信息·出版社：世界图书出版公司
·页码：400 页
·出版日期：2009年01月
·ISBN：7506292785/9787506292788
·条形码：9787506292788
·版本：第1版
·装帧：平装
·开本：16
·正文语种：英语
·丛书名：经典英文物理教材系列
·外文书名：Cosmological inflation and large-scale structure
内容简介 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.
目录 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
……
序言 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.
This book is based loosely on our 1993 Physics Reports article. We have widened the range of discussion and have made much of the material more pedagogical. We believe that this book will prove useful to starting graduate students in cosmology, to active researchers specializing in the field, and to all levels in between.
Our view of the inflationary cosmology and its consequences has been influenced by many people over the years. ARL especially thanks Alfredo Henriques and Gordon Moorhouse for showing the way into this research area. DHL would like particularly to acknowledge a long term collaboration with Ewan Stewart. Much thanks is due to all our collaborators on the topics within this book, namely Mark Abney, Domingos Barbosa, Tiago Barreiro, John Barrow, Marco Bruni, Ted Bunn, Ed Copeland, Laura Covi, George Ellis, Mary Galliard, Juan Garcia-Bellido, Anne Green, Louise Griffiths, Ian Grivell, Rocky Kolb, Andrew Laycock, Jim Lidsey, Andrei Linde, Anupam Mazumdar, Milan Miji~, Manash Mukherjee, Hitoshi Murayama, Paul Parsons, Antonio Riotto, Dave Roberts, Leszek Roszkowski, Bob Schaefer, Franz Schunck, Douglas Scott, Qaisar Shaft, Ewan Stewart, Will Sutherland, Michael Turner, Pedro Viana, David Wands, Martin White, and Andrzej Woszczyna. Apart from our collaborators, we have had useful conversations with many others, far too many to mention. We hope they know who they are!
We are extremely grateful to Andrei Linde, Martin White, and especially Gordon Moorhouse
for their careful reading of the manuscript. The figures for Chapter 12 were made by Pedro Viana, and the compilation of cosmic microwave background anisotropy data shown in Figures 5.9 and 9.2 was kindly provided by Martin White. Many figures were made using the superb publically available CMBFAST code (Seljak and Zaldarriaga 1996), which we strongly recommend everyone to get.
Although we wrote most of the book at our home institutes, occasionally we were some where more glamorous. ARL would like to thank the Universit di Padova, the University of New South Wales, and the Aspen Center for Physics, and DHL the University of California at Berkeley. ARL acknowledges the generous support of the Royal Society throughout this endeavour.
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