Is the Universe Open or Closed?

, by Coles, Peter; Ellis, George Francis Rayner

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ISBN: 9780521566896 | 0521566894
Cover: Paperback
Copyright: 6/1/1997

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This controversial book examines one of the most fundamental questions of modern cosmology: how much matter is there in the Universe? This issue affects theories of the origin and evolution of the Universe as well as its geometrical structure and ultimate fate. The authors address this debate and point out the most likely avenues for determining the actual density of Universe matter in both visible and invisible forms by pulling together evidence from all available sources. They conclude that the balance of arguments presently lies with a density of around twenty percent of the critical density required for the Universe to ultimately recollapse. Written by two eminent cosmologists, this topical and provocative book will be essential reading for all cosmologists and astrophysicists.

Preface

xiii

(2)

Acknowledgements

1 Introduction

(18)

1.1 The issue

(3)

1.2 Cosmological models

(6)

1.2.1 The nature of cosmological models

(1)

1.2.2 Geometry: the cosmological principle

(1)

1.2.3 The Friedman equations

(1)

1.2.4 Open, closed and flat cosmologies

(1)

1.2.5 The equation of state

(1)

1.2.6 Useful formulae

(1)

1.2.7 The big-bang model

(1)

1.3 Cosmological criteria

(3)

1.4 Preliminary discussion of estimates

(3)

1.5 Plan of the argument

(3)

2 Theoretical aguments

(28)

2.1 Simplicity

(1)

2.2 The flatness problem

(7)

2.2.1 Evolution of

(1)

2.2.2 Statement of the problem

(1)

2.2.3 An extended Copernican principle?

(2)

2.2.4 Measures and probabilities

(3)

2.3 Inflationary models

(9)

2.3.1 The effect of inflation

(2)

2.3.2 Can inflation produce a low value of?

(1)

2.3.3 Probability arguments

(4)

2.3.4 The modification of by inflation

(1)

2.3.5 The occurrence of inflation

(1)

2.3.6 The exactly critical case

(1)

2.4 The cosmological constant

(3)

2.4.1 Flatness without a critical density

(1)

2.4.2 Fine-tunning of

(2)

2.5 Particle physics

(7)

2.5.1 Hot thermal relics (HDM)

(2)

2.5.2 Cold thermal relics (CDM)

(1)

2.5.3 Decaying dark matter

(1)

2.5.4 Possible laboratory tests?

(1)

2.6 Summary

(1)

3 Cosmological observations

(22)

3.1 The age of the universe

(7)

3.1.1 Model ages

(1)

3.1.2 The Hubble constant

(2)

3.1.3 Ages of objects

(2)

3.1.4 Discussion

(1)

3.1.5 The cosmological constant

(2)

3.2 `Classical cosmology'

(10)

3.2.1 Standard candles

(3)

3.2.2 Angular sizes

(2)

3.2.3 Number counts

(4)

3.3 Gravitational lensing

(2)

3.3.1 Multiply imaged QSOs

(1)

3.3.2 Microlensing

(1)

3.4 Summary

(3)

4 Element abundances

(20)

4.1 Theory of nucleosynthesis

(8)

4.1.1 Prelude

(3)

4.1.2 Big-bang nucleosynthesis

(2)

4.1.3 Helium 4

(1)

4.1.4 Other light nuclei

(2)

4.2 The evidence

(5)

4.2.1 Helium 4

(1)

4.2.2 Deuterium

(1)

4.2.3 Helium 3

(1)

4.2.4 Lithium 7

(1)

4.2.5 Observations vs. theory

(2)

4.3 Non-standard nucleosynthesis

(3)

4.4 Implications for

(1)

4.4.1 Summary of constraints

(1)

4.4.2 Non-baryonic dark matter

(1)

4.5 Summary

(3)

5 Astrophysical arguments

(22)

5.1 Galaxies

(4)

5.1.1 The mass-to-light ratio

(1)

5.1.2 Spiral and elliptical galaxies

(1)

5.1.3 Galactic microlensing

(1)

5.1.4 The galactic density of matter

(1)

5.2 Clusters of galaxies

(8)

5.2.1 Galaxies in clusters

(1)

5.2.2 Dynamical dark matter in clusters

(2)

5.2.3 X-ray gas in clusters

(1)

5.2.4 The baryon catastrophe?

(1)

5.2.5 Arcs, arclets and image distortions

(2)

5.2.6 Subclustering and time-scales

(2)

5.3 The intergalactic medium (IGM)

101

(8)

5.3.1 Quasar spectra

101

(5)

5.3.2 Spectral distortions of the CMB

106

(1)

5.3.3 A hot IGM?

107

(2)

5.4 Summary

109

(2)

6 Large-scale structure

111

(38)

6.1 Theoretical prelude

111

(13)

6.1.1 Gravitational instability

112

(1)

6.1.2 Linear perturbation theory

113

(2)

6.1.3 Primordial density fluctuations

115

(2)

6.1.4 The transfer function

117

(2)

6.1.5 Beyond linear theory?

119

(1)

6.1.6 The contenders

120

(4)

6.2 Galaxy clustering

124

(7)

6.2.1 Redshift surveys

124

(1)

6.2.2 Galaxy and cluster correlations

125

(2)

6.2.3 Angular correlations

127

(1)

6.2.4 Fluctuations in counts

127

(1)

6.2.5 Power-spectra

128

(1)

6.2.6 The abundances of objects

128

(3)

6.3 Diple analysis

131

(6)

6.3.1 The basic idea

132

(1)

6.3.2 The IRAS dipole

133

(1)

6.3.3 Rich clusters of galaxies

134

(2)

6.3.4 Other sources of error

136

(1)

6.4 Galaxy peculiar velocities

137

(10)

6.4.1 Bulk flows and streaming motions

137

(4)

6.4.2 Velocity-denstiy reconstruction

141

(3)

6.4.3 Redshift-space distortions

144

(3)

6.5 Summary

147

(2)

7 The cosmic microwave background

149

(32)

7.1 Introduction

150

(7)

7.1.1 The relic radiation

150

(2)

7.1.2 The angular power spectrum

152

(3)

7.1.3 Folklore and phenomenology

155

(1)

7.1.4 Compatible low-density models

156

(1)

7.2 The Sachs-Wolfe effect

157

(7)

7.2.1 The flat case

159

(1)

7.2.2 Gravitational waves

160

(2)

7.2.3 Non-flat models

162

(2)

7.3 Smaller-scale radiation anisotropies

164

(9)

7.3.1 A two-fluid model

165

(2)

7.3.2 Kinetic theory

167

(3)

7.3.3 Intermediate scales: the Doppler peaks

170

(3)

7.4 Obserational status

173

(6)

7.4.1 COBE and all that

173

(3)

7.4.2 The search for the Doppler peak

176

(2)

7.4.3 Prospects for the future

178

(1)

7.5 Summary

179

(2)

8 Moew realistic universe models

181

(12)

8.1 Lumpy universe models

181

(1)

8.2 The fitting problem and integral constraints

182

(3)

8.3 Dynamical and observational effects of clumpiness

185

(4)

8.3.1 Effects on the field equations

185

(3)

8.3.2 Effects on observations

188

(1)

8.3.3 Implications

188

(1)

8.4 The issue of scale

189

(3)

8.4.1 Local and global values of

189

(1)

8.4.2 Selection effects related to scale

190

(1)

8.4.3 Estimating the packing fraction

191

(1)

8.5 Taking inhomogeneity seriously

192

(1)

9 What is the verdict?

193

(16)

9.1 The evidence

195

(4)

9.2 The weight of evidence

199

(4)

9.3 Criteria for cosmological theories

203

(1)

9.4 Future prospects

204

(1)

9.5 The standard model of cosmology

205

(4)

References

209

(14)

Index

223

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Is the Universe Open or Closed?

Summary

Table of Contents

Supplemental Materials