Is the Universe Open or Closed?: The Density of Matter in the Universe

✍ Scribed by Peter Coles, George Ellis

• Publisher: Cambridge University Press
• Year: 1997
• Tongue: English
• Leaves: 253
• Series: Cambridge Lecture Notes in Physics; 7
• Edition: 1
• Category: Library

✦ Synopsis

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.

✦ Table of Contents

Cover
Intro Blurb
Half Title
CAMBRIDGE LECTURE NOTES IN PHYSICS
Title
Copyright
Contents
Preface
Acknowledgements
1 Introduction
1.1 The issue
1.2 Cosmological models
1.2.2 Geometry: the cosmological principle
1.2.3 The Friedman equations
1.2.4 Open, closed and flat cosmologies
1.2.5 The equation of state
1.2.6 Useful formulae
1.2.7 The big-bang model
1.3 Cosmological criteria
1.4 Preliminary discussion of estimates
1.5 Plan of the argument
2 Theoretical arguments
2.1 Simplicity
2.2 The flatness problem

2.2.2 Statement of the problem
2.2.3 An extended Copernican principle?
2.2.4 Measures and probabilities
2.3 Inflationary models
2.3.1 The effect of inflaizon

2.3.3 Probability arguments
Different ways of using probability
Different probability measures
The applicability of probability ideas

2.3.5 The occurrence of inflation
2.3.6 The exactly critical case
2.4 The cosmological constant
2.4.1 Flatness without a critical density

2.5 Particle physics
2.5.1 Hot thermal relics (HDM)
2.5.2 Cold thermal relics (CDM)
2.5.3 Decaying dark matter
2.5.4 Possible laboratory tests?
2.6 Summary
3 Cosmological observations
3.1 The age of the universe
3.1.1 Model ages
3.1.2 The Hubble constant
3.1.3 Ages of objects
3.1.4 Discussion
3.1.5 The cosmological constant
3.2 'Classical cosmology'
3.2.1 Standard candles
3.2.2 Angular sizes
3.2.3 Number counts
3.3 Gravitational lensing
3.3.1 Multiply imaged QSOs
3.3.2 Microlensing
3.4 Summary
• Ages
• Classical cosmology
• Gravitational lensing
4 Element abundances
4.1 Theory of nucleosynthesis
4.1.1 Prelude
4.1.2 Big-bang nucleosynthesis
4.1.3 Helium 4
4.1.4 Other light nuclei
4.2 The evidence
4.2.1 Helium 4
4.2.2 Deuterium
4.2.3 Helium 3
4.2.4 Lithium 7
4.2.5 Observations vs. theory
4.3 Non-standard nucleosynthesis

4.4.1 Summary of constraints
4.4.2 Non-baryonic dark matter
4.5 Summary
5 Astrophysical arguments
5.1 Galaxies
5.1.1 The mass-to-light ratio
5.1.2 Spiral and elliptical galaxies
5.1.3 Galactic microlensing
5.1.4 The galactic density of matter
5.2 Clusters of galaxies
5.2.1 Galaxies in clusters
5.2.2 Dynamical dark matter in clusters
5.2.3 X-ray gas in clusters
5.2.4 The baryon catastrophe?
5.2.5 Arcs, arclets and image distortions
5.2.6 Subclustering and time-scales
5.3 The intergalactic medium (1GM)
5.3.1 Quasar spectra
5.3.2 Spectral distortions of the CMB
5.3.3 A hot 1GM?
5.4 Summary
6 Large-scale structure
6.1 Theoretical prelude
6.1.1 Gravitational instability
6.1.2 Linear perturbation theory
6.1.3 Primordial density fluctuations
6.1.4 The transfer function
6.1.5 Beyond linear theory?
6.1.6 The contenders
6.2 Galaxy clustering
6.2.1 Redshift surveys
6.2.2 Galaxy and cluster correlations
6.2.3 Angular correlations
6.2.4 Fluctuations in counts
6.2.5 Power-spectra
6.2.6 The abundances of objects
6.3 Dipole analysis
6.3.1 The basic idea
6.3.2 The IRAS dipole
6.3.3 Rich clusters of galaxies
6.3.4 Other sources of error
6.4 Galaxy peculiar velocities
6.4.1 Bulk flows and streaming motions
6.4.2 Velocity-density reconstruction
6.4.3 Redshift-space distortions
6.5 Summary
7 The cosmic microwave background
7.1 Introduction
7.1.1 The relic radiation
7.1.2 The angular power spectrum
7.1.3 Folklore and phenomenology
7.1.4 Compatible low-density models
7.2 The Sachs—Wolfe effect
7.2.1 The fiat case
7.2.2 Gravitational waves
7.2.3 Non-flat models
7.3 Smaller-scale radiation anisotropies
7.3.1 A two-fluid model
7.3.2 Kinetic theory
7.3.3 Intermediate scales: the Doppler peaks
7.4 Observational status
7.4.1 COBE and all that
7.4.2 The search for the Doppler peak
7.4.3 Prospects for the future
7.5 Summary
8 More realistic universe models
8.1 Lumpy universe models
8.2 The fitting problem and integral constraints
8.3 Dynamical and observational effects of dumpiness
8.3.1 Effects on the field equations
Newtonian theory
General relativity
8.3.2 Effects on observations
8.3.3 Implications
8.4 The issue of scale

8.4.2 Selection effects related to scale
8.4.3 Estimating the packing fraction
Horizons and scales beyond the horizon
8.5 Taking inhomogeneity seriously
9 What is the verdict?
9.1 The evidence
9.2 The weight of evidence
9.3 Criteria for cosmological theories
9.4 Future prospects
9.5 The standard model of cosmology
References
Index