Is the Universe Open or Closed?

by Coles, Peter; Ellis, George Francis Rayner

• ISBN13: 9780521566896
• ISBN10: 0521566894
• Format: Paperback
• Copyright: 1997-06-01
• Publisher: Cambridge Univ Pr

Summary

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

Preface	xiii	(2)
Acknowledgements	xv
1 Introduction	1	(18)
1.1 The issue	1	(3)
1.2 Cosmological models	4	(6)
1.2.1 The nature of cosmological models	4	(1)
1.2.2 Geometry: the cosmological principle	5	(1)
1.2.3 The Friedman equations	6	(1)
1.2.4 Open, closed and flat cosmologies	7	(1)
1.2.5 The equation of state	8	(1)
1.2.6 Useful formulae	9	(1)
1.2.7 The big-bang model	9	(1)
1.3 Cosmological criteria	10	(3)
1.4 Preliminary discussion of estimates	13	(3)
1.5 Plan of the argument	16	(3)
2 Theoretical aguments	19	(28)
2.1 Simplicity	19	(1)
2.2 The flatness problem	20	(7)
2.2.1 Evolution of	20	(1)
2.2.2 Statement of the problem	21	(1)
2.2.3 An extended Copernican principle?	22	(2)
2.2.4 Measures and probabilities	24	(3)
2.3 Inflationary models	27	(9)
2.3.1 The effect of inflation	27	(2)
2.3.2 Can inflation produce a low value of?	29	(1)
2.3.3 Probability arguments	30	(4)
2.3.4 The modification of by inflation	34	(1)
2.3.5 The occurrence of inflation	34	(1)
2.3.6 The exactly critical case	35	(1)
2.4 The cosmological constant	36	(3)
2.4.1 Flatness without a critical density	36	(1)
2.4.2 Fine-tunning of	37	(2)
2.5 Particle physics	39	(7)
2.5.1 Hot thermal relics (HDM)	41	(2)
2.5.2 Cold thermal relics (CDM)	43	(1)
2.5.3 Decaying dark matter	44	(1)
2.5.4 Possible laboratory tests?	45	(1)
2.6 Summary	46	(1)
3 Cosmological observations	47	(22)
3.1 The age of the universe	47	(7)
3.1.1 Model ages	47	(1)
3.1.2 The Hubble constant	48	(2)
3.1.3 Ages of objects	50	(2)
3.1.4 Discussion	52	(1)
3.1.5 The cosmological constant	52	(2)
3.2 `Classical cosmology'	54	(10)
3.2.1 Standard candles	55	(3)
3.2.2 Angular sizes	58	(2)
3.2.3 Number counts	60	(4)
3.3 Gravitational lensing	64	(2)
3.3.1 Multiply imaged QSOs	64	(1)
3.3.2 Microlensing	65	(1)
3.4 Summary	66	(3)
4 Element abundances	69	(20)
4.1 Theory of nucleosynthesis	69	(8)
4.1.1 Prelude	69	(3)
4.1.2 Big-bang nucleosynthesis	72	(2)
4.1.3 Helium 4	74	(1)
4.1.4 Other light nuclei	75	(2)
4.2 The evidence	77	(5)
4.2.1 Helium 4	78	(1)
4.2.2 Deuterium	78	(1)
4.2.3 Helium 3	79	(1)
4.2.4 Lithium 7	80	(1)
4.2.5 Observations vs. theory	80	(2)
4.3 Non-standard nucleosynthesis	82	(3)
4.4 Implications for	85	(1)
4.4.1 Summary of constraints	85	(1)
4.4.2 Non-baryonic dark matter	86	(1)
4.5 Summary	86	(3)
5 Astrophysical arguments	89	(22)
5.1 Galaxies	89	(4)
5.1.1 The mass-to-light ratio	90	(1)
5.1.2 Spiral and elliptical galaxies	91	(1)
5.1.3 Galactic microlensing	92	(1)
5.1.4 The galactic density of matter	92	(1)
5.2 Clusters of galaxies	93	(8)
5.2.1 Galaxies in clusters	93	(1)
5.2.2 Dynamical dark matter in clusters	94	(2)
5.2.3 X-ray gas in clusters	96	(1)
5.2.4 The baryon catastrophe?	97	(1)
5.2.5 Arcs, arclets and image distortions	97	(2)
5.2.6 Subclustering and time-scales	99	(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