Is the Universe Open Or Closed?: The Density of Matter in the UniverseThis 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 discuss all the relevant cosmological and astrophysical evidence and come to the conclusion that the balance of arguments presently lies with a density of around twenty per cent of the critical density required for the Universe to ultimately recollapse. Because the arguments presented constitute a 'state-of-the-art' analysis of the observational and theoretical arguments surrounding the existence of dark matter, primordial nucleosynthesis, large-scale structure formation and the cosmic microwave background radiation, this study provides the reader with an indispensable introduction to the most exciting recent developments in modern cosmology. Written by two eminent cosmologists, this topical and provocative book will be essential reading for all cosmologists and astrophysicists. |
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abundance analysis angular scales anisotropy arguments astrophysical background model baryonic bias CDM model Chapter COBE Coles Coma cluster component constraints contribution corresponding cosmic cosmological constant cosmological models cosmologists critical density curvature dark matter decoupling density fluctuations density universe depends detection deuterium dipole discussed distance distribution dynamical Efstathiou Ellis epoch estimates evidence evolution expansion flat fraction Friedman equation function galactic galactic haloes galaxy clustering global gravitational lensing haloes helium Hubble inferred inflation inflationary models inhomogeneities ionised issue large scales large-scale structure linear Lucchin luminosity mass measure microwave background MNRAS modes neutrino neutrons nucleosynthesis objects observations parameter particle peculiar velocity Peebles perturbations photons Phys physics Planck possible potential power spectrum predicted primordial problem produce quasar radiation relatively rich clusters Sachs-Wolfe effect sample scalar field spatial sections standard model statistical stellar temperature theoretical theory tion uncertainty unity universe models