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N-Body Results on Dark Matter

Published online by Cambridge University Press:  04 August 2017

Simon D. M. White
Simon D. M. White*
Affiliation:
Steward Observatory, University of Arizona, Tucson, Arizona 85721, U.S.A.

Abstract

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The structure of the dominant “dark” component of the Universe may evolve primarily under the influence of gravity. A number of models for the evolution of the Universe make specific predictions for the statistical properties of density fluctuations at early times. N-body simulations can follow the nonlinear development of such fluctuations to the present day. A major difficulty arises because we cannot observe the present mass distribution directly. Recent N-body work has concentrated on models dominated by weakly interacting free elementary particles. Neutrino-dominated but otherwise conventional cosmologies pass rapidly from a smooth distribution to one dominated by lumps with masses greater than those of any known object. Cosmologies dominated by “cold dark matter” produce mass distributions which fit the observed galaxy distribution (i) if Ω = 0.1–0.2 and galaxies follow the mass distribution, or (ii) if Ω = 1, HO < 50 km/s/Mpc and galaxies form preferentially in high density regions. In the latter case, clumps form with flat rotation curves with about the amplitude and abundance expected for galaxy halos.

Type
Review Paper
Information
Symposium - International Astronomical Union , Volume 117: Dark Matter in the Universe , 1987 , pp. 263 - 278
Copyright
Copyright © Reidel 1987 

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