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Many observational problems such as the observed flat rotation curves of galaxies and so on can be explained by a judicious invocation of this invisible “matter” whose constituents and interactions other than gravitational, is yet to be discovered. Since it is indicated that more than 90% of the observed universe consists of dark matter,the models incorporate the dynamics of the dark matter prior to that of visible matter. Thus the computer simulation model has three core components. The Friedmann metric, the dark matter and the visible matter.
E h(n + 3) = 1 at very nonlinear scales. Testing the conjecture that h(n + 3) is a constant is probably a little easier than looking for invariant profiles in the simulations but the results are still uncertain]. ¯ x) < The corresponding analysis for the intermediate regime, with 1 < ∼ 200, ∼ ξ(a, is more involved. 20) which shows that the power spectrum [and hence the correlation function] depends both on the fourier transform of the halo profiles as well as the power spectrum of the distribution of halo centres.
In a formal sense, numerical simulations cannot disprove [or even prove, strictly speaking] the occurrence of stable clustering, because of the finite dynamic range of any simulation. (2). Theoretically speaking, the “naturalness” of stable clustering is often overstated. The usual argument is based on the assumption that at very small scales — corresponding to high nonlinearities — the structures are “expected to be” frozen at the proper coordinates. However, this argument does not take into account the fact that mergers are not negligible at any scale in an Ω = 1 universe.