Astronomy and Astrophysics – Astrophysics
Scientific paper
2008-08-28
Astrophys.J.690:102-110,2009
Astronomy and Astrophysics
Astrophysics
25 pages, 3 figures, fig with parts 1 to d, fig 3 with parts a to d
Scientific paper
10.1088/0004-637X/690/1/102
Cosmological simulations consistently predict specific properties of dark matter halos, but these have not yet led to a physical understanding that is generally accepted. This is especially true for the central regions of these structures. Recently two major themes have emerged. In one, the dark matter halo is primarily a result of the sequential accretion of primordial structure (ie `Nature'); while in the other, dynamical relaxation (ie `Nurture') dominates at least in the central regions. Some relaxation is however required in either mechanism. In this paper we accept the recently established scale-free sub-structure of halos as an essential part of both mechanisms. Consequently; a simple model for the central relaxation based on a self-similar cascade of tidal interactions, is contrasted with a model based on the accretion of adiabatically self-similar, primordial structure. We conclude that a weak form of this relaxation is present in the simulations, but that is normally described as the radial orbit instability.
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