Structure of Dark Matter Halos From Hierarchical Clustering

Details Structure of Dark Matter Halos From Hierarchical Clustering Structure of Dark Matter Halos From Hierarchical Clustering

2000-08-07

arxiv.org/abs/astro-ph/0008104v2

Astrophys.J.557:533,2001

Astronomy and Astrophysics

Astrophysics

34 including 23 figures, revised version, accepted for publication in ApJ

Scientific paper

10.1086/321666

We investigate the structure of the dark matter halo formed in the cold dark matter scenario using $N$-body simulations. We simulated 12 halos with the mass of $6.6\times 10^{11}M_{\odot}$ to $8.0\times 10^{14}M_{\odot}$. In almost all runs, the halos have density cusps proportional to $r^{-1.5}$ developed at the center, which is consistent with the results of recent high-resolution calculations. The density structure evolves in a self-similar way, and is universal in the sense that it is independent of the halo mass and initial random realization of density fluctuation. The density profile is in good agreement with the profile proposed by Moore et al. (1999), which has central slope proportional to $r^{-1.5}$ and outer slope proportional to $r^{-3}$. The halo grows through repeated accretion of diffuse smaller halos. We argue that the cusp is understood as a convergence slope for the accretion of tidally disrupted matter.

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