Dark halo mergers and the formation of a universal profile

Details Dark halo mergers and the formation of a universal profile Dark halo mergers and the formation of a universal profile

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.293..337s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 293, p. 337

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120

Halos, Dark Matter, Cosmology, Interacting Galaxies, Celestial Mechanics, Computational Astrophysics, Stellar Motions, Many Body Problem

Scientific paper

We argue that a universal density profile for dark matter haloes arises as a natural consequence of hierarchical structure formation: it is a fixed point in the process of repeated mergers. We present analytic and numerical arguments for the emergence of a particular form of the central cusp profile. At small radii, the density should vary as r exp -alpha, with alpha determined by the way in which the characteristic density of haloes scales with their mass. If small haloes are dense, then alpha is large. The mass-density relation can be related to the power spectrum of initial fluctuations, P(k), through 'formation time' arguments. Early structure formation leads to steep cusps. For P(k) of approximately k exp n, we find alpha equal to about 3(3 + n)/(5 + n). The universal profile is generated by tidal stripping of small haloes as they merge with larger objects.

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