A dynamical determination of the density of galactic halos formed from seeded dark matter

Details A dynamical determination of the density of galactic halos formed from seeded dark matter A dynamical determination of the density of galactic halos formed from seeded dark matter

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...273...95z&link_type=abstract

Astronomy and Astrophysics, Vol. 273, p. 95 (1993)

Astronomy and Astrophysics

Astrophysics

Scientific paper

A new approach for the self-consistent determination of the density profile of halo formed by the gravitational clustering of an initially homogeneous background of dark matter about a seed source is presented. The final steady state configuration consists of particles freely streaming in elongated orbits with a weighting function in terms of the orbital invariants (energy and angular momentum) assumed to be unchanged from the initial, pre-accreting one. Calculations indicate that a galactic halo with the right characteristics (mass ~10 galactic mass at ~10^2^ kpc, an inverse power-law density profile with index ~2) can be formed, but only in the presence of a seed source with a mass typically 10% of that of the halo, and when the dark matter has cooled down.

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