EDP Sciences
Free access
Volume 404, Number 3, June IV 2003
Page(s) 809 - 814
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20030549

A&A 404, 809-814 (2003)
DOI: 10.1051/0004-6361:20030549

Density profile asymptotes at the centre of dark matter halos

J. P. Mücket1 and M. Hoeft2

1  Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
2  International University Bremen, Campusring 1, 28759 Bremen, Germany
    e-mail: m.hoeft@iu-bremen.de

(Received 21 January 2003 / Accepted 10 April 2003)

For the spherical symmetric case, all quantities describing the relaxed dark matter halo can be expressed as functions of the gravitational potential  $\Phi$. Decomposing the radial velocity dispersion  $\sigma_{\rm r}$ with respect to  $\Phi$ at very large and very small radial distances the possible asymptotic behavior for the density and velocity profiles can be obtained. If reasonable boundary conditions are posed such as a finite halo mass and force-free halo centre the asymptotic density profiles at the centre should be much less steep than the profiles obtained within numerical simulations. In particular cases profiles like Plummer's model are obtained. The reasons of that seeming discrepancy with respect to the results of N-body simulations are discussed.

Key words: cosmology: theory -- dark matter -- galaxies: formation -- galaxies: structure -- methods: analytical

Offprint request: J. P. Mücket, jpmuecket@aip.de

© ESO 2003