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Understanding the Equilibrium Structure of CDM Halos

Published online by Cambridge University Press:  19 May 2006

P.R. Shapiro
Affiliation:
Department of Astronomy, 1 University Station, C1400, Austin, TX 78712, USA
K. Ahn
Affiliation:
Department of Astronomy, 1 University Station, C1400, Austin, TX 78712, USA
M. Alvarez
Affiliation:
Department of Astronomy, 1 University Station, C1400, Austin, TX 78712, USA
I.T. Iliev
Affiliation:
Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada
H. Martel
Affiliation:
Département de Physique, de Génie Physique et d'Optique, Université Laval, Québec, QC G1K 7P4, Canada
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Abstract

N-body simulations find a universal structure for the halos which result from the nonlinear growth of Gaussian-random-noise density fluctuations in the CDM universe. This talk summarized our attempts to derive and explain this universal structure by analytical approximation and simplified models. As an example, we show here that a 1D spherical infall model involving a fluid approximation derived from the Boltzmann equation can explain not only the halo density profile but its phase-space density profile, as well.

Type
Research Article
Copyright
© EAS, EDP Sciences, 2006

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