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Understanding the Equilibrium Structureof CDM Halos

Published online by Cambridge University Press:  19 May 2006

G.A. Mamon ,
F. Combes ,
C. Deffayet ,
B. Fort ,
P.R. Shapiro ,
K. Ahn ,
M. Alvarez ,
I.T. Iliev  and
H. Martel
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 whichresult from the nonlinear growth of Gaussian-random-noise densityfluctuations in the CDM universe. This talk summarized our attempts toderive and explain this universal structure by analyticalapproximation and simplified models. As an example, we show here thata 1D spherical infall model involving a fluid approximation derivedfrom the Boltzmann equation can explain not only the halo density profilebut its phase-space density profile, as well.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 20: Mass Profiles and Shapes of Cosmological Structures , 2006 , pp. 5 - 10
Copyright
© EAS, EDP Sciences, 2006

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