Self-Similar Secondary Infall: Trying to Understand Halo Formation

Details Self-Similar Secondary Infall: Trying to Understand Halo Formation Self-Similar Secondary Infall: Trying to Understand Halo Formation

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21823402z&link_type=abstract

American Astronomical Society, AAS Meeting #218, #234.02; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

N-body simulations have revealed a wealth of information about dark matter halos, but their results are largely empirical. Using analytic means, we attempt to shed light on simulation results by generalizing the self-similar secondary infall model to include tidal torque. Imposing self-similarity allows us to analytically calculate the structure of the the halo in different radial regimes and numerically compute the profiles of the halo without being limited by resolution effects inherent to N-body codes. I will describe this simplified halo formation model and compare our results to mass and velocity profiles from recent N-body simulations. We find that angular momentum plays an important role in determining the structure of the halo at small radii.

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