Density profiles in a spherical infall model with non–radial motions
Lyceum of Naxos, Chora of Naxos, Naxos 84300, Greece
Corresponding author: N. Hiotelis, email@example.com
Accepted: 5 November 2001
A generalized version of the Spherical Infall Model (SIM) is used to study the effect of angular momentum on the final density profile of a spherical structure. The numerical method presented is able to handle a variety of initial density profiles (scale or not scale free) and no assumption of self-similar evolution is required. The realistic initial overdensity profiles used are derived by a CDM power spectrum. We show that the amount of angular momentum and the initial overdensity profile affect the slope of the final density profile at the inner regions. Thus, a larger amount of angular momentum or shallower initial overdensity profiles lead to shallower final density profiles at the inner regions. On the other hand, the slope at the outer regions is not affected by the amount of angular momentum and has an almost constant value equal to that predicted in the radial collapse case.
Key words: galaxies: formation / galaxies: halos / galaxies: structure / methods: numerical
© ESO, 2002