## Density profiles of dark matter halos in an improved secondary infall model
^{1} Istituto di Astronomia dell'Università di Catania, Viale A. Doria 6, I-95125 Catania, Italy^{2} Dipartimento di Matematica, Università Statale di Bergamo, Piazza Rosate 2, I-24129 Bergamo, Italy^{3} Osservatorio Astrofisico di Catania and CNR-GNA, Viale A. Doria 6, I-95125 Catania, Italy^{4} Facoltá di Ingegneria, Università Statale di Bergamo, Viale G. Marconi 5, I-24044 Dalmine, Bergamo, Italy^{5} I.N.F.N., Sezione di Milano, Milano, Italy^{6} C.C.S. and D.M.O./FEEC, State University at Campinas, S. P., Brazil
In this paper we calculate the density profiles of virialized halos
both in the case of structure evolving hierarchically from a
scale-free Gaussian field having a
power spectrum in a
Universe and in the case of the CDM
model, by using a modified version of Hoffman & Shaham's (1985)
(hereafter HS) and Hoffman's (1988) model. We suppose that the initial
density contrast profile around local maxima is given by the mean peak
profile introduced by Bardeen et al. (1986) (hereafter BBKS), and is
not just proportional to the two-point correlation function, as
assumed by HS. We show that the density profiles, both for scale-free
Universes and the CDM model, are not power-laws but have a logarithmic
slope that increases from the inner halo to its outer parts. Both
scale-free, for , and CDM density
profiles are well approximated by Navarro et al. (1995, 1996, 1997)
profile. The radius
This article contains no SIMBAD objects. ## Contents- 1. Introduction
- 2. Limits of the SIM and Hoffman & Shaham's approaches
- 3. The model
- 4. Results and discussion
- 5. Conclusions
- References
© European Southern Observatory (ESO) 2000 Online publication: December 17, 1999 |