The structure of dark matter halos: self-similar models versus N-body simulations
| dc.creator | Chuzhoy, Leonid | |
| dc.date | 2006-08-29 | |
| dc.date.accessioned | 2026-07-07T07:19:27Z | |
| dc.date.available | 2026-07-07T07:19:27Z | |
| dc.description | We derive the density profile of cold dark matter halos using a self-similar accretion model. We show that if the clumpiness of the infalling matter is taken into account, then the inner density slope, d(log{rho})/d(log{r}), is close to -1. Compared with the density profiles predicted by different numerical simulations, we find that outside ~0.1% of the virial radius, our solutions agree best with the fitting formula proposed by Navarro et al. (2004), d(ln{rho})/d(ln{r})=-2(r/R)^0.17, where R is a characteristic radius, inside which the density profile becomes shallower than isothermal. | |
| dc.description | 3 pages, 3 figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0608637 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0608637 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/114628 | |
| dc.subject | Astrophysics | |
| dc.title | The structure of dark matter halos: self-similar models versus N-body simulations | |
| dc.type | text |