Density Profiles of Dark Halos from their Mass Accretion Histories
| dc.creator | Alvarez, Marcelo A. | |
| dc.creator | Ahn, Kyungjin | |
| dc.creator | Shapiro, Paul R. | |
| dc.date | 2003-02-17 | |
| dc.date.accessioned | 2026-07-07T02:07:37Z | |
| dc.date.available | 2026-07-07T02:07:37Z | |
| dc.description | We use the universal mass accretion history recently reported for simulations of halo formation in the cold dark matter model (CDM) to analyze the formation and growth of a single halo. We derive the time-dependent density profile three different ways, based upon three approximations of successively greater realism: equilibrium, radial orbits, and a fluid approximation. For the equilibrium model, the density profile is well-fit by either an NFW or Moore profile over a limited range of radii and scale factors. For the radial orbit model, we find profiles which are generally steeper than the NFW profile, with an inner logarithmic slope approaching -2, consistent with a purely radial collisionless system. In the fluid approximation, we find good agreement with the NFW and Moore profiles for radii resolved by N-body simulations (r/r_200 > 0.01), and an evolution of concentration parameter nearly identical to that found in N-body simulations. The evolving structure of cosmological halos is therefore best understood as the effect of a time-varying rate of mass infall on a smoothly distributed, isotropic, collisionless fluid. | |
| dc.description | 3 pages, 5 figures, to appear in proceedings of "The Eighth Texas-Mexico Conference on Astrophysics" eds. Mauricio Reyes, Enrique Vazquez-Semadeni (2003), RevMexAA SC (2003) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0302336 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0302336 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/5756 | |
| dc.subject | Astrophysics | |
| dc.title | Density Profiles of Dark Halos from their Mass Accretion Histories | |
| dc.type | text |