2000/08/31 by Toshiyuki Fukushige, Junichiro Makino · 2 citations
Mathematics · Physics and Astronomy · #Accretion (finance) #Astrophysics #Cold dark matter #Cosmology #Cusp (singularity) #Cuspy halo problem #Dark Matter and Cosmic Phenomena #Dark matter #Dark matter halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Geometry #Halo #Hot dark matter #Mathematics #Physics #Realization (probability) #Scientific Research and Discoveries #Statistics #Structure formation #astro-ph
paper · pdf · doi:10.1086/321666
published as Astrophys.J.557:533,2001 · 34 including 23 figures, revised version, accepted for publication in ApJ
arxiv created 2001/04/21 · openalex publication_date 2001/08/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the structure of the dark matter halo formed in the cold dark matter scenario using N -body simulations. We simulated 12 halos with masses of 6.6 × 10 11 -8.0 × 10 14 M ☉ . In all runs, the halos have density cusps proportional to r -1.5 developed at their centers, which is consistent with the results of recent high-resolution calculations. The density structure evolves in a self-similar way and is universal in the sense that it is independent of the halo mass and initial random realization of density fluctuation. The density profile is in good agreement with the profile proposed by Moore et al., which has a central slope proportional to r -1.5 and an outer slope proportional to r -3 . The halo grows through repeated accretion of diffuse smaller halos. We argue that the cusp is understood as a convergence slope for the accretion of tidally disrupted matter.