1996/10/23 by Julio F. Navarro, V. R. Eke, Vincent R. Eke +1 · 616 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Cold dark matter #Cuspy halo problem #Dark matter #Dark matter halo #Dwarf galaxy #Dwarf galaxy problem #Dwarf spheroidal galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #Halo #Interacting galaxy #Physics #RADIUS #Stellar, planetary, and galactic studies #Supernova #astro-ph
paper · pdf · doi:10.1093/mnras/283.3.l72
published in Monthly Notices of the Royal Astronomical Society 283(3), L72-L78 (Oxford University Press) · PS file. 6 figures included. 531072 bytes. Accepted for publication in MNRAS Letters. Also available from http://penedes.as.arizona.edu/~jfn/preprints . (File name: rcore.ps.gz)
arxiv created 1996/10/23 · openalex publication_date 1996/12/01 · arxiv updated 2016/06/08 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We use N-body simulations to examine the effects of mass outflows on the density profiles of cold dark matter (CDM) haloes surrounding dwarf galaxies. In particular, we investigate the consequences of supernova-driven winds that expel a large fraction of the baryonic component from a dwarf galaxy disc after a vigorous episode of star formation. We show that this sudden loss of mass leads to the formation of a core in the dark matter density profile, although the original halo is modelled by a coreless (Hernquist) profile. The core radius thus created is a sensitive function of the mass and radius of the baryonic disc being blown up. The loss of a disc with mass and size consistent with primordial nucleosynthesis constraints and angular momentum considerations imprints a core radius that is only a small fraction of the original scalelength of the halo. These small perturbations are, however, enough to reconcile the rotation curves of dwarf irregulars with the density profiles of haloes formed in the standard CDM scenario.