Dark Matter Density in Disk Galaxies
arXiv:0807.1973 · doi:10.1017/S1743921308027415
Abstract
I show that the predicted densities of the inner dark matter halos in LCDM models of structure formation appear to be higher than estimates from real galaxies and constraints from dynamical friction on bars. This inconsistency would not be a problem for the LCDM model if physical processes that are omitted in the collisionless collapse simulations were able to reduce the dark matter density in the inner halos. I review the mechanisms proposed to achieve the needed density reduction.
12 pages, 5 figures, to appear in "The Galaxy Disk in Cosmological Context" eds Andersen, Bland-Hawthorn & Nordstrom
References in corpus (9)
- Formation and evolution of galaxy dark matter halos and their substructure
- Beyond Inside-Out Growth: Formation and Evolution of Disk Outskirts
- Stellar Feedback in Dwarf Galaxy Formation
- Cosmological puzzle resolved by stellar feedback in high redshift galaxies
- The Causes of Halo Shape Changes Induced by Cooling Baryons: Disks Versus Substructures
- Dark and Baryonic Matter in Bright Spiral Galaxies: II. Radial Distributions for 34 Galaxies
- Resonances in Barred Galaxies
- Bar-Halo Friction in Galaxies III: Halo Density Changes
- Modeling the Gas Flow in the Bar of NGC 1365