Numerical modeling of galaxy evolution |
| |
Authors: | Naohito Nakasato |
| |
Institution: | (1) Department of Astronomy, University of Tokyo, Japan |
| |
Abstract: | A very significant problem in the modeling of disk-galaxy formation in the cold dark matter (CDM) cosmology is the so-called
`angular momentum problem'. This problem arises when we numerically model the collapse of baryons within a dark halo in the
CDM model. The formed baryonic disk has much less angular momentum than observed disk galaxies due to the considerable loss
of angular momentum during the progressive merger of small clumps. As a result of efficient radiative cooling, the gas component
collapses too deeply within the dark halo. When two such systems are merging, the angular momentum of the material near the
center is effectively transported outwards by the tidal force. This is a physical reason for this problem, however, there
may be a numerical origin due to the nature of the Smoothed Particle Hydrodynamics (SPH) method widely used in galaxy formation
models. To address the numerical origin of the `angular momentum problem' with a much higher-resolution SPH model, we are
developing our Parallel Tree-SPH code. After evolving four initial models with different mass and force resolution, we compare
the angular momentum content of SPH particles. We find that both mass and force resolutions clearly affect the evolution of
radiative cosmological SPH models. In most previous radiative cosmological SPH models, a mass ratio between SPH and dark matter
particles is
.However, we find that this mass ratio is a crucial parameter when we consider the angular momentum content of SPH particles
and it is better to make the mass ratio ∼ 1.0 in such models.
This revised version was published online in August 2006 with corrections to the Cover Date. |
| |
Keywords: | Hydrodynamics |
本文献已被 SpringerLink 等数据库收录! |
|