paper

The Formation of a Disk Galaxy within a Growing Dark Halo

arXiv:astro-ph/0301499 · doi:10.1051/0004-6361:20021842

Abstract

We present a dynamical model for the formation and evolution of a massive disk galaxy, within a growing dark halo whose mass evolves according to cosmological simulations of structure formation. The galactic evolution is simulated with a new 3D chemo-dynamical code, including dark matter, stars and a multi-phase ISM. The simulations start at redshift z=4.85 with a small dark halo in a LCDM universe and we follow the evolution until the present epoch. The energy release by massive stars and SNe prevents a rapid collapse of the baryonic matter and delays the maximum star formation until z=1. The galaxy forms radially from inside-out and vertically from halo to disk. The first galactic component that forms is the halo, followed by the bulge, the disk-halo transition region, and the disk. At z=1, a bar begins to form which later turns into a triaxial bulge. There is a pronounced deficiency of low-metallicity disk stars due to pre-enrichment of the disk ISM with metal-rich gas from the bulge and inner disk (G-dwarf problem). The mean rotation and the distribution of orbital eccentricities for all stars as a function of metallicity are not very different from those observed in the solar neighbourhood, showing that homogeneous collapse models are oversimplified. The approach presented here provides a detailed description of the formation and evolution of an isolated disk galaxy in a LCDM universe, yielding new information about the kinematical and chemical history of the stars and the ISM, but also about the evolution of the luminosity, the colours and the morphology of disk galaxies.

23 pages, LaTeX, 18 figures, A&A accepted, a high resolution version of the paper can be found at http://www.astro.unibas.ch/leute/ms.shtml

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