| |
 |
| Paper: |
Formation Models of the Galactic Bulge |
| Volume: |
491, Fifty Years of Wide Field Studies in the Southern Hemisphere: Resolved Stellar Populations in the Galactic Bulge and the Magellanic Clouds |
| Page: |
169 |
| Authors: |
Gerhard, O. |
| Abstract: |
The Galactic bulge is now considered to be the inner
three-dimensional part of the Milky Way's bar. It has a peanut shape
and is characterized by cylindrical rotation. In N-body simulations,
box/peanut bulges arise from disks through bar and buckling
instabilities. Models of this kind explain much of the structure and
kinematics of the Galactic bulge and, in principle, also its
vertical metallicity gradient. Cosmological disk galaxy formation
models with high resolution and improved feedback models are now
able to generate late-type disk galaxies with disk-like or barred
bulges. These bulges often contain an early collapse stellar
population and a population driven by later disk instabilities. Due
to the inside-out disk formation, these bulges can be predominantly
old, similar to the Milky Way bulge. |
|
|
|
|
|
