Pseudobulge formation in the Milky Way type galaxies as a result of buckling instability
Abstract
Two models of a disk galaxy, characterized by a classical bulge and the absence of a spiral structure at the beginning of the simulation, are numerically investigated. With similar rotation curves and bulges, one of the models turns out to be significantly more unstable to the formation of a bar, so that a noticeable bar is formed during 100 Myr. In the second model, the corresponding time is almost an order of magnitude longer — 700 Myr. On the background of a quickly formed bar, a secondary (buckling) instability occurs in the first model, leading to a sharp increase in the thickness of the bar. This thick bar can be associated with a pseudobulge. In the second model, the thickening of the bar occurs gradually.
- Publication:
-
INASAN Science Reports
- Pub Date:
- October 2019
- DOI:
- 10.26087/INASAN.2019.4.2.057
- Bibcode:
- 2019INASR...4..381S