Document 
- Same authors
-
Related articles
- Recommend this article
- Download citation
- Alert me when this article is cited
- Alert me when this article is corrected
BibSonomy
CiteUlike
Connotea
Del.icio.us
Digg
Facebook
|
A&A 481, 651-659 (2008)
DOI: 10.1051/0004-6361:20078285
Star formation and bar instability in cosmological halos
A. Curir1, P. Mazzei2, and G. Murante11 INAF - Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Torino, Italy
e-mail: curir@oato.inaf.it
2 INAF - Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy
(Received 16 July 2007 / Accepted 1 February 2008)
Abstract
Context. This is the third in a series of papers presenting the first attempt to
analyse the growth of the bar instability in a consistent cosmological
scenario. In the previous two articles, we explored the role of the cosmology
on stellar disks and the impact of the gaseous component on a disk embedded
in a cosmological dark matter halo.
Aims. The aim of this paper is to point out the impact of the star
formation on the bar instability inside disks having different gas
fractions.
Methods. We performed cosmological simulations of the same disk-to-halo mass systems
as in the previous works where the star formation was not triggered. We
compared the results of the new simulations with the previous ones to
investigate the effect of the star formation by analysing the morphology of the
stellar components,
the bar strength, the behaviour of the pattern speed. We followed the gas and
the central mass concentration during the evolution and their impact on the
bar strength.
Results. A stellar bar, lasting 10 Gyr,
is still living at z=0 in all our cosmological simulations.
The central mass concentration of gas and of the new stars has a mild effect
on the ellipticity of the bar but is not able to destroy it, and at z=0 the
stellar bar strength is enhanced by the star formation.
The bar pattern speed decreases with the disk evolution.
Key words: galaxies: spiral -- galaxies: structure -- galaxies: evolution -- galaxies: halos -- galaxies: kinematics and dynamics
© ESO 2008
| What is OpenURL? |
