Hostname: page-component-76fb5796d-zzh7m Total loading time: 0 Render date: 2024-04-25T10:57:54.938Z Has data issue: false hasContentIssue false
  • English
  • Français

Radial migration in barred galaxies

Published online by Cambridge University Press:  05 March 2015

P. Di Matteo ,
M. Haywood ,
F. Combes ,
B. Semelin ,
C. Babusiaux  and
A. Gomez
P. Di Matteo
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: paola.dimatteo@obspm.fr
M. Haywood
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: paola.dimatteo@obspm.fr
F. Combes
Affiliation:
LERMA, CNRS, UPMC, Observatoire de Paris, 61 Avenue de l'Observatoire, 75014 Paris, France
B. Semelin
Affiliation:
LERMA, CNRS, UPMC, Observatoire de Paris, 61 Avenue de l'Observatoire, 75014 Paris, France
C. Babusiaux
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: paola.dimatteo@obspm.fr
A. Gomez
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France email: paola.dimatteo@obspm.fr
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this talk, I will present the result of high resolution numerical simulations of disk galaxies with various bulge/disk ratios evolving isolated, showing that:

  • • Most of migration takes place when the bar strength is high and decreases in the phases of low activity (in agreement with the results by Brunetti et el. 2011, Minchev et al. 2011).

  • • Most of the stars inside the corotation radius (CR) do not migrate in the outer regions, but stay confined in the inner disk, while stars outside CR can migrate either inwards or outwards, diffusing over the whole disk.

  • • Migration is accompanied by significative azimuthal variations in the metallicity distribution, of the order of 0.1 dex for an initial gradient of ~-0.07 dex/kpc.

  • • Boxy bulges are an example of stellar structures whose properties (stellar content, vertical metallicity, [α/Fe] and age gradients, ..) are affected by radial migration (see also Fig. 1).

Keywords

Galaxies: abundancesGalaxies: evolutionGalaxies: dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 355
Copyright
Copyright © International Astronomical Union 2015 

References

Brunetti, M., Chiappini, C., & Pfenniger, D. 2011, A&A 534, 75Google Scholar
Minchev, I., et al. 2011, A&A 527, 147Google Scholar