Radial migration in barred galaxies. (5th March 2015)

• Record Type: Journal Article
• Authors: Di Matteo, P.; Haywood, M.; Combes, F.; Semelin, B.; Babusiaux, C.; Gomez, A.
• Editors: Montmerle, Thierry
• Is Part Of: Proceedings of the International Astronomical Union. Volume 10:Number H16(2012)Highlights
• Page Start: 355
• Page End: 355
• Publication Date: 2015-03-05
• Subjects: Galaxies: abundances, -- Galaxies: evolution, -- Galaxies: dynamics; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921314011272
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: 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).