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Metal-rich infall onto the inner disk through the interaction between bulge winds and gaseous halos

Published online by Cambridge University Press:  09 March 2010

Takuji Tsujimoto  and
Kenji Bekki
Takuji Tsujimoto
Affiliation:
National Astronomical Observatory, Mitaka-shi, Tokyo 181-8588, Japan email: [email protected]
Kenji Bekki
Affiliation:
School of Physics, University of New South Wales, Sydney 2052, NSW, Australia email: [email protected]
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Abstract

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We demonstrate for the first time that gaseous halos of disk galaxies can play a vital role in recycling metal-rich gas ejected from the bulges and thus in promoting the chemical evolution of the disks. Our numerical simulations show that metal-rich bulge winds can be accreted onto the thin disks owing to hydrodynamical interaction between the gaseous ejecta and the gaseous halos. Accordingly, we anticipate that chemical abundances of the inner disk stars are significantly influenced by the enriched winds. About ~1% of gaseous ejecta from the bulges can be accreted onto the middle disk corresponding to the sun's position. We discuss these results in the context of the origin of super metal-rich stars in the solar neighborhood as well as an observed flattening of the abundance gradient in the Galactic disk.

Keywords

Galaxy: bulgeGalaxy: diskGalaxy: evolutionstars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 384 - 385
Copyright
Copyright © International Astronomical Union 2010

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