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SPH simulations of the chemical evolution of bulges

Published online by Cambridge University Press:  01 July 2007

F. J. Martínez-Serrano ,
R. Domínguez-Tenreiro  and
M. Mollá
F. J. Martínez-Serrano
Affiliation:
Depto. de Física y A.C., Univ. Miguel Hernández, 03206 Elche, Alicante, Spain
R. Domínguez-Tenreiro
Affiliation:
Depto. de Física Teórica, Univ. Autónoma de Madrid, 28040 Cantoblanco, Madrid, Spain
M. Mollá
Affiliation:
Depto. de Investigación Básica, C.I.E.M.A.T., Avda. Complutense 22, 28040 Madrid, Spain
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Abstract

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We have implemented a chemical evolution model on the parallel AP3M+SPH DEVA code which we use to perform high resolution simulations of spiral galaxy formation. It includes feedback by SNII and SNIa using the Qij matrix formalism. We also include a diffusion mechanism that spreads newly introduced metals. The gas cooling rate depends on its specific composition. We study the stellar populations of the resulting bulges finding a potential scenario where they seem to be composed of two populations: an old, metal poor, α-enriched population, formed in a multiclump scenario at the beginning of the simulation and a younger one, formed by slow accretion of satellites or gas, possibly from the disk due to instabilities.

Keywords

galaxies: abundancesgalaxies: formationgalaxies: bulgesmethods: n-body simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 35 - 36
Copyright
Copyright © International Astronomical Union 2008

References

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