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Impact of radial migration on the chemical evolution of the Milky Way disk

Published online by Cambridge University Press:  17 July 2015

N. Prantzos ,
M. Kubryk  and
E. Athanassoula
N. Prantzos
Affiliation:
Sorbonne Universités, UPMC Paris 6, and CNRS, UMR 7095, Institut d'Astrophysique de Paris, France
M. Kubryk
Affiliation:
Sorbonne Universités, UPMC Paris 6, and CNRS, UMR 7095, Institut d'Astrophysique de Paris, France
E. Athanassoula
Affiliation:
Laboratoire d'Astrophysique de Marseille, OAMP, France
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Abstract

We study the role of radial migration of stars on the chemical evolution of the Milky Way disk with a 1D semi-analytical disk model. We describe radial migration with parametrised time- and radius-dependent diffusion coefficients, based on the analysis of a N-body+SPH simulation of a disk galaxy (analyzed by Kubryk et al. 2013). Our model reproduces well the present day values of most of the main global observables of the MW. Assuming that the thick disk is the oldest (>9 Gyr) part of the disk, we find that the adopted radial migration scheme can reproduce quantitatively the main local properties of the thin and thick disk: metallicity-distributions, dispersion in age-metallicity relation, “two-branch” behaviour in the O/Fe vs. Fe/H relation, local surface densities of stars, etc..

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 68: The Milky Way Unravelled by Gaia: GREAT Science from the Gaia Data Releases , 2014 , pp. 137 - 140
Copyright
© EAS, EDP Sciences, 2015

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