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Metallicity gradients in the Milky Way

Published online by Cambridge University Press:  09 March 2010

Walter J. Maciel  and
Roberto D. D. Costa
Walter J. Maciel
Affiliation:
University of São Paulo, Astronomy Department, Rua do Matão 1226, Cidade Universitária, São Paulo SP, CEP 05509-0900, Brazil email: maciel@astro.iag.usp.br, roberto@astro.iag.usp.br
Roberto D. D. Costa
Affiliation:
University of São Paulo, Astronomy Department, Rua do Matão 1226, Cidade Universitária, São Paulo SP, CEP 05509-0900, Brazil email: maciel@astro.iag.usp.br, roberto@astro.iag.usp.br
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Abstract

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Radial metallicity gradients are observed in the disks of the Milky Way and in several other spiral galaxies. In the case of the Milky Way, many objects can be used to determine the gradients, such as HII regions, B stars, Cepheids, open clusters and planetary nebulae. Several elements can be studied, such as oxygen, sulphur, neon, and argon in photoionized nebulae, and iron and other elements in cepheids, open clusters and stars. As a consequence, the number of observational characteristics inferred from the study of abundance gradients is very large, so that in the past few years they have become one of the main observational constraints of chemical evolution models. In this paper, we present some recent observational evidences of abundance gradients based on several classes of objects. We will focus on (i) the magnitude of the gradients, (ii) the space variations, and (iii) the evidences of a time variation of the abundance gradients. Some comments on recent theoretical models are also given, in an effort to highlight their predictions concerning abundance gradients and their variations.

Keywords

stars: abundancesISM: abundancesphotoionized nebulaeGalaxy: 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. 317 - 324
Copyright
Copyright © International Astronomical Union 2010

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