Chemical evolution and abundance gradients in the Milky Way

Details Chemical evolution and abundance gradients in the Milky Way Chemical evolution and abundance gradients in the Milky Way

2001-07-02

arxiv.org/abs/astro-ph/0107016v1

Astronomy and Astrophysics

Astrophysics

16 pages, 11 figures, submitted to A&A

Scientific paper

We extend our model of chemical evolution that successfully account for the main observables in the solar neighborhood (Alibes, Labay & Canal 2001) to the whole Milky Way halo and disk. We assume an inside-out scenario for the assembling of the Galaxy through the infall of external material. Two different compositions of the infalling material have been considered: primordial and slightly metal-enriched (0.1 Z_{\sun}). Our calculations follow the evolution of 76 isotopes up to the Iron peak, but we only present here results for the elements having well-measured gradients: C, N, O, Ne, Mg, Al, Si, S, Ar and Fe. The calculated current radial distributions of these elements are compared with large samples of data from HII regions, B stars, planetary nebulae and open clusters. We also discuss the time evolution of the abundance gradients. Good fits are achieved with both infall compositions, closer to the observational data in the case of primordial infall. We show that contributions from intermediate-mass stars allow to reproduce the measured abundances of C and N, but the profiles of their ratios to oxygen leave still open the nucleosynthetic origin of these elements. In agreement with several previous works, our models predict a flattening with time of the abundance gradients, most of which taking place during the early galactic evolution.

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