Quantifying the uncertainties of chemical evolution studies. I. The stellar initial mass function and the stellar lifetimes

Details Quantifying the uncertainties of chemical evolution studies. I. The stellar initial mass function and the stellar lifetimes Quantifying the uncertainties of chemical evolution studies. I. The stellar initial mass function and the stellar lifetimes

2004-09-20

arxiv.org/abs/astro-ph/0409473v1

Astronomy and Astrophysics

Astrophysics

18 pages, 10 figures, accepted for publication in Astronomy and Astrophysics

Scientific paper

The stellar initial mass function and the stellar lifetimes are basic ingredients of chemical evolution models, for which different recipes can be found in the literature. In this paper, we quantify the effects on chemical evolution studies of the uncertainties in these two parameters. We concentrate on chemical evolution models for the Milky Way, because of the large number of good observational constraints. Such chemical evolution models have already ruled out significant temporal variations for the stellar initial mass function in our own Galaxy, with the exception perhaps of the very early phases of its evolution. Therefore, here we assume a Galactic initial mass function constant in time. Through an accurate comparison of model predictions for the Milky Way with carefully selected data sets, it is shown that specific prescriptions for the initial mass function in particular mass ranges should be rejected. As far as the stellar lifetimes are concerned, the major differences among existing prescriptions are found in the range of very low-mass stars. Because of this, the model predictions widely differ for those elements which are produced mostly by very long-lived objects, as for instance 3He and 7Li. However, it is concluded that model predictions of several important observed quantities, constraining the plausible Galactic formation scenarios, are fairly robust with respect to changes in both the stellar mass spectrum and the stellar lifetimes. For instance, the metallicity distribution of low-mass stars is nearly unaffected by these changes, since its shape is dictated mostly by the time scale for thin-disk formation.

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