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By adopting a chemical evolution model for the Milky Way already reproducingthe evolution of several chemical elements, we compare our theoretical resultswith accurate and new stellar data of neutron capture elements and we are ableto impose strong constraints on the nucleosynthesis of the studied elements. Wecan suggest the stellar sites of production for each element. In particular,the r-process component of each element (if any) is produced in the mass rangefrom 10 to 30 Msun, whereas the s-process component arises from stars in therange from 1 to 3 Msun. Using the same chemical evolution model, extended todifferent galactocentric distances, we obtain results on the radial gradientsof the Milky Way. We compare the results of the model not only for the neutroncapture elements but also for alpha-elements and iron peak elements with newdata of Cepheids stars. We give a possible explanation to the considerablescatter of neutron capture elements observed in low metallicity stars in thesolar vicinity, compared to the small star to star scatter observed for thealpha-elements. In fact, we have developed a stochastic chemical evolutionmodel, in which the main assumption is a random formation of new stars, subjectto the condition that the cumulative mass distribution follows a given initialmass function. With our model we are able to reproduce the different featuresof neutron capture elements and alpha-elements. Finally, we test theprescriptions for neutron capture elements also for the dwarf spheroidalgalaxies of the Local Group. We predict that the chemical evolution of theseelements in dwarf spheroidal galaxies is different from the evolution in thesolar vicinity and indicates that dwarf spheroidal galaxies (we see nowadays)cannot be the building blocks of our Galaxy.

Chemical evolution of neutron capture elements in our Galaxy and in the dwarf spheroidal galaxies of the Local Group