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We present a comprehensive study of the abundance evolution of the elementsfrom H to U in the Milky Way halo and local disk. We use a consistent chemicalevolution model, metallicity dependent isotopic yields from low andintermediate mass stars and yields from massive stars which include, for thefirst time, the combined effect of metallicity, mass loss and rotation for alarge grid of stellar masses and for all stages of stellar evolution. Theyields of massive stars are weighted by a metallicity dependent function of therotational velocities, constrained by observations as to obtain a primary-like$^{14}$N behavior at low metallicity and to avoid overproduction of s-elementsat intermediate metallicities. We show that the solar system isotopiccomposition can be reproduced to better than a factor of two for isotopes up tothe Fe-peak, and at the 10\% level for most pure s-isotopes, both light ones(resulting from the weak s-process in rotating massive stars) and the heavyones (resulting from the main s-process in low and intermediate mass stars). Weconclude that the light element primary process (LEPP), invoked to explain theapparent abundance deficiency of the s-elements with A< 100, is not necessary.We also reproduce the evolution of the heavy to light s-elements abundanceratio ([hs/ls]) - recently observed in unevolved thin disk stars - as a resultof the contribution of rotating massive stars at sub-solar metallicities. Wefind that those stars produce primary F and dominate its solar abundance and weconfirm their role in the observed primary behavior of N. In contrast, we showthat their action is insufficient to explain the small observed values ofC12/C13 in halo red giants, which is rather due to internal processes in thosestars.

Chemical evolution with rotating massive star yields: I. The solar neighbourhood and the s-process elements