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The decomposition of the Solar system abundances of heavy isotopes into theirs- and r- components plays a key role in our understanding of the correspondingnuclear processes and the physics and evolution of their astrophysical sites.We present a new method for determining the s- and r- components of the Solarsystem abundances, fully consistent with our current understanding of stellarnucleosynthesis and galactic chemical evolution. The method is based on a studyof the evolution of the solar neighborhood with a state-of-the-art 1-zonemodel, using recent yields of low and intermediate mass stars as well as ofmassive rotating stars. We compare our results with previous studies and weprovide tables with the isotopic and elemental contributions of the s- andr-processes to the Solar system composition.

Chemical evolution with rotating massive star yields II. A new assessment of the solar s- and r- process components