Chemical evolution with rotating massive star yields II. A new
  assessment of the solar s- and r- process components
  The decomposition of the Solar system abundances of heavy isotopes into their
s- and r- components plays a key role in our understanding of the corresponding
nuclear processes and the physics and evolution of their astrophysical sites.
We present a new method for determining the s- and r- components of the Solar
system abundances, fully consistent with our current understanding of stellar
nucleosynthesis and galactic chemical evolution. The method is based on a study
of the evolution of the solar neighborhood with a state-of-the-art 1-zone
model, using recent yields of low and intermediate mass stars as well as of
massive rotating stars. We compare our results with previous studies and we
provide tables with the isotopic and elemental contributions of the s- and
r-processes to the Solar system composition.
