Complete nucleosynthesis calculations for low−mass stars from NuGrid

Many nucleosynthesis and mixing processes of low−mass stars as they evolve from the Main Sequence to the thermal-pulse Asymptotic Giant Branch phase (TP−AGB) are well understood (although of course important physics components, e.g. rotation, magnetic fields, gravity wave mixing, remain poorly known). Nevertheless, in the last years presolar grain measurements with high resolution have presented new puzzling problems and strong constraints on nucleosynthesis processes in stars. The goal of the NuGrid collaboration is to pr esent uniform yields for a large range of masses and metallicities, including low−mass stars and massive stars and their explosions. Here we present the first calculations of stellar evolution a nd high−resolution, post−processing simulations of an AGB star with an initial mass of 2 M⊙ and solar−like metallicity (Z=0.01), based on the post−processing code PPN. In particular, we analyze the formation and evolution of the radiative 13 C−pocket between the 17th TP and the 18th TP. The s-process nucleosynthesis profile of a sample of heavy isotopes is also discussed, befor e the next convective TP occurrence.