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Using the stellar evolution code Kepler, which includes a fu ll adaptive nuclear reaction network, we have performed calculations of neutrino driven winds fro m the surface of protoneutron stars which include hydrodynamics, all strong processes, and all weak processes of importance. In this environment, neutrino interactions push the material in th e wind to high entropies and at later times weak charged current interactions tend to reduce the e lectron fraction to values possibly favorable for an r-process. We have also included time depen dent neutrino luminosities and energies so as to follow the evolution of the wind from the proto n rich stage through the neutron rich stage to calculate integrated nucleosynthetic yields . Here, we report preliminary results of our calculations and discuss future directions for this wor k.

Nucleosynthesis in the Neutrino Driven Wind of Protoneutron Stars