An Update on the Hot Supernova Bubble R-Process

The neutrino-energized high-entropy bubble above the proto neutron star in a core-collapse supernova remains as one of the most promising sites for r-process nucleosynthesis. In this paper we briefly summarize the appealing features of this model along with its remaining difficulties. We present some new approaches to their resolution. In particular, we show first results from a new version of with Livermore supernova code with improved neutrino transport and numerics. Very high entropy per baryon (s/k ~ 600) appears within the bubble at late times. Though favorable for the r-process, seed nuclei are still over produced when neutrino-nucleus interactions are included. Even so, encouraging new results from the effects of magnetic fields, neutrino oscillations, and better nuclear physics input data are discussed.