r-Process Nucleosynthesis in the Hot Supernova Bubble: Revisited

Details r-Process Nucleosynthesis in the Hot Supernova Bubble: Revisited r-Process Nucleosynthesis in the Hot Supernova Bubble: Revisited

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dnp.dc015m&link_type=abstract

American Physical Society, Division of Nuclear Physics Meeting, 27-30 October, 2004, Chicago, IL. MEETING ID: DNP04., abstract #

Physics

Nuclear Physics

Scientific paper

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. Recent studies, however have pointed out that neutrino interactions with material in the expanding bubble limit the production of heavy nuclei by decreasing the neutron to seed ratio. In this paper we briefly summarize 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. Moreover, we show that the deleptonization and contraction of the core at very late times (t ≈ 30 s post bounce) leads to a high electron anti-neutrino energy. This makes for efficient neutron production and a robust r-process at late times even when other neutrino interactions are included.

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