Quantitative Estimate of the Reaction Dependence of the R-Process Nucleosynthesis

Details Quantitative Estimate of the Reaction Dependence of the R-Process Nucleosynthesis Quantitative Estimate of the Reaction Dependence of the R-Process Nucleosynthesis

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..517s&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Astronomy and Astrophysics

Astrophysics

Scientific paper

Very massive stars ≥ 8M&sun; culminate their evolution by supernova (SN) explosions which are presumed to be most viable candidate for the astrophysical site of heavy r-process nucleosynthesis. In an explosive circumstances of the neutrino-driven winds in gravitational core-collapse Type II SNe, not only heavy neutron-rich nuclei but also light unstable nuclei play the significant roles. We first studied in this article the efficiency and sensitivity of the SN r-process nucleosynthesis to many relevant nuclear reaction rates. Our adopted theoretical method and formulae are very effective, and their successful power has already been established in theoretical studies of the missing solar neutrino problem. We also adopted two different models of the neutrino-driven winds in order to study the dependence of our result on wind models. In this study we found quantitatively that several specific nuclear reactions on light neutron-rich nuclei take very critical keys to the final nucleosynthesis yields of r-process elements [1]. Our numerical result of the sensitivity analysis emphasizes and motivates the importance of future experiments aimed at unambiguously determining the nuclear reaction rates that most strongly affect the SN r-process abundance. It would in turn serve to constrain physical and environmental conditions for successful r-process nucleosynthesis in exploding Type II SNe.

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