Abstract
Nucleosynthesis theory predicts that half of the chemical elements above Fe are formed in explosive stellar scenarios by the r-process. A correct modelling of this process requires knowledge of nuclear properties very far from stability and a detailed description of the astrophysical environments. Using updated experimental and theoretical nuclear-physics data, we have performed detailed r-process calculations within the classical, site-independent “waiting-point” approximation and the “neutrino-wind” scenario of core-collapse type II supernovae (SNII). Nuclear and astrophysical constraints on the reproduction of the available r-process observables will be reviewed.
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