Abstract
While the origin of r -process nuclei remains a long-standing mystery, recent spectroscopic studies of extremely metal-poor stars in the Galactic halo strongly suggest that it is associated with core-collapse supernovae. In addition, recent comprehensive analysis of such stars implies the presence of the “weak” r -process that is responsible for only lighter nuclei with A r -process nuclei can be produced in the neutrino winds from a typical proto-neutron star of $1.4 M_\odot$ . This suggests that the significant fraction of weak r -process elements (Sr, Y, Zr, etc.) originate from typical core-collapse supernovae with the progenitor mass range of ∼ 10– $20 M_\odot$
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