6533b7d7fe1ef96bd1268d2d

RESEARCH PRODUCT

The Astrophysical r-process

subject

description

In 1957, Burbidge, Burbidge, Fowler and Hoyle (B2FH) provided a basis for forty years of research in various aspects of nucleosynthesis in stars. We will focus in this paper on progress in r-process nucleosynthesis, with emphasis on the most recent developments in nuclear physics. In 1986, the first experimental data on two crucial, neutron-magic “waiting-point” nuclei provided valuable clues to the astrophysical conditions and the nature of the r-process site. Beginning in the 1990’s, our group (FK2L) presented considerably improved r-abundance calculations, which were for the first time based on a modern, internally consistent nuclear-theory input. The phenomenon of shell-quenching far from β-stability required at that time seems to become evident by now. This new nuclear-structure phenomenon leads to improved predictions of astrophysical observables like the solar-system isotopic r-abundances (Nr,⊙) or the recently observed abundances of ultra-metal-poor halo stars.