出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：Slow neutron capture reactions in massive stars are substantially contributing to the abundances of
the elements between Fe and Zr, producing the so-called weak s component. The weak s process
is characterized by a low neutron exposure, where the reaction flow does not reach equilibrium
conditions. As a consequence, uncertainties in the stellar (n,γ ) rates give rise to large propagation
effects. This is illustrated by the impact of recently improved experimental cross sections.
Massive stars are also the main production site of the unstable isotope 60Fe, which provides an
important chronometer for the early solar system. The successful measurement of the stellar
(n,γ ) cross section of 60Fe represents an important step towards a quantitative determination of
the s-process origin of 60Fe in massive stars.
