Neutron captures produce the vast majority of abundances of elements heavier than iron in
the Universe. Beyond the classical slow (s) and rapid (r) processes, there is observational …

Nucleosynthesis in the s process takes place in the He-burning layers of low-mass
asymptotic giant branch (AGB) stars and during the He-and C-burning phases of massive …

The slow neutron capture process in massive stars (weak s process) produces most of the s-
process isotopes between iron and strontium. Neutrons are provided by the 22 Ne (α, n) 25 …

A small number of naturally occurring, proton-rich nuclides (the p-nuclei) cannot be made in
the s-and r-processes. Their origin is not well understood. Massive stars can produce p …

The quest for the origin of matter in the Universe had been the subject of philosophical and
theological debates over the history of mankind, but quantitative answers could be found …

Accelerator mass spectrometry (AMS) was born in the late 1970s, when it was realized at
nuclear physics laboratories that the accelerator systems can be used as a sensitive mass …

The astrophysical p-process, which is responsible for the origin of the proton-rich stable
nuclei heavier than iron, was investigated using a full nuclear reaction network for a Type II …

The primary aim of experimental nuclear astrophysics is to determine the rates of nuclear
reactions taking place in stars in various astrophysical conditions. These reaction rates are …

Neutron capture cross sections are one of the most important nuclear inputs to models of
stellar nucleosynthesis of the elements heavier than iron. The activation technique and the …

We have calculated the Maxwellian-averaged cross sections and astrophysical reaction
rates of the stellar nucleosynthesis reactions (n, γ),(n, fission),(n, p),(n, α), and (n, 2n) using …