https://www.cns.s.u-tokyo.ac.jp/~shimoura/research/nuc_data/pdf/11.pdf

Energy levels of light nuclei A = 11-12

Energy levels of light nuclei A = 16-17

: Nucleosynthesis of elements heavier than the iron group by neutron capture on both slow and fast time scales is evaluated. The s-process calculations of Clayton, Fowler, Hull, and Zimmerman (Ann. Phys. 12:331, 1961) were revised to include more recent experimental results on abundances and neutron capture cross-sections. The solar-system s-process abundances indicate a history of neutron exposure distributions characterized by decreasing probability of high integrated flux; an exponential exposure distribution is extracted. Estimates are made of the s-process contribution to each isotopic abundance; a table gives the amounts of elements produced by each process in the solar-system material. The r-process calculations are carried out using a semi-empirical atomic-mass law to determine neutron-binding energies and beta-decay probabilities. The solar-system r-process material has probably been synthesized in two distinct types of environments. (Author)

/pdf/nucleosynthesis-of-heavy-elements-by-neutron-capture-5ezmnk0fbn.pdf

Nucleosynthesis of Heavy Elements by Neutron Capture

Energy levels of light nuclei, A = 20

Effects of electron screening on the 3He(d, p)4He low-energy cross sections

The review describes the current status of nuclear astrophysics, where special emphasis is given to primordial and stellar nucleosynthesis of the chemical elements. The laboratory approaches in obtaining relevant reaction rates are discussed. The authors also focus attention on those processes where new knowledge of nuclear physics may have important astrophysical consequences. The major burning phases in stars and some critical reactions are discussed. Finally, miscellaneous topics of current interest are described.

https://iopscience.iop.org/article/10.1088/0034-4885/50/3/001/pdf

W S Rodney

Papers

Current status of nuclear astrophysics