The p-process of stellar nucleosynthesis is aimed at explaining the production of the stable
neutron-deficient nuclides heavier than iron that are observed up to now in the solar system …

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 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 …

Optical-model potentials (OMPs) continue to play a key role in nuclear reaction calculations.
However, the uncertainty of phenomenological OMPs in widespread use—inherent to any …

The Cd 106 (α, γ) Sn 110 reaction cross section has been measured in the energy range of
the Gamow window for the astrophysical p-process scenario. The cross sections for Cd 106 …

The cross section of the 88 Sr (p, γ) 89 Y reaction was determined by in-beam
measurements at energies E p= 1.4–5 MeV relevant to the nucleosynthetic p process. At E …

The cross section of the reaction Sn 112 (α, γ) Te 116 has been measured in the energy
range of astrophysical interest for the p-process. Highly enriched self-supporting Sn 112 foils …

Experimental isomeric ratios of light (A≤ 4) particle-induced nuclear reactions were
compiled for the product nuclides having metastable states with half-lives longer than 0.1 s …

Photon-induced reactions play a key role in the nucleosynthesis of rare neutron-deficient p-
nuclei. The paper focuses on (γ,α), (γ,\rmp), and (γ,\rmn) reactions which define the …

In beam angle-integrated cross section measurements of the Y 89 (p, γ) Zr 90 reaction were
carried out at E p= 1.7–4.8 MeV by using a 4 π NaI (Tl) summing detector. The resulting …