Suppression of the stellar enhancement factor and the reaction 85Rb(p,n)85Sr

  title={Suppression of the stellar enhancement factor and the reaction 85Rb(p,n)85Sr},
  author={Thomas Rauscher and G{\'a}bor Gyula Kiss and Gy. Gyurky and A. Simon and Zs. Fulop and E. Somorjai},
  journal={Physical Review C},
Astrophysical reaction rates are central to tracing changes in the abundances of nuclei by nuclear reactions. They provide the temperature- and density-dependent coefficients entering reaction networks, the large sets of coupled differential equations required to study nucleosynthesis and energy generation in astrophysical environments. The reaction rates are computed from reaction cross sections which, in turn, may be predicted in theoretical models or extracted from experiments. In addition… 
General properties of astrophysical reaction rates in explosive nucleosynthesis
Fundamental differences in the prediction of reaction rates with intermediate and heavy target nuclei compared to the ones with light nuclei are discussed, with special emphasis on stellar
Challenges in nucleosynthesis of trans-iron elements
Nucleosynthesis beyond Fe poses additional challenges not encountered when studying astrophysical processes involving light nuclei. Astrophysical sites and conditions are not well known for some of
The path to improved reaction rates for astrophysics
This review focuses on nuclear reactions in astrophysics and, more specifically, on reac- tions with light ions (nucleons andparticles) proceeding via the strong interaction. It is intended to
Sensitivity of Astrophysical Reaction Rates to Nuclear Uncertainties
Sensitivities of nuclear reaction rates to a variation of nuclear properties are studied. Target nuclei range from proton- to neutron dripline for 10 ≤ Z ≤ 83. Reactions considered are nucleon- and
Alpha-induced reaction cross section measurements on $^{151}$Eu for the astrophysical $\gamma$-process
In order to extend the experimental database relevant for the astrophysical -process towards the unexplored heavier mass region, the cross sections of the 151 Eu(�,) 155 Tb and 151 Eu(�,n) 154 Tb
Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data.
The main part of the review focuses on the nuclear uncertainties involved in the determination of the astrophysical reaction rates required for the extended reaction networks used in nucleosynthesis studies.
Origin of the p-Nuclei in Explosive Nucleosynthesis
A number of naturally occurring, proton-rich nuclides (the p-nuclei) cannot be made in the s- and r-process. It has been found that massive stars can produce p-nuclei through photodisintegration of
Systematic Study Of (p,γ) Reactions On Ni Isotopes
A systematic study of the radiative proton capture reaction for all stable nickel isotopes is presented. The results were obtained using 2.0–6.0 MeV protons from the 11-MV tandem Van de Graaff


Nuclear physics of stars
Preface. 1 Aspects of Nuclear Physics and Astrophysics. 1.1 History. 1.2 Nomenclature. 1.3 Solar System Abundances. 1.4 Astrophysical Aspects. 1.4.1 General Considerations. 1.4.2 Hertzsprung-Russell
Stellar Evolution
Stellar EvolutionAn Exploration from the Observatory. By Otto Struve. Pp. xiv + 266 + 17 plates. (Princeton, N.J.: Princeton University Press; London: Oxford University Press, 1950.) 25s. net.
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