The Karlsruhe Astrophysical Database of Nucleosynthesis in Stars Project - Status and Prospects

@article{Dillmann2014TheKA,
  title={The Karlsruhe Astrophysical Database of Nucleosynthesis in Stars Project - Status and Prospects},
  author={Iris Dillmann and Tam'as Szucs and Zs. Fulop and Ralf Plag and Franz Kappeler and Thomas Rauscher},
  journal={Nuclear Data Sheets},
  year={2014},
  volume={120},
  pages={171-174}
}

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References

SHOWING 1-10 OF 61 REFERENCES
KADoNiS‐ The Karlsruhe Astrophysical Database of Nucleosynthesis in Stars
The “Karlsruhe Astrophysical Database of Nucleosynthesis in Stars” (KADoNiS) project is an online database for experimental cross sections relevant to the s process and p process. It is available
NEUTRON CROSS SECTIONS FOR NUCLEOSYNTHESIS STUDIES
Previous compilations of (n, gamma) cross sections of relevance for neutron capture nucleosynthesis in the big bang and in the slow neutron capture process (s process) have been updated to encompass
Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data.
TLDR
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.
OPPORTUNITIES TO CONSTRAIN ASTROPHYSICAL REACTION RATES FOR THE s-PROCESS VIA DETERMINATION OF THE GROUND-STATE CROSS-SECTIONS
Modern models of s-process nucleosynthesis in stars require stellar reaction rates of high precision. Most neutron-capture cross-sections in the s-process have been measured, and for an increasing
Suppression of the stellar enhancement factor and the reaction 85Rb(p,n)85Sr
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
Neutron capture cross section of unstable 63Ni: implications for stellar nucleosynthesis.
TLDR
Stellar model calculations for a 25M⊙ star show that the new data have a significant effect on the s-process production of 63Cu, 64Ni, and 64Zn in massive stars, allowing stronger constraints on the Cu yields from explosive nucleosynthesis in the subsequent supernova.
Astrophysical reaction rates from statistical model calculations
Theoretical reaction rates in the temperature range 0.01 x 10(9) less than or equal to T(K) less than or equal to 10.0 x 10(9) are calculated in the statistical model (Hauser-Feshbach formalism) for
Critical Reactions in Contemporary Nuclear Astrophysics
Nuclear reaction rates play a critical role in the understanding of stellar evolution and explosions. However, in many cases nuclear reaction rates still carry large uncertainties due to the paucity
...
...