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

  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},

Figures from this paper

Determination of Solar System R-Process Abundances using ENDF/B-VIII.0 and TENDL-2015 libraries
Recent multi-messenger detection of the binary neutron star merger (GW170817) energized the astrophysical community and encouraged further research for determination of nuclear physics observables.
Heavy elements nucleosynthesis on accreting white dwarfs: building seeds for the p-process
The origin of the proton-rich trans-iron isotopes in the solar system is still uncertain. Single-degenerate thermonuclear supernovae (SNIa) with n-capture nucleosynthesis seeds assembled in the
Determination of the photodisintegration reaction rates involving charged particles: Systematic calculations and proposed measurements based on the facility for Extreme Light Infrastructure–Nuclear Physics
Photodisintegration reaction rates involving charged particles are of relevance to the p-process nucleosynthesis that aims at explaining the production of the stable neutron-deficient nuclides
Explosive Nucleosynthesis: What We Learned and What We Still Do Not Understand
This review touches on historical aspects, going back to the early days of nuclear astrophysics, initiated by B\(^2\)FH and Cameron, discusses (i) the required nuclear input from reaction rates and
Prospects for direct neutron capture measurements on s-process branching point isotopes
Abstract.The neutron capture cross sections of several unstable key isotopes acting as branching points in the s -process are crucial for stellar nucleosynthesis studies, but they are very
Chemical evolution with rotating massive star yields II. A new assessment of the solar s- and r- process components
The decomposition of the Solar system abundances of heavy isotopes into their s- and r- components plays a key role in our understanding of the corresponding nuclear processes and the physics and
Presolar Grain Isotopic Ratios as Constraints to Nuclear and Stellar Parameters of Asymptotic Giant Branch Star Nucleosynthesis
Recent models for evolved low-mass stars (with M ≲ 3 M ⊙), undergoing the asymptotic giant branch (AGB) phase assume that magnetic flux-tube buoyancy drives the formation of 13C reservoirs in He-rich
Measurement of the 72Ge(n,γ) cross section over a wide neutron energy range at the CERN n_TOF facility
The 72 Ge( n ,γ ) cross section was measured for neutron energies up to 300 keV at the neutron time-of-flight facility n_TOF (CERN), Geneva, for the first time covering energies relevant to


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
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.
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.
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.
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.
Stellar (n,gamma) cross section of 62Ni.
The total cross section of the 62Ni(n,gamma)63Ni(t(1/2)=100+/-2 yr) reaction for a quasi-Maxwellian (kT=25 keV) neutron flux is measured for the first time.
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