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S-process studies in the light of new experimental cross sections - Distribution of neutron fluences and r-process residuals
Kaeppeler, F.; Beer, H.; Wisshak, K.; Clayton, D. D.; Macklin, R. L.; Ward, R. A.
AA(Kernforschungszentrum Karlsruhe GmbH, Karlsruhe, Germany), AB(Kernforschungszentrum Karlsruhe GmbH, Karlsruhe, Germany), AC(Kernforschungszentrum Karlsruhe GmbH, Karlsruhe, Germany), AD(Max-Planck-Institut für Kernphysik, Heidelberg, Germany; Rice University, Houston, TX), AE(Oak Ridge National Laboratory, Oak Ridge, TN), AF(Max-Planck-Institut für Physik und Astrophysik, Munich, Germany)
Astrophysical Journal, Part 1, vol. 257, June 15, 1982, p. 821-846. (ApJ Homepage)
Publication Date:
Nuclear and High-Energy Physics
NASA/STI Keywords:
Absorption Cross Sections, Neutron Cross Sections, Neutron Irradiation, Nuclear Fusion, Nuclei (Nuclear Physics), Red Giant Stars, Abundance, Branching (Physics), Fluence, Flux (Rate), Isotopes, Maxwell-Boltzmann Density Function, Stellar Envelopes, Stellar Models
Bibliographic Code:


A best set of neutron-capture cross sections has been evaluated for the most important s-process isotopes. With this data base, s-process studies have been carried out using the traditional model which assumes a steady neutron flux and an exponential distribution of neutron irradiations. The calculated sigma-N curve is in excellent agreement with the empirical sigma-N-values of pure s-process nuclei. Simultaneously, good agreement is found between the difference of solar and s-process abundances and the abundances of pure r-process nuclei. The abundance pattern of the iron group elements where s-process results complement the abundances obtained from explosive nuclear burning is discussed. The results obtained from the traditional s-process model such as seed abundances, mean neutron irradiations, or neutron densities are compared to recent stellar model calculations which assume the He-burning shells of red giant stars as the site for the s-process.

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