Beta-delayed fission and neutron emission: Consequences for the astrophysical r-process and the age of the galaxy

Details Beta-delayed fission and neutron emission: Consequences for the astrophysical r-process and the age of the galaxy Beta-delayed fission and neutron emission: Consequences for the astrophysical r-process and the age of the galaxy

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983zphya.309..301t&link_type=abstract

Zeitschrift für Physik A Atoms and Nuclei, Volume 309, Issue 4, pp.301-317

Mathematics

Probability

51

Scientific paper

Beta-delayed neutron emission and beta-delayed fission probabilities ( P n and P β d j ) were calculated for neutron-rich nuclei between the beta stability line and the neutron-drip line in the range 10≦Z≦100 and 75≦Z≦100, respectively. These results were obtained by applying recent β-strength function calculations, fission barrier height predictions, and a neutron optical potential from infinite nuclear matter calculations. An area of ˜100% fission probability is predicted around Z=94, N=168 extending beyond the well-known island of spontaneous fission in that region. Astrophysical r-process calculations were performed including the calculated P n and P β d f values. This puts the method to determine the age of the Galaxy by the actinide chronometers on a reliable basis. An excellent overall agreement with the observed r-abundance distribution is obtained. The predicted r-process production ratios for the Chronometrie pairs232Th/238U,235U/238U and244Pu/238U result in an age of the Galaxy of t G =(20.8±{4/2})×109 a, which is by almost a factor two larger than earlier predictions by this method, but in accordance with recent astronomical observations from globular clusters. The predicted island of 100% β-delayed fission acts as a sink to the r-process with the consequence that no superheavy elements are produced in nature.

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