Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ap%26ss..58..149o&link_type=abstract
Astrophysics and Space Science, vol. 58, no. 1, Sept. 1978, p. 149-165.
Astronomy and Astrophysics
Astrophysics
3
Electron Emission, Nuclear Astrophysics, Nuclear Fission, Nuclear Interactions, Abundance, Atomic Weights, Neutron Stars, Nuclides, Supernovae
Scientific paper
The initial condition for the r-cooling process is determined using a model of the dynamical r-process. All nuclides with Z of at least 80 on the neutron-rich side of the beta-stable line are assumed to have finite probabilities for spontaneous fission, neutron-induced fission, and beta-decay-induced fission. Rates for beta decay, neutrino energy loss, beta-decay-induced fission, and delayed neutron emission are obtained on the basis of Fermi theory, the gross theory of Kodama and Takahashi (1975), and the theory of Cameron et al. (1970). The effect of the accumulation of fission fragments resulting from fissions of r-cooling nuclei on the r-abundance curve is examined. It is concluded that symmetric fission fragments produced during the r-cooling process accumulate in the medium mass range to form a broad fission peak centered around A = 128 and that asymmetric spontaneous fissions occurring during the r-cooling stage can explain the r-abundance anomaly around A = 105.
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