Fission barriers of neutron-rich and superheavy nuclei calculated with the ETFSI method

By A. Mamdouh, J. Pearson, M. Rayet, F. T. I. D. E. d'Astrophysique, Universit́e Libre de Bruxelles, Belgium, D. Physique, U. Montŕeal, Montreal, Canada. and 1 more. 2000

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Abstract Using the ETFSI (extended Thomas–Fermi plus Strutinsky integral) method, we have calculated the fission barriers of nearly 2000 exotic nuclei, including all the neutron-rich nuclei up to A=318 that are expected to be relevant to the r-process, and all superheavy nuclei in the vicinity of N=184 , with Z≤120 . Our calculations were performed with the Skyrme force SkSC4, which was determined in the ETFSI-1 mass fit. For proton-deficient nuclei in the region of N=184 we find the barriers to be much higher than previously believed, which suggests that the r-process path might continue to mass numbers well beyond 300. For the superheavy nuclei we typically find barrier heights of 6–7 MeV.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f096869b6ab61040e9dccd97ed093e76ad61419e

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In Nuclear and High Energy Physics

Citations in the corpus

Signatures of hypermassive neutron star lifetimes on r-process nucleosynthesis in the disc ejecta from neutron star mergers (2017, background): “Spontaneous and neutron-induced fission rates are taken from Frankel & Metropolis (1947), Panov et al. (2010), Mamdouh et al. (2001), and Wahl (2002).”
Nuclear weak-interaction processes in stars (2002, background): “The relevant beta-delayed fission probabilities depend sensitively on the modelling of the fission barriers (Howard and Möller, 1980; Mamdouh et al., 2001).”
ELECTROMAGNETIC TRANSIENTS POWERED BY NUCLEAR DECAY IN THE TIDAL TAILS OF COALESCING COMPACT BINARIES (2011, unknown): “Fission barriers are taken from Mamdouh et al. (2001).”