Influence of shell-quenching far from stability on the astrophysical r-process

Details Influence of shell-quenching far from stability on the astrophysical r-process Influence of shell-quenching far from stability on the astrophysical r-process

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phlb..355...37c&link_type=abstract

Physics Letters B, v. 355, p. 37-44

Physics

89

Elsevier: R-Process, Nuclear Masses, Shell-Quenching

Scientific paper

Comparison of results from r-process calculations within the waiting-point assumption and the r-process component (Nr,solar) of the solar-system composition of heavy elements, permits to test nuclear structure far from stability. Previous investigations, making use of nuclear mass predictions from global macroscopic-microscopic models, showed abundance deficiencies around A ~= 120 and 140, indicating an overly strong N = 82 strength (some models also showed problems around A ~= 180 related to the N = 126 shell). In this paper we calculate masses based on Skyrme interactions locally around N = 82, within the HF+BCS method with the SIII interaction and the HFB theory with SkP interaction. The shell-quenching obtained in the latter approach results in a considerable improvement of the global Nr,solar fit, indicating a solution to a puzzle existing in r-process nucleosynthesis.

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