INFLUENCE OF SHELL-QUENCHING FAR FROM STABILITY ON THE ASTROPHYSICAL R-PROCESS

被引:141
作者
CHEN, B
DOBACZEWSKI, J
KRATZ, KL
LANGANKE, K
PFEIFFER, B
THIELEMANN, FK
VOGEL, P
机构
[1] UNIV WARSAW,INST THEORET PHYS,PL-00681 WARSAW,POLAND
[2] UNIV MAINZ,INST KERNCHEM,D-55099 MAINZ,GERMANY
[3] UNIV BASEL,INST THEORET PHYS,CH-4056 BASEL,SWITZERLAND
[4] CALTECH,DEPT PHYS,PASADENA,CA 91125
基金
美国国家科学基金会;
关键词
D O I
10.1016/0370-2693(95)00737-6
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Comparison of results from r-process calculations within the waiting-point assumption and the r-process component (N-r,.) 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 similar or equal to 120 and 140, indicating an overly strong N = 82 strength (some models also showed problems around A similar or equal to 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 N-r,. fit, indicating a solution to a puzzle existing in r-process nucleosynthesis.
引用
收藏
页码:37 / 44
页数:8
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