Realistic fission model and the r-process in neutron star mergers

被引：0

作者：

Shibagaki, S. ^{[1
,2
]}

Kajino, T. ^{[1
,2
]}

Chiba, S. ^{[3
]}

Mathews, G. J. ^{[2
,4
]}

机构：

[1] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan

[2] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[3] Tokyo Inst Technol, Nucl Reactors Res Lab, Meguro Ku, Tokyo 1528850, Japan

[4] Univ Notre Dame, Dept Phys, Ctr Astrophys, Notre Dame, IN 46556 USA

来源：

SEVENTH EUROPEAN SUMMER SCHOOL ON EXPERIMENTAL NUCLEAR ASTROPHYSICS | 2014年 / 1595卷

关键词：

r-process; nucleosynthesis; abundance; PROCESS NUCLEOSYNTHESIS;

D O I：

10.1063/1.4875313

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

About half of heavy elements are considered to be produced by the rapid neutron-capture process, r-process. The neutron star merger is one of the viable candidates for the astrophysical site of r-process nucleosynthesis. Nuclear fission reactions play an important role in the r-process of neutron star mergers. However theoretical predictions about fission properties of neutron-rich nuclei have some uncertainties. Especially, their fission fragment distributions are totally unknown and the phenomenologically extrapolated distribution was often applied to nucleosynthesis calculations. In this study, we have carried out r-process nucleosynthesis calculations based upon new theoretical estimates of fission fragment distributions. We discuss the effects on the r-process in neutron star mergers from the nuclear fission of heavy neutron-rich actinide elements. We also discuss how variations in the fission fragment distributions affect the abundance pattern.

引用

页码：211 / 213

页数：3

共 13 条

[1]

Chiba S, 2008, AIP CONF PROC, V1016, P162, DOI 10.1063/1.2943568

[2] Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations [J].