Nuclear structure theory for the astrophysical rp-process and r-process

被引：9

作者：

Brown, BA ^{[1
]}

Clement, R

Schatz, H

Giansiracusa, J

Richter, WA

Hjorth--Jensen, M

Kratz, KL

Pfeiffer, B

Walters, WB

机构：

[1] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA

[2] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA

[3] Univ Stellenbosch, Dept Phys, ZA-7600 Stellenbosch, South Africa

[4] Univ Oslo, Dept Phys, N-0316 Oslo, Norway

[5] Johannes Gutenberg Univ Mainz, Inst Kernchem, D-55128 Mainz, Germany

[6] Univ Maryland, Dept Chem, College Pk, MD 20742 USA

来源：

NUCLEAR PHYSICS A | 2003年 / 719卷

关键词：

D O I：

10.1016/S0375-9474(03)00914-X

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

The astrophysical processes of rapid-proton capture and rapid-neutron capture require the knowledge of many nuclear properties which are not known from experiment. I will describe two examples of how theoretical models are used to provide this input. The first of these uses the Hartree-Fock method for displacement energies to obtain the masses of proton-rich nuclei needed for the rp-process. The second uses a model for configuration mixing near Sn-132 to provide Q values and beta-decay lifetimes for the r-process.

引用

页码：177C / 184C

页数：8

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