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

Conference item

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.

Authors: Brown, B; Clement, R; Schatz, H; Giansiracusa, J; Richter, W

• Publication status: Published
• Journal: NUCLEAR PHYSICS A
• Volume: 719
• Pages: 177C-184C
• Publication date: 2003-05-19
• Event title: 17th International Nuclear Physics Divisional Conference of the European-Physical-Society
• DOI: 10.1016/S0375-9474(03)00914-X
• ISSN: 0375-9474
• Keywords: ISOTOPES; SD-SHELL; SHELL-MODEL; FRAGMENTATION; PROTON DRIP-LINE; ISOTONES