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

Abstract:
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.
Publication status:
Published

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Institution:
University of Oxford
Department:
Oxford, MPLS, Mathematical Inst
Role:
Author
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Volume:
719
Pages:
177C-184C
Publication date:
2003-05-19
DOI:
ISSN:
0375-9474
URN:
uuid:3c5140cd-15ad-40a5-ad14-a097faa49fca
Source identifiers:
13547
Local pid:
pubs:13547

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