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

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

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003nupha.719..177b&link_type=abstract

Nuclear Physics A, Volume 719, p. C177-C184.

Physics

Nuclear Physics

5

Scientific paper

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 132Sn to provide Q values and beta-decay lifetimes for the r-process.

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