Unstable Nuclei and AN EOS Table for Supernovae and the R-Process in a Relativistic Many-Body Approach

Details Unstable Nuclei and AN EOS Table for Supernovae and the R-Process in a Relativistic Many-Body Approach Unstable Nuclei and AN EOS Table for Supernovae and the R-Process in a Relativistic Many-Body Approach

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003omeg.conf..297s&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2000. Proceedings of the International Symposium. Held 19-21 January 2000 in Universi

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We study supernova explosions and the associated r-process using a nuclear-matter equation of state (EOS) derived by a relativistic many-body approach. Recently, we have completed a relativistic EOS table which spans the wide range of density, composition and temperature relevant to supernova explosions. We apply this EOS table to numerical simulations of the gravitational core collapse, subsequent evolution of the proto-neutron star, and the r-process. To derive the requisite nuclear-physics ingredients for supernova, we have constructed a relativistic mean field (RMF) framework based upon relativistic Brückner-Hartree-Fock theory. We have successfully applied the constructed RMF framework to the ground state properties of many nuclei in the nuclear chart. We apply this same RMF framework to derive the supernova EOS table. As examples of astrophysical applications of the EOS table, hydrodynamical simulations of core collapse have been performed. We have also performed numerical simulations of the hydrodynamics of the ν-driven wind from the nascent proto-neutron star. We find that a successful r-process is indeed possible with a short expansion time scale in the ν-driven wind above the massive and compact proto-neutron star.

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