Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..407o&link_type=abstract
ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,
Astronomy and Astrophysics
Astronomy
Scientific paper
The equation of state (EOS) of asymmetric nuclear matter dominates macroscopic properties of neutron rich nuclei in laboratories, and extremely neutron-rich pasta nuclei (rodlike and slablike nuclei and rodlike and spherical nuclear bubbles) in a neutron star crust. The purpose of this study is to identify the most important EOS parameter that governs the radii of neutron-rich laboratory nuclei and the density range of the pasta nuclei. In a simplified Thomas-Fermi method, we calculate the masses and density distributions of neutron-rich laboratory nuclei and pasta nuclei using various EOS's that are consistent with empirical data for masses and radii of stable nuclei, and systematically examine the EOS dependence of the matter radii of laboratory nuclei and the density range of the crustal part including pasta nuclei. It is found that both the calculated matter radii of neutron-rich laboratory nuclei and the calculated density range of the pasta nuclei show a clear dependence on the density symmetry coefficient L, while the dependence on the incompressibility K0 is much weaker. The density range of the pasta nuclei is found to disappear for extremely large L values. These results suggest that future systematic measurements of the matter radii of neutron-rich nuclei could help deduce the L value, which in turn could give useful information about the presence of pasta nuclei in neutron star crusts.
Iida Kei
Oyamatsu Kazuhiro
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