Neutron-Rich Nuclei in Heaven and Earth

Details Neutron-Rich Nuclei in Heaven and Earth Neutron-Rich Nuclei in Heaven and Earth

2005-04-11

arxiv.org/abs/nucl-th/0504034v1

Phys. Rev. Lett. 95, 122501 (2005)

Physics

Nuclear Physics

Nuclear Theory

4 pages, 3 tables, and no figures

Scientific paper

10.1103/PhysRevLett.95.122501

An accurately calibrated relativistic parametrization is introduced to compute the ground state properties of finite nuclei, their linear response, and the structure of neutron stars. While similar in spirit to the successful NL3 parameter set, it produces an equation of state that is considerably softer -- both for symmetric nuclear matter and for the symmetry energy. This softening appears to be required for an accurate description of several collective modes having different neutron-to-proton ratios. Among the predictions of this model are a symmetric nuclear-matter incompressibility of K=230 MeV and a neutron skin thickness in 208Pb of Rn-Rp=0.21 fm. Further, the impact of such a softening on the properties of neutron stars is as follows: the model predicts a limiting neutron star mass of Mmax=1.72 Msun, a radius of R=12.66 km for a ``canonical'' M=1.4 Msun neutron star, and no (nucleon) direct Urca cooling in neutrons stars with masses below M=1.3 Msun.

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