I use properties of doubly magic nuclei to constrain symmetric nuclear matter and neutron matter equations of state. I conclude that these data determine the value of the neutron equation of state at a density of ρ(on)=0.10  nucleons/fm3 to be 11.4(10) MeV. The slope at that point is constrained by the value of the neutron skin. Analytical equations are given that show the dependence of the Sky...

Matter of subnuclear density in the inner crusts of neutron stars consists of neutron-rich atomic nuclei immersed in strongly degenerate relativistic gas of electrons and strongly nonideal liquid of neutrons. Thermodynamic and kinetic properties of this matter are greatly affected by Coulomb and nuclear interactions and can be studied, in principle, from observations of thermal radiation of you...

We analyze the correlations of the slope and curvature parameters of the symmetry energy with the neutron skin thickness of neutron-rich isotopes, and the crust-core transition density in neutron stars. The results are obtained within the microscopic Brueckner–Hartree–Fock approach, and are compared with those obtained with several Skyrme and relativistic mean field models.

We seek a measure of the neutron density of Pb from analyses of intermediate energy nucleon elastic scattering. The pertinent model for such analyses is based on coordinate space nonlocal optical potentials obtained from model nuclear ground state densities. Those potentials give predictions of integral observables and of angular distributions which show sensitivity to the neutron density. When...

We seek a measure of the neutron density of 208Pb from analyses of intermediate energy nucleon elastic scattering. The pertinent model for such analyses is based on coordinate space nonlocal optical potentials obtained from model nuclear ground state densities. Those potentials give predictions of integral observables and of angular distributions which show sensitivity to the neutron density. W...

We discuss SU(2) chiral sigma model in the nuclear matter using mean field approach at high density. In this model we include a dynamically generated isoscalar vector field and higher order terms in scalar field. With inclusion of these, we reproduce the empirical values of the nuclear matter saturation density, binding energy and the nuclear incompressibility. The desirable value of incompress...

Neutron star mass and radius measurements are becoming sufficiently accurate as to offer astrophysical constraints on the properties of neutron-rich matter near the nuclear saturation density. Current observations, which imply that the radius of a 1.4 solar mass neutron star lies between 10.4 and 12.9 km (95% confidence), also imply that 43 < L < 67 MeV, where L is a parameter describing the sl...

We show that the widely used parabolic approximation to the Equation of State (EOS) of asymmetric nuclear matter leads systematically to significantly higher core-crust transition densities and pressures. Using an EOS for neutron-rich nuclear matter constrained by the isospin diffusion data from heavy-ion reactions in the same sub-saturation density range as the neutron star crust, the density ...