Abstract
The symmetry energy, the neutron pressure and the asymmetric compressibility of spherical Ni, Sn, Pb and deformed Kr, Sm neutron-rich even-even nuclei are calculated within the coherent density fluctuation model using the symmetry energy as a function of density within the Brueckner energy-density functional. The correlation between the thickness of the neutron skin and the characteristics related with the density dependence of the nuclear symmetry energy is investigated for isotopic chains of these nuclei in the framework of the deformed self-consistent mean-field Skyrme HF+BCS method. The mass dependence of the nuclear symmetry energy and the neutron skin thickness are also studied together with the role of the neutron-proton asymmetry. The studied correlations reveal a smoother behavior in the case of spherical nuclei than for deformed ones. We also notice that the neutron skin thickness obtained for 208Pb with SLy4 force is found to be in a good agreement with the recent data. In addition to the interest that this study may have by itself, we give some numerical arguments in proof of the existence of peculiarities of the studied quantities in Ni and Sn isotopic chains that are not present in the Pb chain.
Highlights
Great attention has been paid to the nuclear equation of state of isospin asymmetric nuclear matter (ANM), in particular the nuclear matter symmetry energy
The main aim of this work is to investigate the relation between the neutron skin thickness and some nuclear matter properties in finite nuclei, such as the symmetry energy at the saturation point s, symmetry pressure p0, and asymmetric compressibility ∆K, considering nuclei in given isotopic chains and within a certain theoretical approach
We observe a smooth growth of the symmetry energy till the double-magic nucleus 78Ni (N = 50) and a linear decrease of s while the neutron skin thickness of the isotopes increases
Summary
Great attention has been paid to the nuclear equation of state of isospin asymmetric nuclear matter (ANM), in particular the nuclear matter symmetry energy. The density-dependent symmetry energy governs numerous isospin-dependent properties of nuclei such as the binding energy, the location of the drip lines, the density distributions, as well as the reactions: giant resonances, heavy ion collisions, isospin diffusion, and multifragmentation. The nuclear symmetry energy is crucial in the astrophysical calculations of neutron stars, supernova explosions and stellar nucleosynthesis. The neutron skin thickness is one of the observables where symmetry energy shows up in the ground state of nuclei [1]. Neutron skin defined through the rms radii of protons and neutrons depends on the properties of the nuclear surface. The relative differences of the neutron and the proton distributions in this region are sensitive to the symmetry energy at the subsaturation densities
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