Application of the coherent density fluctuation model to study the nuclear matter properties of finite nuclei within the relativistic mean-field formalism

Abstract

We obtained a density-dependent analytical expression of binding energy per nucleon for different neutron-proton asymmetry of the nuclear matter (NM) with a polynomial fitting, which manifests the results of effective field theory motivated relativistic mean-field (E-RMF) model. This expression has the edge over the Br$\ddot{u}$ckner energy density functional [Phys. Rev. {\bf 171}, 1188 (1968)] since it resolves the Coster-Band problem. The NM parameters like incompressibility, neutron pressure, symmetry energy, and its derivatives are calculated using the acquired expression of energy per nucleon. Further, the weight function calculated by E-RMF densities are folded with calculated NM parameters within coherent density fluctuation model to find the properties of closed/semi-closed-shell even-even ${}^{16}$O, ${}^{40}$Ca, ${}^{48}$Ca, ${}^{56}$Ni, ${}^{90}$Zr, ${}^{116}$Sn, and ${}^{208}$Pb nuclei. The values obtained for the neutron pressure $P^A$, symmetry energy $S^A$ and its derivative $L_{sym}^A$ known as slope parameter, lie within a narrow domain whereas there is a large variation in isoscalar incompressibility $K^A$ and surface incompressibility $K_{sym}^A$ while moving from light to heavy nuclei. The sizable variation in $K^A$ and $K_{sym}^A$ for light and heavy nuclei depicts their structural dependence due to the peculiar density distribution of each nucleus. A comparison of surface quantities calculated in the present work has also been made with ones obtained via Br$\ddot{u}$ckner energy density functional.

arXiv comment8 pages, 5 figures, 3 tables. Published in Phys. Rev. C 103 , 024305 (2021)

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• Systematic study for the surface properties of neutron star