Abstract
In this paper, I have discussed the numerical predictions for the neutron-skin thickness (NST) of various finite nuclei starting from $^{40}$Ca to $^{238}$U using recently developed effective relativistic mean-field models G3 and IOPB-I \cite{G3, IOPB}. The calculated results are compared with the PREX-II data, and the experiment has been done with antiprotons at CERN. Further, I have also calculated the dimensional tidal deformability of a canonical neutron star 1.4$M_\odot$ and compared it with the recent observation of GW1701817.
Highlights
The accurate description of the matter distribution in nuclei is an important problem in nuclear physics to understand the nuclear structure of the nuclei
I have calculated neutron-skin thickness (NST) for the finite nuclei starting from 40 Ca to 238 U using the recently developed new energy density functional G3 and IOPB-I
I have examined the NST of 26 stable nuclei starting from 40 Ca and 238 U without considering the nuclear deformation and superfluidity [9]
Summary
The accurate description of the matter distribution in nuclei is an important problem in nuclear physics to understand the nuclear structure of the nuclei. These bounds can, in turn, constrain the neutron star equation of state In this contribution, I have calculated NST for the finite nuclei starting from 40 Ca to 238 U using the recently developed new energy density functional G3 and IOPB-I. The mean-field formalism approximates the effect of vacuum fluctuation and Fock term in the calculation by fitting the coupling constant with experimental observables. It is the virtue of mean-field that can ignore the basic formalism difficulties like renormalization and divergence of the system and take the simple way just by fitting the coupling constant. From the energy density functional in Eq., the terms having gγ , f, βσ and βω are responsible for the effects related to the electromagnetic structure of the pion and nucleon [8]
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