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The neutron skin thickness $Delta r_{rm{np}}$ of heavy nuclei is essentially determined by the symmetry energy density slope $L({rho })$ at $rho_c = 0.11/0.16rho_0$ ($rho_0$ is nuclear saturation density), roughly corresponding to the average density of finite nuclei. The PREX collaboration recently reported a model-independent extraction of $Delta r^{208}_{rm{np}} = 0.29 pm 0.07$ fm for the $Delta r_{rm{np}}$ of $^{208}$Pb, which suggests a rather stiff symmetry energy $E_{rm{sym}}({rho })$ with $L({rho_c }) ge 55$ MeV. We demonstrate that the $E_{rm{sym}}({rho })$ cannot be too stiff and $L({rho_c }) le 73$ MeV is necessary to be compatible with (1) the ground-state properties and giant monopole resonances of finite nuclei, (2) the constraints on the equation of state of symmetric nuclear matter at suprasaturation densities from flow data in heavy-ion collisions, (3) the largest neutron star (NS) mass reported so far for PSR J0740+6620, (4) the NS tidal deformability extracted from gravitational wave signal GW170817 and (5) the mass-radius of PSR J0030+045 measured simultaneously by NICER. This allow us to obtain $55 le L({rho_c }) le 73$ MeV and $0.22 le Delta r^{208}_{rm{np}} le 0.27$ fm, and further $E_{rm{sym}}({rho_0 }) = 34.5 pm 1.5$ MeV, $L({rho_0 }) = 85.5 pm 22.2$ MeV, and $E_{rm{sym}}({2rho_0 }) = 63.9 pm 14.8$ MeV. A number of critical implications on nuclear physics and astrophysics are discussed.
The recent announcement of the PREX-II measurement of the neutron skin of $^{208}$Pb that suggests a stiff symmetry energy near nuclear matter density $n_0$ and its impact on the EoS of massive compact stars raise the issue as to whether the widely a
A number of observed phenomena associated with individual neutron star systems or neutron star populations find explanations in models in which the neutron star crust plays an important role. We review recent work examining the sensitivity to the slo
The symmetry energy obtained with the effective Skyrme energy density functional is related to the values of isoscalar effective mass and isovector effective mass, which is also indirectly related to the incompressibility of symmetric nuclear matter.
Recently, the radius of neutron star (NS) PSR J0740+6620 was measured by NICER and an updated measurement of neutron skin thickness of ${}^{208}$Pb ($R_{rm skin}^{208}$) was reported by the PREX-II experiment. These new measurements can help us bette
In this work we investigate protoneutron star properties within a modified version of the quark coupling model (QMC) that incorporates a omega-rho interaction plus kaon condensed matter at finite temperature. Fixed entropy and trapped neutrinos are t