Constraining the relativistic mean-field models from PREX-2 data: effective forces revisited *

Abstract

Based on the current measurement of the neutron distribution radius ($R_n$) of $^{208}$Pb through the PREX-2 data, we re-visited the recently developed G3 and IOPB-I force parameters by fine-tuning some of the specific couplings within the relativistic mean-field (RMF) model. The $\omega$-$\rho$-mesons coupling $\Lambda_{\omega}$ and the $\rho$-meson coupling $g_{\rho}$ are constrained to the experimental neutron radius of $^{208}$Pb without compromising the bulk properties of finite nuclei and infinite nuclear matter observable. The modified parameter sets are applied to calculate the gross properties of finite nuclei such as binding energies, charge distributions, nuclear radii, pairing gaps, and single-particle energies. The root-mean-square deviations in binding energy and charge radius are estimated with respect to the available experimental data for 195 even-even nuclei, and the results compare favourably with the well-calibrated effective interactions of Skyrme, Gogny and other relativistic mean-field parametrizations. The pairing gap estimations for modified G3 and IOPB-I (i.e G3(M) and IOPB-I(M)) for Sn isotopes are also compared with the Hartree-Fock-Bogoliubov calculation with the Gogny (D1S) interaction. The isotopic shift and single-particle energy spacing are also calculated and compared with the experimental data for both original (O) and modified (M) versions of G3 and IOPB-I parameter sets. Subsequently, both the modified parameter sets are used to obtain the various infinite nuclear matter observables at saturation. In addition to these, the force parameters are adopted to calculate the properties of a high isospin asymmetry dense system such as neutron star matter and tested for the validation for the constraint from GW170817 binary neutron star merger events. The tuned forces are predicting relatively good results for finite and infinite nuclear matter systems and the current limitation on neutron radius from PREX-2. A systematic analysis using these two refitted parameter sets over the nuclear chart will be communicated shortly.

Raychaudhuri equation in $k$-essence geometry: conditional singular and non-singular cosmological models

“…Considering the background gravitational metric to be flat Friedmann-Lemaitre-Robertson-Walker (FLRW), then from Eq. ( 9) we have the corresponding emergent gravity line element as [63][64][65]…”

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Isotopic Shift in Hg-Isotopes within Brückner versus Relativistic Energy Density Functional

“…The conventional non-linear relativistic mean-field Lagrangian density is constructed from the interacting nucleons with the interchange of the σ, ω and ρ mesons. As an extension of the previous version, the self-and cross-couplings of the σ, ω and ρ mesons are introduced into the Lagrangian, called "the effective field theory motivated relativistic mean-field formalism" [23,[28][29][30][31]. As a result of the cross-coupling within the participating mesons, the variation of the neutron-skin thickness in heavy-mass nuclei such as 208 Pb becomes feasible.…”