Impact of Nuclear Deformation on Neutron Dripline Prediction: A Study of Mg Isotopes

We have employed the relativistic Hartree-Bogoliubov (RHB) model with density-dependent meson-exchange interaction and separable pairing to investigate neutron dripline mechanisms for heavy Mg isotopes. In the present study, 40Mg is predicted to be dripline nuclei. The calculations are carried out by taking axial deformation into account. An investigation of shape transition is also done for even-even 32-42Mg isotopes. Our prediction for neutron dripline for 40Mg is consistent with some recent studies

Deformation Effect on Proton Bubble Structure in N = 28 Isotones

Purpose: To study the effect of nuclear deformation on proton bubble structure of N = 28 isotones and and compare it with the spherical limits. The reduction of depletion fraction due to deformation can be explained by studying the relative differences in the central densities.Methods: In this work, we have employed relativistic Hartree-Bogoliubov (RHB) model withdensity-dependent meson-exchange (DD-ME2) interaction and separable pairing interaction. We have performed axially constrained calculations to investigate the deformed proton bubble structure in 40Mg, 42Si, 44S, and 46Ar, isotones of N = 28 shell closure.Results: We have observed that the nuclear deformation play againsts the formation of bubble structure. In the spherical limits, the isotones of N = 28 shell closure have pronounced bubble structure with large value of depletion fraction. But, the increase in deformation leads to the disappearance of bubble structure. The internal densities in deformed nuclei are found to increase with deformation which can be related to the decrease in depletion fraction.Conclusion: By using RHB model, we have investigated the ground state and proton bubble structure of N = 28 isotones. In 44S, and 46Ar, the 2s1/21d3/2 states get inverted due to the weakning of spin-orbit strength. Due to strong dynamical correlations, arising from deformation, the central depletion of proton density is greatly affected in these isotones. The decrease in depletion fraction can be related to increase in the internal density due to deformatio

Nuclear shape evolution and shape coexistence in Zr and Mo isotopes

The phenomena of shape evolution and shape coexistence in even-even $^{88-126}$Zr and $^{88-126}$Mo isotopes is studied by employing covariant density functional theory (CDFT) with density-dependent point coupling parameter sets DD-PCX and DD-PC1, and with separable pairing interaction. The results for rms deviation in binding energies, two-neutron separation energy, the differential variation of two-neutron separation energy, and rms charge radii, as a function of neutron number, are presented and compared with available experimental data. In addition to the oblate-prolate shape coexistence in $^{96-110}$Zr isotopes, the correlation between shape transition and discontinuity in the observables are also examined. A smooth trend of charge radii in Mo isotopes is found to be due to the manifestation of triaxiality softness. The observed oblate and prolate minima are related to the low single-particle energy level density around the Fermi level of neutron and proton respectively. The present calculations also predict a deformed bubble structure in $^{100}$Zr isotope.Comment: this preprint contains incomplete data and some mistake

Relativistic Mean Field Model parameterizations in the light of GW170817, GW190814, and PSR J0740 + 6620

Three parameterizations DOPS1, DOPS2, and DOPS3 (named after the Department of Physics Shimla) of the Relativistic Mean Field (RMF) model have been proposed with the inclusion of all possible self and mixed interactions between the scalar-isoscalar (\sigma), vector-isoscalar (\omega) and vector-isovector (\rho) mesons up to quartic order. The generated parameter sets are in harmony with the finite and bulk nuclear matter properties. A set of Equations of State (EOSs) composed of pure hadronic (nucleonic) matter and nucleonic with quark matter (hybrid EOSs) for superdense hadron-quark matter in \beta-equilibrium is obtained. The quark matter phase is calculated by using the three-flavor Nambu-Jona-Lasinio (NJL) model. The maximum mass of a non-rotating neutron star with DOPS1 parameterization is found to be around 2.6 M$\odot$ for the pure nucleonic matter which satisfies the recent gravitational wave analysis of GW190814 Abbott et al.,(2020) with possible maximum mass constraint indicating that the secondary component of GW190814 could be a non-rotating heaviest neutron star composed of pure nucleonic matter. EOSs computed with the DOPS2 and DOPS3 parameterizations satisfy the X-Ray observational data and the recent observations of GW170817 maximum mass constraint of a stable non-rotating neutron star in the range 2.01 \pm 0.04 - 2.16 \pm 0.03 M\odot and also in good agreement with constraints on mass and radius measurement for PSR J0740+6620 (NICER) Riley et al., L27 (2021)}, Miller et al., (2021). The hybrid EOSs obtained with the NJL model also satisfy astrophysical constraints on the maximum mass of a neutron star from PSR J1614-2230 and Demorest et al., (2010) .We also present the results for dimensionless tidal deformability, ${\Lambda}$ which are consistent with the waveform models analysis of GW170817.Comment: 14 Pages, 10 Figures. arXiv admin note: text overlap with arXiv:2110.07877 by other author

Observational constraint from the heaviest pulsar PSR J0952-0607 on the equation of state of dense matter in relativistic mean field model

In the present work, we constrain the equation of the state of dense matter in the context of heaviest observed neutron star mass M$_{max}$ = 2.35$\pm 0.17$ M$_{\odot}$ for the black widow pulsar PSR J0952-0607. We propose three interactions HPU1, HPU2 and HPU3 (named after Himachal Pradesh University)for the relativistic mean field model which include different combinations of non-linear, self and cross-couplings among isoscalar-scalar $\sigma$, isoscalar-vector $\omega$ and isovector-vector $\rho$ meson fields up to the quartic order. These interactions are in harmony with the finite nuclei and bulk nuclear matter properties. The equations of state computed by using newly generated interactions for the $\beta$-equilibrated nucleonic matter satisfy the heaviest observed neutron star mass M$_{max}$ = 2.35$\pm 0.17$ M$_{\odot}$ for the black widow pulsar PSR J0952-0607. The results for the radius ($R_{1.4}$) and dimensionless tidal deformability (${\Lambda_{1.4}}$) corresponding to the canonical mass are also presented and agree well with the GW170817 event and astrophysical observations. The radius of $2.08M_{\odot}$ neutron star mass is predicted to be in the range $R_{2.08}$ = 12.98 -13.09 Km which also satisfies the NICER observations by Miller et al. (2021) and Riley et al.(2021). A covariance analysis is also performed to assess the theoretical uncertainties of model parameters and to determine their correlations with nuclear matter observables.Comment: 19 pages, 12 Figures. arXiv admin note: substantial text overlap with arXiv:2305.06667, arXiv:2305.0593

Structural properties of rotating hybrid compact stars with color-flavor-locked quark matter core and their tidal deformability

We investigate the hybrid compact stars consisting of nucleons, hyperons and three flavor color-flavor-locked quark phase under global neutrality and chemical equilibrium conditions. The hadronic equations of state are computed within the framework of energy density functionals based on the relativistic mean field theory by employing two different model. The quark matter phase of equation of state is computed by using Quark Quasiparticle model derived from a non-relativistic energy density-functional approach. A set of hybrid equations of state for superdense hadron-quark matter is obtained and, employed to investigate the structural properties of non-rotating and rotating compact stars. The internal structure of rotating star with observed spin down frequencies, exhibiting shrinkage of soft quark core of compact stars are discussed for constant baryonic mass. We present the theoretically computed limits of radii for the spin down configurations of hybrid stars corresponding to the recently observed millisecond pulsars. The various EOSs considered in the present work are well within the recent astrophysical constraints on mass and radius measurements (Riley et al. in Astrophys J Lett 918(2):L27, 2021; Millet et al. in http://arxiv.org/abs/2105.0697

Effect of nuclear deformation on proton bubble structure in

We have studied the density distribution in some “bubble” nuclei. The bubble nuclei are characterized by the depletion of nucleonic density at the center of the nucleus. We have explored the effect of nuclear deformation on proton bubble structure in the Si isotopic chain. The Covariant Density Functional Theory (CDFT) with density-dependent meson-exchange (DD-ME2) interaction has been employed. Triaxially constrained calculations are performed to investigate the deformed bubble structure. Deformation causes the mixing of shells hence reducing the bubble effect in the nuclei. The role of nuclear deformation in nuclear density profiles is explored and compared with the spherical limits