New equations of state for dense nuclear matter properties

Sharma, Anuj; Kumar, Mukul; Kumar, Sunil; Thakur, Virender; Kumar, Raj; Dhiman, Shashi K.

doi:10.1016/j.nuclphysa.2023.122762

Cited by 2 publications

(1 citation statement)

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“…The overall effective Lagrangian density characterizing the RMF model outlines the interaction mechanism between nucleons through the exchange of σ, ω μ , and ρ μ mesons, accounting for interactions up to the fourth power in terms of these particles. The Lagrangian density for the RMF model including the isoscalar (σ and ω μ ) and isovector (ρ μ ) mesons as well as nucleons (N = p, n) [32][33][34][35] is given by…”

Section: Theoretical Modelmentioning

confidence: 99%

Relativistic description of dense matter equation of state and neutron star observables constrained by recent astrophysical observations

Kumar,

Kumar

et al. 2024

J. Phys. G: Nucl. Part. Phys.

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In the present work, we investigate the bulk properties of nuclear matterand neutron stars with the newly proposed relativistic interaction NL-RS whichprovides an opportunity to readjust the coupling constants keeping in view theproperties of finite nuclei, nuclear matter, PREX-II results for neutron skin thickness in208Pb and astrophysical observations. The NL-RS model interaction has been proposedby fitting the ground state properties (binding energies and charge radii) of finitenuclei, bulk nuclear matter properties, and PREX-II results for neutron skin thicknessof 208 Pb. The relativistic interaction has been generated by including non-linear self-interactions of σ and ωµ -mesons and mixed interactions of ωµ , and ρµ -meson up tothe quartic order. The proposed interaction harmonizes with the finite nuclei, bulknuclear matter, and neutron star properties. A covariance analysis is performed toassess the statistical uncertainties on the model parameters and nuclear observables ofinterest along with correlations amongst them. The equation of state (EoS) composedof nucleons and leptons in β - β-equilibrium is computed with the proposed parameterset and used to study the neutron star structure. The maximum mass of the neutronstar by employing the EoS computed with the NL-RS parameter set is 2.04±0.03M⊙ and the radius of a canonical mass neutron star (R1.4 ) comes out to be equal to13.06±0.16 Km. The value of dimensionless tidal deformability, for canonical mass, is602.23±33.13 which satisfies the

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Section: Theoretical Modelmentioning

confidence: 99%