Effects of $\omega$ meson self-coupling on the properties of finite nuclei and neutron stars

Abstract

The effects of $\omega$ meson self-coupling (OMSC) on the properties of finite nuclei and neutron stars are investigated within the framework of effective field theory based relativistic mean-field (ERMF) model which includes the contributions from all possible mixed interactions between the scalar-isoscalar ($\sigma$), vector-isoscalar ($\omega$) and vector-isovector ($\rho$) mesons upto the quartic order. For a realistic investigation, several parameter sets corresponding to different values of OMSC are generated by adjusting the remaining parameters of the ERMF model to fit the properties of the finite nuclei. Though, all these parameter sets give equally good fit to the properties of the finite nuclei, only moderate values of OMSC are favored from the "naturalness" point of view. The equation of state for the symmetric nuclear and pure neutron matters resulting from the parameter sets with the moderate values of OMSC are in close agreement with the ones obtained within the Dirac-Brueckner-Hartree-Fock approximation. For such parameter sets the limiting mass for the neutron stars composed of $\beta$-stable matter is $\sim 1.9M_{\odot }$. It is found that the direct Urca process can occur in the neutron stars with "canonical" mass of $1.4M_{\odot }$ only for the moderate and higher values of OMSC. Some other interesting properties for the neutron stars are also discussed.

arXiv comment23 pages, 11 figures. Phys. Rev. C (in press)

References in corpus (18)

• Neutron Star Structure and the Equation of State
• A New Parameterization for the Lagrangian Density of Relativistic Mean Field Theory
• The Physics of Neutron Stars
• Recent Progress in Quantum Hadrodynamics
• Neutron-Rich Nuclei in Heaven and Earth
• Relativistic Mean-Field Theory and the High-Density Nuclear Equation of State
• Neutron Radii in Mean-Field Models
• A Chiral Effective Lagrangian for Nuclei
• Nuclear matter symmetry energy and the neutron skin thickness of heavy nuclei
• Nuclear Ground State Observables and QCD Scaling in a Refined Relativistic Point Coupling Model
• Determination of the parameters of a Skyrme type effective interaction using the simulated annealing approach
• Analysis of Chiral Mean-Field Models for Nuclei
• Unmasking the nuclear matter equation of state
• Roles of Hyperons in Neutron Stars
• Exploring the extended density-dependent Skyrme effective forces for normal and isospin-rich nuclei to neutron stars
• Atomic Parity Non-Conservation, Neutron Radii, and Effective Field Theories of Nuclei
• Density dependencies of interaction strengths and their influence on nuclear matter and neutron star in relativistic mean field theory
• Adjustment studies in self-consistent relativistic mean-field models

Cited by in corpus (27)

• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Non-rotating and rotating neutron stars in the extended field theoretical model
• New relativistic effective interaction for finite nuclei, infinite nuclear matter and neutron stars
• Asymmetric nuclear matter and neutron-skin in extended relativistic mean field model
• Stellar properties and nuclear matter constraints
• Time-odd mean fields in covariant density functional theory I. Non-rotating systems
• Neutron stars in $f(\mathcal{R},\mathcal{T})$ gravity using realistic equations of state in the light of massive pulsars and GW170817
• Optimization of relativistic mean field model for finite nuclei to neutron star matter
• Investigating Dark Matter-Admixed Neutron Stars with NITR Equation of State in Light of PSR J0952-0607
• A Neutron Star is born
• Low-energy nuclear physics and global neutron star properties
• Compiled Properties of Nucleonic Matter and Nuclear and Neutron Star Models from Non-Relativistic and Relativistic Interactions
• Many-body forces in magnetic neutron stars
• Effect of isovector scalar meson on equation of state of dense matter within relativistic mean field model
• Thermal Relaxation of Dark Matter Admixed Neutron Star
• Critical parameters of consistent relativistic mean-field models
• CREX- and PREX-II-motivated relativistic interactions and their implications for the bulk properties of nuclear matter and neutron stars
• Relativistic Mean Field Model parameterizations in the light of GW170817, GW190814, and PSR J0740 + 6620
• Observational constraint from the heaviest pulsar PSR J0952-0607 on the equation of state of dense matter in relativistic mean field model
• Relativistic approach for the determination of nuclear and neutron star properties in consideration of PREX-II results
• Criteria for nonlinear parameters of relativistic mean field models
• Nuclear fragmentation reactions as a probe of neutron skins in nuclei
• The symmetry energy $\gamma$ parameter of relativistic mean-field models
• The nuclear symmetry energy and the neutron skin thickness in nuclei
• Neutron star crustal properties from relativistic mean-field models and bulk parameters effects
• Dark energy effects on realistic neutron stars
• Implications of nuclear interaction for nuclear structure and astrophysics within the relativistic mean-field model