The ground state properties of finite,bulk matter,and neutron stars are investigated using a proposed effective interaction(HPU4)of the relativistic mean field model(RMF)that incorporates self and cross-couplings ofσ...The ground state properties of finite,bulk matter,and neutron stars are investigated using a proposed effective interaction(HPU4)of the relativistic mean field model(RMF)that incorporates self and cross-couplings ofσ,ω,andρmesons with nucleons.This interaction has been constructed by fitting data on binding energies and charge radii of finite nuclei,neutron skin (Δr_(np)) of^(48)Ca nucleus,and astrophysical observations of the maximum masses of neutron stars.Δr_(np)(^48Ca)=0.146±0.019 fm is achieved with soft symmetry energy(J_(0)=27.91±1.31 MeV)and its corresponding slope(L_(0)=42.85±14.26 MeV)at saturation density.An equation of state(EoS)with a composition ofβ-equilibrated nucleonic and leptonic matter is computed.The nuclear matter and neutron star properties are also analyzed for this interaction and agree well with the astrophysical observations,such as the NICER and GW170817 events.We also perform a statistical analysis to estimate the theoretical errors in coupling parameters and neutron star observables and to determine the correlation coefficients.We observe that the neutron skins of ^(208)Pb and ^(48)Ca are strongly correlated and exhibit a strong dependence on J_(0),L(0)and the curvature of symmetry energy(K_(sym))as suggested from their correlations.A strong correlation of canonical mass neutron star radius,R1.4 with ρ-meson-nucleon coupling quantified by the term gpN and mixed interaction terms σ_(μ)ρ^(μ) and σ^(2)ρ_(μ)ρ^(μ) is also observed.展开更多
基金Sunil Kumar is highly thankful to CSIR-UGC(Govt.of India)for providing financial assistance(NTA/211610029883 dated 19/04/2022)under the Junior/Senior Research Fellowship scheme。
文摘The ground state properties of finite,bulk matter,and neutron stars are investigated using a proposed effective interaction(HPU4)of the relativistic mean field model(RMF)that incorporates self and cross-couplings ofσ,ω,andρmesons with nucleons.This interaction has been constructed by fitting data on binding energies and charge radii of finite nuclei,neutron skin (Δr_(np)) of^(48)Ca nucleus,and astrophysical observations of the maximum masses of neutron stars.Δr_(np)(^48Ca)=0.146±0.019 fm is achieved with soft symmetry energy(J_(0)=27.91±1.31 MeV)and its corresponding slope(L_(0)=42.85±14.26 MeV)at saturation density.An equation of state(EoS)with a composition ofβ-equilibrated nucleonic and leptonic matter is computed.The nuclear matter and neutron star properties are also analyzed for this interaction and agree well with the astrophysical observations,such as the NICER and GW170817 events.We also perform a statistical analysis to estimate the theoretical errors in coupling parameters and neutron star observables and to determine the correlation coefficients.We observe that the neutron skins of ^(208)Pb and ^(48)Ca are strongly correlated and exhibit a strong dependence on J_(0),L(0)and the curvature of symmetry energy(K_(sym))as suggested from their correlations.A strong correlation of canonical mass neutron star radius,R1.4 with ρ-meson-nucleon coupling quantified by the term gpN and mixed interaction terms σ_(μ)ρ^(μ) and σ^(2)ρ_(μ)ρ^(μ) is also observed.
