Extended Skyrme interactions for nuclear matter, finite nuclei and neutron stars

Abstract

Recent progress in theory, experiment and observation challenges the mean field models using the conventional Skyrme interaction, suggesting that the extension of the conventional Skyrme interaction is necessary. In this work, by fitting the experimental data of a number of finite nuclei together with a few additional constraints on nuclear matter using the simulated annealing method, we construct three Skyrme interaction parameter sets, namely, eMSL07, eMSL08 and eMSL09, based on an extended Skyrme interaction which includes additional momentum and density dependent two-body forces to effectively simulate the momentum dependence of the three-body force. The three new interactions can reasonably describe the ground-state properties and the isoscalar giant monopole resonance energies of various spherical nuclei used in the fit as well as the ground-state properties of many other spherical nuclei, nicely conform to the current knowledge on the equation of state of asymmetric nuclear matter, eliminate the notorious unphysical instabilities of symmetric nuclear matter and pure neutron matter up to a very high density of $1.2$ fm${}^{-3}$, and simultaneously support heavier neutron stars with mass larger than two times solar mass. One important difference of the three new interactions is about the prediction of the symmetry energy at supra-saturation densities, and these new interactions are thus potentially useful for the determination of the largely uncertain high-density symmetry energy in future. In addition, a comparison is made for the predictions of nuclear matter, finite nuclei and neutron stars with the three new interactions versus those with three typical interactions BSk22, BSk24 and BSk26 from Brussels group.

18 pages, 6 figures, 5 tables. Results and discussions added. Accepted version to appear in PRC

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• From neutron skins and neutron matter to the neutron star crust
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• Impact of initial fluctuations and nuclear deformations in isobar collisions
• Relativistic self-energy decomposition of nuclear symmetry energy and equation of state of neutron matter within QCD sum rules
• Evidence for strong isovector nuclear spin-orbit interaction
• New Skyrme parametrizations to describe finite nuclei and neutron star matter with realistic effective masses
• Neutron matter within QCD sum rules
• Impact of choices for center-of-mass correction energy on the surface energy of Skyrme energy density functionals
• Probing neutron skin and symmetry energy with relativistic isobar collisions
• Constraining the Hadron-Quark Phase Transition Chemical Potential via Astronomical Observation
• Skewness of nuclear matter and three-particle correlations
• The restriction of ${\sigma }^{\ast }$ and $\varphi$ on the protoneutron stars PSR J0348+0432
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• Effects of isovector spin-orbit interaction on the charge-weak form factor difference in ${}^{48}$Ca, ${}^{208}$Pb, ${}^{90}$Zr and ${}^{62}$Ni
• Effects of isoscalar- and isovector-scalar meson mixing on neutron star structure