Nuclear symmetry energy and the role of three-body forces

Abstract

Density dependence of nuclear symmetry energy as well as its partial wave decomposition is studied within the framework of lowest-order constrained variational (LOCV) method using AV18 two-body interaction supplemented by UIX three-body force. The main focus of the present work is to introduce a revised version of three-body force which is based on an isospin-dependent parametrization of coefficients in the UIX force, in order to overcome the inability to produce correct saturation-point parameters} in the framework of LOCV method. We find that employing the new model of {\ph three-body force} in the LOCV formalism leads to successfully reproducing the semi-empirical parameters of cold nuclear matter, including} $E_{sym}({\rho }_0)$, $L$, and $K_{sym}$. All our models of three-body force combined with AV18 two-body force give maximum neutron star mass higher than $2M_{\odot }$. The fraction of protons in the nucleon cores of neutron stars strongly depends on the three-body force parametrization.

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• The nuclear symmetry energy from relativistic Brueckner-Hartree-Fock model
• Nuclear matter calculations with the phenomenological three-nucleon interaction
• Hyperons in Neutron Stars across the observed mass range: Insights from realistic $\Lambda$-N and $\Lambda$-$\Lambda$ interactions within a Microscopic Framework
• Thermal impacts on the properties of nuclear matter and young neutron star