Abstract
We analyze the effect of the tensor force and other components of the nucleon-nucleon interaction on the nuclear symmetry energy and its density dependence by using the Hellmann–Feynman theorem. The analysis is performed within the microscopic Brueckner–Hartree–Fock approach using the Argonne V18 potential plus a Urbana IX three-nucleon force. Our results show that the potential part of the nuclear Hamiltonian, and in particular its tensor component, gives the largest contribution to the symmetry energy. The decomposition of the symmetry energy into a kinetic part and a potential energy part provides physical insight on the correlated nature of the system, indicating that pure neutron matter is less correlated than symmetric nuclear matter.
Highlights
The density dependence of the nuclear symmetry energy, Esym (ρ), is a crucial ingredient of the nuclear equation of state (EoS) needed to understand many important properties of isospin-rich nuclear systems such as exotic nuclei, supernovae and neutron stars [1,2,3,4]
We explore the different effects of NN correlations on symmetric nuclear matter (SNM) and pure neutron matter (PNM) and discuss how the isospin dependence of these correlations affects the density dependence of the nuclear symmetry energy
In this work we have analyzed the effect of the tensor force and other components of the nucleon-nucleon (NN) interaction on the nuclear symmetry energy and its slope parameter for a wide range of densities
Summary
The density dependence of the nuclear symmetry energy, Esym (ρ), is a crucial ingredient of the nuclear equation of state (EoS) needed to understand many important properties of isospin-rich nuclear systems such as exotic nuclei, supernovae and neutron stars [1,2,3,4]. In this work we analyze the effect of the tensor force and other components of the NN interaction on Esym (ρ), and discuss how the isospin dependence of the NN correlations affects it This analysis is carried out with the help of the Hellmann–Feynman theorem [6,7] within the framework of the microscopic Brueckner–Hartree–Fock (BHF) approach [8,9]. We explore the different effects of NN correlations on SNM and PNM and discuss how the isospin dependence of these correlations affects the density dependence of the nuclear symmetry energy To such end we compare the kinetic and potential energy contributions with those of the free Fermi gas and the so-called correlation energy.
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