An essential component of the equation of state (EOS) of isospin asymmetric nuclear matter is nuclear symmetry energy. It influences the structure of neutron stars and finite nuclei. We perform qualitative investigations within chiral forces and do Brueckner-Hartree-Fock calculations for nuclear and neutron matter EOS in order to further our understanding of the influence of the symmetry energy on nuclear ... Read more

Using an expanded Brueckner–Hartree–Fock (BHF) framework with a phenomenological three-body force (3BF), we study the microscopic characteristics and equation of state (EOS) of symmetric nuclear and neutron matter. Both symmetric nuclear and pure neutron matter are used in the G-matrix computations, which are carried out by adding the 3BF to the initial two-body force (2BF) and employing a partial wave ... Read more