Narrow Results

The properties of neutron star are studied in the framework of relativistic Hartree–Fock (RHF) model with realistic nucleon–nucleon (NN) interactions, i.e., Bonn potentials. The strong repulsion of NN interaction at short range is properly removed by the unitary correlation operator method (UCOM). Meanwhile, the tensor correlation is neglected due to the very rich neutron environment in neutron star, where the total isospin of two nucleons can be approximately regarded as $T=1$. The equations of state of neutron star matter are calculated in $\beta$ equilibrium and charge neutrality conditions. The properties of neutron star, such as mass, radius and tidal deformability, are obtained by solving the Tolman–Oppenheimer–Volkoff equation and tidal equation. The maximum masses of neutron from Bonn A, B, C potentials are around $2.2M_{\odot }$. The radius are $12.40-12.91$km at $1.4M_{\odot }$, respectively. The corresponding tidal deformabilities are ${\mathrm{\Lambda }}_{1.4}=293-355$. All of these properties are satisfied with the recent observables from the astronomical and gravitational wave devices and are consistent with the results from the relativistic Brueckner–Hartree–Fock model.

Nuclear matter is studied by using beyond relativistic Hartree-Fock (RHF) model with the realistic nucleon-nucleon (NN) interaction. We use the unitary correlation operator method (UCOM) to treat the strong repulsive interaction in the short-range region between two nucleons. We find that the equation of state (EOS) of pure neutron matter is completely comparable with the results of Dirac-Brueckner-Hartree-Fock (DBHF) theory. However, for the symmetric nuclear matter, the EOS is largely different from the DBHF result particularly in the low density region.