Nuclear pasta and symmetry energy in the relativistic point-coupling model

Thermodynamically Consistent Equation of State for an Accreted Neutron Star Crust

“…At larger pressures, P > P inst , the crust can be continued by "relic" layers that are not replaced by the accreted material in the FAC regime. These layers are formed at the initial stages of accretion and can be composed of the spherical nuclei or more complicated nuclear shapes referred to as "pasta" (see, e.g., [41][42][43][44][45][46][47][48][49][50] for a recent discussion of pasta in pristine crust). Clearly, the unambiguous determination of the composition of these layers requires consideration of their formation, which is beyond the scope of the present paper.…”

The hyperonic star in relativistic mean-field model

“…When the nucleon density approaches ρ 0 /2, heavy nuclei dissolve and the neutron star matter becomes homogeneous, which corresponds to the outer core of neutron star. It plays an essential role in determining the mass and radius of the neutron star [37][38][39][40][41]. In the inner core region, the baryons including the strangeness degree of freedom, such as Λ, Σ, and Ξ hyperons, will be present, when the Fermi energies of nucleons are larger than their chemical potentials, which is also called as a hyperonic star.…”

Nonlinear point-coupling interaction for the relativistic Hartree-Bogoliubov approach

“…The most widely used effective interactions serving as the mean-field potential of the RMF and RHB frameworks are the meson-exchange [24,25,26,27,28,29,30]. In recent years, the point-coupling model offers an alternative to the meson-exchange model as the exchange of heavy mesons associated with short-distance dynamics cannot be resolved at low energies [14,18,31,32,33,34,35,36,37,38,39,40]. The presently and commonly used point-coupling parameterized interactions include PC-PK1 [14], PC-F1 [18], PC-LA [31], and DD-PC1 [33].…”