Nuclear matter EOS with light clusters within the mean-field approximation
The crust of a neutron star is essentially determined by the low-density region ($ρ<ρ_0\approx0.15-0.16\unit{fm}^{-3}$) of the equation of state. At the bottom of the inner crust, where the density is $ρ\lesssim0.1ρ_0$, the formation of light clusters in nuclear matter will be energetically favorable at finite temperature. At very low densities and moderate temperatures, the few body correlations are expected to become important and light nuclei like deuterons, tritons, helions and $α$-particles will form. Due to Pauli blocking, these clusters will dissolve at higher densities $ρ\gtrsim 0.1ρ_0$. The presence of these clusters influences the cooling process and quantities, such as the neutrino emissivity and gravitational waves emission. The dissolution density of these light clusters, treated as point-like particles, will be studied within the Relativistic Mean Field approximation. In particular, the dependence of the dissolution density on the clusters-meson couplings is studied.