Equation of State for low density nuclear matter

Neutron-rich matter at subnuclear densities---present in core-collapse supernovae and the crust of neutron stars---displays fascinating complex structures such as spherical, slablike, and rodlike shapes. The equation of state and the two-body correlation function (both spin dependent and spin independent) are computed via semi-classical Monte-Carlo simulations that incorporate a momentum-dependent two-body potential to simulate Pauli correlations.