Equation of State of the Nuclear Pasta

Pasta phase -- the neutron-rich matter at subnuclear densities present in the core-collapse supernovae and the crust of neutron stars -- displays fascinating complex structures. The equation of state and the two-body spin-isospin dependent correlation function in the nuclear pasta are computed via semi-classical Monte Carlo simulation that incorporates a ``semi classical'' short-range spin-dependent term to simulate Pauli correlations.