Stars freeze. But not all of them. Only some parts of some stars will. In white dwarfs and neutron stars, despite temperatures of millions of degrees, the densities and pressures are great enough to compact nuclei into a crystalline lattice millions of times more dense than any material on earth. Deeper still in neutron stars, near the nuclear saturation density, nuclei begin to touch and rearrange into non-spherical structures called 'nuclear pasta.' To interpret observations of neutron stars the composition and structure of the crystal and pasta layers must be understood, as the microscopic properties of the crust determine the macroscopic properties of the star, such as its thermal and electrical conductivity. At Indiana University, we perform computer simulations of these exotic astromaterials to calculate the physical properties of these stars.