The properties of nuclear matter and dense neutron-star matter are studied by an approach which largely avoids the microscopic assumptions of nuclear-matter theory. The method is empirical, employing an extended form of the law of corresponding states to deduce the properties of nuclear systems from those of laboratory substances such as helium. It is possible to predict the solidification pressure and density, the compressibility, and the critical temperature of nuclear and neutron-star matter. As previously reported, a comparatively low solidification pressure is found for neutron-star matter, implying a solid core for most neutron stars. © 1974 The American Physical Society.