ABSTRACT
Most of the mass of the star is contributed by highly compressed matter at nuclear and supernuclear densities. The surface and crust regions of neutron stars are so thin that these contribute only little to the bulk properties like masses, radii, moments of inertia, and limiting rotational periods of the more massive members of a neutron star sequence. Gravity compresses the matter in the cores of the neutron stars to densities between 9 to 13 times the densities of ordinary nuclear matter. The particle populations must arrange themselves in such a way as to minimize the energy density in accord with electric charge neutrality and chemical equilibrium. The intense magnetic fields that are believed to exist on the surfaces of neutron stars will plausibly modify the structure of bulk matter. Abrahams and Shapiro improved on previous statistical calculations of the equation of state of matter subject to such strong magnetic fields.
