Neutron Stars. I. Properties at Absolute Zero Temperature

The properties of a neutron star at absolute zero temperature are discussed. The problem of determining the ground state of a neutron star is formulated in a general way and the conditions are described under which one might reasonably hope that an individual-particle model (which we adopt) is valid. The effects of the strong interactions on the number densities and production thresholds of the various hadrons are illustrated with several examples. The modification of the energy spectrum of neutrons and protons in a neutron star is calculated using an effective-mass approximation adapted from the theory of nuclear matter. Crude estimates are made of the contributions of hadrons other than nucleons to the equation of state and specific heat.