A theory of highly condensed matter

Superfluid condensation energy of neutron matter

As indicated by the title, this article is primarily concerned with nuclear matter calculations. I have tried to discuss enough of the theory to make it reasonably self-contained, especially at the level of explaining the physical ideas underlying the development. The reader who wishes more detail may find it rewarding to consult the set of articles in Reviews of Modern Physics for October 1967 (Day 67, RB 67, Bra 67). On a subject on which so much has been written it is difficult to adequately review all the material, and I have not really attempted to do so. I have referred to the papers that were useful or helpful to me, of which as you will see there are a fair number. Undoubtedly there is a larger number not referred to, either because I do not know of them or else they did not come to mind as I was writing. Hopefully their authors will not be too put out. What results is my personal view of the subject.

Nuclear Matter Calculations

Neutron matter: Binding energy and magnetic susceptibility

Properties of the neutron gas and applications to neutron stars

The equation of state of the neutron gas is calculated by a variational method, using the HamadaJohnson potential for the two-nucleon interaction. The energy-density relation determined in this way is valid for low and moderate densities. This result is extrapolated to higher densities and is joined smoothly to the relativistic energy-density relation for free particles. The critical mass of neutron stars is obtained by integrating the general relativistic equations for hydrostatic equilibrium using the equation of state. The critical mass is found to be less than 0.7 of the mass of the Sun.

M. Razavy

Papers

Equation of state of neutron gas and the critical mass of neutron stars