The equation of state of the neutron gas is calculated by a variational method, using the Hamada–Johnson 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.
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Binder et al. (1969) studied this question.
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