Abstract
The Δ(1236) resonance plays an important role in saturating nuclear matter and in determining the properties of neutron star matter. In transition potential models, the Δ is explicitly excited and de-excited by predominantly tensor forces. The many-body aspects of these models suggest a simple prescription for calculating the energy in a two-body cluster approximation. With one parameter, we generate the energy of bulk matter as a function of total baryon density and neutron fraction. Nuclear matter saturates at subnuclear density with reasonable symmetry energy and estimated compressibility. Neutron matter is unbound at all densities and leads to appealing neutron star models. The extra degree of freedom associated with transition potential models may make it (too?) easy to obtain saturation of nuclear matter at nuclear matter density.
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