A Theory of highly condensed matter
197439 pages
Published in:
- Annals Phys. 83 (1974) 491-529
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Abstract: (Elsevier)
To discuss properties of cold, condensed stellar objects such as neutron stars, it is necessary to know the stress tensor T μν , the source in Einstein's field equations, from nuclear matter densities upwards. To overcome some of the difficulties with the conventional many-body approach to this problem, a model relativistic, many-body, quantum field theory composed of a baryon field, a neutral scalar meson field coupled to the scalar density ψ ψ , and a neutral vector meson field coupled to the conserved baryon current i Ψ γλψ is developed. For a uniform system of given baryon density ϱ B , the linearized theory obtained by replacing the scalar and vector fields by their expectation pectation values, φ → φ 0 , V λ → iδ λ 4 V 0 can be solved exactly. The resulting equation of state for nuclear matter exhibits nuclear saturation, and if the two dimensionless coupling constants in this theory are matched to the binding energy and density of nuclear matter, predictions are obtained for all other systems at all densities. In particular, neutron matter is unbound and the equation of state for neutron matter at all densities is presented; it extrapolates smoothly into the relativistic form P = ϵ . Comparison is made with some conventional many-body calculations.References(50)
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