Hyperon stars in the Brueckner-Bethe-Goldstone theory

Abstract

In the framework of the Brueckner-Bethe-Goldstone theory, we determine a fully microscopic equation of state for asymmetric and $\beta$-stable nuclear matter containing $\sim$ and $\la$ hyperons. We use the Paris and the new Argonne $A{v}_{18}$ two-body nucleon interaction, whereas the nucleon-hyperon interaction is described by the Njimegen soft-core model. We stress the role played by the three-body nucleon interaction, which produces a strong repulsion at high densities. This enhances enormously the hyperon population, and produces a strong softening of the equation of state, which turns out almost independent on the nucleon-nucleon interaction. We use the new equation of state in order to calculate the structure of static neutron stars. We obtain a maximum mass configuration with $M_{\max }$ = 1.26 (1.22) when the Paris ($A{v}_{18}$) nucleon potential is adopted. Central densities are about 10 times normal nuclear matter density. Stellar rotations, treated within a perturbative approach, increase the value of the limiting mass by about 12%.

16 pages, latex, 10 figures, submitted to Phys. Rev. C

References in corpus (1)

• Asymmetric Nuclear Matter from Extended Brueckner-Hartree-Fock Approach

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