M. Baldo

Hyperon stars in the Brueckner-Bethe-Goldstone theory

In the framework of the Brueckner-Bethe-Goldstone theory, we determine a fully microscopic equation of state for asymmetric and

Superfluidity in neutron matter and nuclear matter with realistic interactions

\beta

Medium Polarization Effects on Neutron Matter Superfluidity

-stable nuclear matter containing

Hadron-quark phase transition in dense matter and neutron stars

\sim

Proton and neutron superfluidity in neutron star matter

and

3 P 2 − 3 F 2 pairing in neutron matter with modern nucleon-nucleon potentials

\la

Bethe-Brueckner-Goldstone expansion in neutron matter

hyperons. We use the Paris and the new Argonne

Low densities in nuclear and neutron matters and in the nuclear surface

Av_{18}

Off-the-energy-shell properties of the mass operator and spectral functions in nuclear matter

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

The nuclear symmetry energy

M_{\rm max}