## Tabulated Equations of State

The nuclear matter equation of state is the fundamental input for building models of neutron stars according to the Einstein's general theory of relativity. In fact typical properties like masses and radii depend strongly on the equation of state at densities 8-10 times larger than the nuclear matter saturation density.

For this purpose we have developed a microscopic equation of state for nuclear matter using the Brueckner-Bethe-Goldstone many-body theory, including modern nucleonic two and three-body forces.

Below you may find and download a set of equations of state in tabular form.

ASYMMETRIC, BETA-STABLE and CHARGE NEUTRAL MATTER at T=0.

This is obtained using the Argonne v_{18}nucleon-nucleon potential, supplemented by a three-body force derived in the Urbana model.

HYPERNUCLEAR, BETA-STABLE and CHARGE NEUTRAL MATTER at T=0.

The appearance of strange baryons softens dramatically the equation of state.

This has been derived using the Argonne v

_{18}nucleon-nucleon potential, supplemented by the Urbana three-body force, and the Njimegen soft-core potential as nucleon-hyperon interaction. No hyperon-hyperon interaction is included.ASYMMETRIC, BETA-STABLE and CHARGE NEUTRAL MATTER at finite T.

It has been derived in the framework of the Bloch-De Dominicis many-body approach for the scattering matrix at finite temperature. The Argonne v_{18}nucleon-nucleon potential has been used, and supplemented by a three-body force as in the Urbana model.

HYPERNUCLEAR, BETA-STABLE and CHARGE NEUTRAL MATTER at finite T.

The Bloch-De Dominicis approach has been used, with the Frozen Correlation Approximation for the self-consistent mean field. The Argonne v

_{18}nucleon-nucleon potential has been used, supplemented by the Urbana three-body force, and the Njimegen soft-core potential as nucleon-hyperon interaction. No hyperon-hyperon interaction is included.