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The most popular Gogny parametrizations, namely D1S, D1N and D1M, describeaccurately the ground-state properties of spherical and deformed finite nucleiall across the mass table obtained with Hartree--Fock--Bogoliubov (HFB)calculations. However, these forces produce a rather soft equation of state(EoS) in neutron matter, which leads to predict maximum masses of neutron starswell below the observed value of two solar masses. To remove this limitation,we built new Gogny parametrizations by modifying the density dependence of thesymmetry energy predicted by the force in such a way that they can be appliedto the neutron star domain and can also reproduce the properties of finitenuclei as good as their predecessors. These new parametrizations allow us toobtain stiffer EoS's based on the Gogny interactions, which predict maximummasses of neutron stars around two solar masses. Moreover, other globalproperties of the star, such as the moment of inertia and the tidaldeformability, are in harmony with those obtained with other well tested EoSsbased on the SLy4 Skyrme force or the Barcelona--Catania--Paris--Madrid (BCPM)energy density functional. Properties of the core-crust transition predicted bythese Gogny EoSs are also analyzed. Using these new Gogny forces, the EoS inthe inner crust is obtained with the Wigner--Seitz approximation in theVariational Wigner--Kirkwood approach along with the Strutinsky integralmethod, which allows one to estimate in a perturbative way the proton shell andpairing corrections. For the outer crust, the EoS is determined basically bythe nuclear masses, which are taken from the experiments, wherever they areavailable, or by HFB calculations performed with these new forces if theexperimental masses are not known.

Unified Equation of State for Neutron Stars Based on the Gogny Interaction