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We study the symmetry energy and the core-crust transition in neutron starsusing the finite-range Gogny nuclear interaction and examine the deducedcrustal thickness and crustal moment of inertia. We start by analyzing thesecond-, fourth- and sixth-order coefficients of the Taylor expansion of theenergy per particle in powers of the isospin asymmetry for Gogny forces. Thesecoefficients provide information about the departure of the symmetry energyfrom the widely used parabolic law. The neutron star core-crust transition isevaluated by looking at the onset of thermodynamical instability of the liquidcore. The calculation is performed with the exact (i.e., without Taylorexpansion) Gogny EoS for the core, and also with its Taylor expansion in orderto assess the influence of isospin expansions on locating the inner edge ofneutron star crusts. It is found that the properties of the core-crusttransition derived from the exact EoS differ from the predictions of the Taylorexpansion even when the expansion is carried through sixth order in the isospinasymmetry. Gogny forces, using the exact EoS, predict the ranges $0.094 \text{fm}^{-3} \lesssim \rho_t \lesssim 0.118\text{ fm}^{-3}$ for the transitiondensity and $0.339 \text{ MeV fm}^{-3} \lesssim P_t \lesssim 0.665 \text{ MeVfm}^{-3}$ for the transition pressure. The transition densities show ananticorrelation with the slope parameter $L$ of the symmetry energy. Thetransition pressures are not found to correlate with $L$. Neutron starsobtained with Gogny forces have maximum masses below $1.74M_\odot$ andrelatively small moments of inertia. The crustal mass and moment of inertia areevaluated and comparisons are made with the constraints from observed glitchesin pulsars.

Higher-order symmetry energy and neutron star core-crust transition with Gogny forces