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In this work we study the effect of the symmetry energy on several propertiesof neutron stars. First, we discuss its effect on the density, proton fractionand pressure of the neutron star crust-core transition. We show that whereasthe first two quantities present a clear correlation with the slope parameter$L$ of the symmetry energy, no satisfactory correlation is seen between thetransition pressure and $L$. However, a linear combination of the slope andcurvature parameters at $\rho=0.1$ fm$^{-3}$ is well correlated with thetransition pressure. In the second part we analyze the effect of the symmetryenergy on the pasta phase. It is shown that the size of the pasta clusters,number of nucleons and the cluster proton fraction depend on the densitydependence of the symmetry energy: a small $L$ gives rise to larger clusters.The influence of the equation of state at subsaturation densities on theextension of the inner crust of the neutron star is also discussed. Finally,the effect of the effect of the density dependence of the symmetry energy onthe strangeness content of neutron stars is studied in the last part of thework. It is found that charged (neutral) hyperons appear at smaller (larger)densities for smaller values of the slope parameter $L$. A linear correlationbetween the radius and the strangeness content of a star with a fixed mass isalso found.

Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars