  In this work we study the effect of the symmetry energy on several properties
of neutron stars. First, we discuss its effect on the density, proton fraction
and pressure of the neutron star crust-core transition. We show that whereas
the first two quantities present a clear correlation with the slope parameter
$L$ of the symmetry energy, no satisfactory correlation is seen between the
transition pressure and $L$. However, a linear combination of the slope and
curvature parameters at $\rho=0.1$ fm$^{-3}$ is well correlated with the
transition pressure. In the second part we analyze the effect of the symmetry
energy 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 density
dependence of the symmetry energy: a small $L$ gives rise to larger clusters.
The influence of the equation of state at subsaturation densities on the
extension 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 on
the strangeness content of neutron stars is studied in the last part of the
work. It is found that charged (neutral) hyperons appear at smaller (larger)
densities for smaller values of the slope parameter $L$. A linear correlation
between the radius and the strangeness content of a star with a fixed mass is
also found.
