  We study the effects of nuclear symmetry energy on the mass-radius relation
and tidal deformability of neutron stars, considering the self-consistency of
the equation of state (EOS). We first construct a set of unified EOSs based on
relativistic mean-field models with different density dependence of the
symmetry energy. For the description of pasta phases appearing in the inner
crust of neutron stars, we perform a self-consistent Thomas-Fermi calculation
using the same nuclear interaction as that for the uniform matter in the core.
To examine possible effects from the self-consistency of the EOS on
neutron-star properties, we separately investigate the impacts of crust and
core segments. By matching the same core EOS to different crust EOSs, it is
found that neutron-star radii are significantly affected by the crust segment.
On the other hand, the neutron-star radii are also strongly dependent on the
core EOS. However, the correlation between the radius and the symmetry energy
slope of the core EOS is opposite to that of the crust EOS. It is likely that
the nuclear model with a small slope parameter is favored by recent
astrophysical observations.
