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

Effects of nuclear symmetry energy and equation of state on neutron star properties