For 1.4 solar mass neutron stars the radius-deformability relation is nearly independent of higher-order nuclear parameters but strongly depends on the symmetry energy slope L, and the relation fails for 1.8 solar mass stars.
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The key factor to determine the relation between radius and tidal deformability of neutron stars: slope of symmetry energy
For 1.4 solar mass neutron stars the radius-deformability relation is nearly independent of higher-order nuclear parameters but strongly depends on the symmetry energy slope L, and the relation fails for 1.8 solar mass stars.