Constraints set on key parameters of the nuclear matter equation of state ( EoS ) by the values of the tidal deformability , inferred from GW170817 , are examined by using a diverse set of relativistic and non-relativistic mean field models .
These models are consistent with bulk properties of finite nuclei as well as with the observed lower bound on the maximum mass of neutron star \sim 2 ~ { } { M } _ { \odot } .
The tidal deformability shows a strong correlation with specific linear combinations of the isoscalar and isovector nuclear matter parameters associated with the EoS .
Such correlations suggest that a precise value of the tidal deformability can put tight bounds on several EoS parameters , in particular , on the slope of the incompressibility and the curvature of the symmetry energy .
The tidal deformability obtained from the GW170817 and its UV/optical/infrared counterpart sets the radius of a canonical 1.4 ~ { } { M } _ { \odot } neutron star to be 11.82 \leqslant R _ { 1.4 } \leqslant 13.72 km .