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Within the parameter space of equation of state (EOS) of dense neutron-richmatter limited by existing constraints mainly from terrestrial nuclearexperiments, we investigate how the neutron star maximum mass$M_{\rm{max}}>2.01\pm0.04$ M$_\odot$, radius $10.62<R_{\rm{1.4}}< 12.83$ km andtidal deformability $\Lambda_{1.4}\leq800$ of canonical neutron stars alltogether constrain the EOS of dense neutron-rich nucleonic matter. While the3-D parameter space of $K_{\rm{sym}}$ (curvature of nuclear symmetry energy),$J_{\rm{sym}}$ and $J_0$ (skewness of the symmetry energy and EOS of symmetricnuclear matter, respectively) are narrowed down significantly by theobservational constraints, more data are needed to pin down the individualvalues of $K_{\rm{sym}}$, $J_{\rm{sym}}$ and $J_0$ with quantifieduncertainties. The $J_0$ largely controls the maximum mass of neutron stars.While the EOS with $J_0=0$ is sufficiently stiff to support neutron stars asmassive as 2.37 M$_{\odot}$, to support the hyperthetical ones as massive as2.74 M$_{\odot}$ (composite mass of GW170817) requires $J_0$ to be larger thanits currently known maximum value of about 400 MeV and beyond the causalitylimit. The upper limit on the tidal deformability of $\Lambda_{1.4}=800$ fromthe recent observation of GW170817 is found to provide upper limits on some EOSparameters consistent with but far less restrictive than the existingconstraints of other observables studied.

Combined Constraints on the Equation of State of Dense Neutron-Rich Matter from Terrestrial Experiments and Observations of Neutron Stars