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The LIGO-Virgo collaboration ground-breaking detection of the binaryneutron-star merger event, GW170817, has intensified efforts towards theunderstanding of the equation of state (EoS) of nuclear matter. In this letter,we compare directly the density-pressure constraint on the EoS obtained from arecent analysis of the neutron-star merger event to density-pressureconstraints obtained from nuclear physics experiments. To relate constraintsfrom nuclear physics to the radii and the tidal deformabilities of neutronstars, we use a large collection of Skyrme density functionals that describeproperties of nuclei to calculate properties of 1.4 solar maass neutron stars.We find that restricting this set of Skyrme equations of state to densityfunctionals that describe nuclear masses, isobaric analog states, and lowenergy nuclear reactions does not sufficiently restrict the predictedneutron-star radii and the tidal deformabilities. Including pressureconstraints on the EoS around twice saturation density, obtained from highenergy nucleus-nucleus collisions, does constrain predicted radii and tidaldeformabilities to be consistent with the results obtained from the analysis ofGW170817. We discuss how new measurements of nucleus-nucleus collisions canimprove these constraints on the EoS to be more restrictive than the currentconstraints from the GW170817 merger event.

Constraining neutron-star equation of state using heavy-ion collisions