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To relate constraints from nuclear physics to the tidal deformabilities ofneutron stars, we construct a neutron star model that accepts input from alarge collection of Skyrme density functions to calculate properties of 1.4solar-mass neutron stars. We find that restricting this set of Skyrme todensity functions that describe nuclear masses, isobaric analog states, and lowenergy nuclear reactions does not sufficiently restrict the predictedneutron-star radii and the tidal deformabilities. However, pressure constraintson the EoS around twice saturation density ($2\times2.74\times10^{14}g/cm^3$),obtained from high energy nucleus-nucleus collisions, does constrain predictedtidal deformabilities with uncertainties smaller than those obtained from theanalysis of GW170817. We also found that the density-pressure constraint on theEoS obtained from a recent analysis of the neutron-star merger event agree verywell with the density pressure constraints obtained from nuclear physicsexperiments published in 2002.

Laboratory Probes of the Neutron-Matter Equation of State