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