  The observation of the gravitational wave signal GW170817, consistent with
emission from the inspiral of a binary neutron-star system, provided
information on the tidal deformation of the participating stars. The available
data may be exploited to constrain the equation of state of densenuclear
matter, as well as to shed light on the underlying models describing nuclear
dynamics at microscopic level. In this paper we compare the experimental
results to the predictions of different theoretical models, based on non
relativistic nuclear many-body theory, the relativistic field-theoretical
formalism, and a more phenomenological approach constrained by observed nuclear
properties. While the precision of the available data does not allow to resolve
the degeneracy of the models, our analysis shows a distinct sensitivity to the
star compactness predicted by the different equations of state, which turns out
to be significantly affected by relativistic boost corrections to the
nucleon-nucleon potential.
