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The observation of the gravitational wave signal GW170817, consistent withemission from the inspiral of a binary neutron-star system, providedinformation on the tidal deformation of the participating stars. The availabledata may be exploited to constrain the equation of state of densenuclearmatter, as well as to shed light on the underlying models describing nucleardynamics at microscopic level. In this paper we compare the experimentalresults to the predictions of different theoretical models, based on nonrelativistic nuclear many-body theory, the relativistic field-theoreticalformalism, and a more phenomenological approach constrained by observed nuclearproperties. While the precision of the available data does not allow to resolvethe degeneracy of the models, our analysis shows a distinct sensitivity to thestar compactness predicted by the different equations of state, which turns outto be significantly affected by relativistic boost corrections to thenucleon-nucleon potential.

Tidal Deformation of Neutron Stars from Microscopic Models of Nuclear Dynamics