  The LIGO/Virgo detection of gravitational waves originating from a
neutron-star merger, GW170817, has recently provided new stringent limits on
the tidal deformabilities of the stars involved in the collision. Combining
this measurement with the existence of two-solar-mass stars, we generate a
generic family of neutron-star-matter Equations of State (EoSs) that
interpolate between state-of-the-art theoretical results at low and high baryon
density. Comparing the results to ones obtained without the tidal-deformability
constraint, we witness a dramatic reduction in the family of allowed EoSs.
Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass
neutron star is 13.6 km, and that smallest allowed tidal deformability of a
similar-mass star is $\Lambda(1.4 M_\odot) = 120$.
