Gravitational-wave signals from binary neutron star coalescences carry information about the star's equation of state (EoS) in their tidal signatures. To be able to extract this crucial knowledge from LIGO/Virgo data, waveform models need to accurately describe tidal interactions. In this talk I will summarize how matter effects are included in state of the art models for inspiral and postmerger waveforms. I will then discuss the prospects of constraining the EoS with next generation detectors, and argue that current inspiral models -- including those from numerical relativity -- are insufficient to unequivocally infer EoS constraints from Gravitational wave parameter estimation from the loudest (and potentially most informative) events.