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.