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We discuss the role of dynamical tidal effects for inspiralling neutron starbinaries, focussing on features that may be considered "unmodelled" ingravitational-wave searches. In order to cover the range of possibilities, weconsider i) individual oscillation modes becoming resonant with the tide, ii)the elliptical instability, where a pair of inertial modes exhibit a nonlinearresonance with the tide, and iii) the non-resonant p-g instability which mayarise as high order p- and g-modes in the star couple nonlinearly to the tide.In each case, we estimate the amount of additional energy loss that needs to beassociated with the dynamical tide in order for the effect to impact on anobserved gravitational-wave signal. We explore to what extent the involvedneutron star physics may be considered known and how one may be able to useobservational data to constrain theory.

Using gravitational-wave data to constrain dynamical tides in neutron star binaries