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With the first detections of binary neutron star mergers bygravitational-wave detectors, it proves timely to consider how the internalstructure of neutron stars affects the way in which they can be asymmetricallydeformed. Such deformations may leave measurable imprints on gravitational-wavesignals and can be sourced through tidal interactions or the formation ofmountains. We detail the formalism that describes fully-relativistic neutronstar models with elastic crusts undergoing static perturbations. This formalismprimes the problem for studies into a variety of mechanisms that can deform aneutron star. We present results for a barotropic equation of state and arealistic model for the elastic crust, which enables us to compute relevantquantities such as the tidal deformability parameter. We find that theinclusion of an elastic crust provides a very small correction to the tidaldeformability. The results allow us to demonstrate when and where the cruststarts to fail during a binary inspiral and we find that the majority of thecrust will remain intact up until merger.

Tidal deformations of neutron stars with elastic crusts