Tidal interactions during neutron star mergers: equation of state considerations

We review the possible constraints on the neutron star structure that can be inferred from various gravitational wave and electromagnetic observables during a binary neutron star merger. We focus particularly on examining the sensitivity of the tidal polarizability of neutron stars to the equation of state (EOS) of dense matter at more than 2-3 times nuclear saturation density, concluding that particularly soft or stiff high density EOSs can be distinguished by advanced LIGO observations of the gravitational wave signal immediately pre-merger. We also discuss neutron star structure effects on dynamical tides and crust shattering events during the inspiral phase, the latter of which has been proposed as a possible EM precursor to short GRBs.