  During the final stages of a neutron-star binary coalescence, stellar
quasi-normal modes can become resonantly excited by tidal fields. If the strain
exerted by the excited modes exceeds the extent to which the crust can respond
linearly, localised crustal failures may occur. In this work, we re-examine
resonant $g$-mode excitations of relativistic neutron stars in the last $\sim$
10 seconds of an inspiral. We adopt realistic equations of state that pass
constraints from GW170817, include 3rd order post-Newtonian terms for the
conservation orbital motion, and employ a 2.5 post-Newtonian scheme for
gravitational back-reaction. Frequency modulations of the modes due to tidal
fields, Lorentz forces, and (slow) rotation are also considered to investigate
the maximal strain achievable by resonantly-excited $g$-modes. Depending on the
equation of state, degree of stratification, and stellar magnetic field, we
find that certain $g$-modes excitations may be able to break the crust some
seconds prior to coalescence.
