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Gamma-ray bursts resulting from binary neutron-star mergers are sometimespreceded by precursor flares. These harbingers may be ignited by quasi-normalmodes, excited by orbital resonances, shattering the stellar crust of one ofthe inspiralling stars up to $\gtrsim10$ seconds before coalescence. In therare case that a system displays two precursors, successive overtones of eitherinterface- or $g$-modes may be responsible for the overstrainings. Since thefree-mode frequencies of these overtones have an almost constant ratio, and theinertial-frame frequencies for rotating stars are shifted relative to staticones, the spin frequency of the flaring component can be constrained as afunction of the equation of state, the binary mass ratio, the mode quantumnumbers, and the spin-orbit misalignment angle. As a demonstration of themethod, we find that the precursors of GRB090510 hint at a spin frequency rangeof $2 \lesssim \nu_{\star}/\text{Hz} \lesssim 20$ for the shattering star if weallow for an arbitrary misalignment angle, assuming $\ell=2$ $g$-modes accountfor the events.

Measuring spin in coalescing binaries of neutron stars showing double precursors