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We explore the potential for detecting rotational instabilities in thepost-merger phase of binary neutron star mergers using different networkconfigurations of upgraded and next-generation gravitational wave detectors.Our study employs numerically generated post-merger waveforms, which reveal there-excitation of the $l=m=2$ $f$-mode at a time of $O(10{\rm})$ms after merger.We evaluate the detectability of these signals by injecting them into coloredGaussian noise and performing a reconstruction as a sum of wavelets usingBayesian inference. Computing the overlap between the reconstructed andinjected signal, restricted to the instability part of the post-merger phase,we find that one could infer the presence of rotational instabilities with anetwork of planned 3rd-generation detectors, depending on the total mass anddistance to the source. For a recently suggested high-frequency detectordesign, we find that the instability part would be detectable even at 200 Mpc,significantly increasing the anticipated detection rate. For a networkconsisting of the existing HLV detectors, but upgraded to twice the A+sensitivity, we confirm that the peak frequency of the whole post-mergergravitational-wave emission could be detectable with a network signal-to-noiseratio of 8 at a distance of 40Mpc.

Exploring the Potential for Detecting Rotational Instabilities in Binary Neutron Star Merger Remnants with Gravitational Wave Detectors