Exploring the Potential for Detecting Rotational Instabilities in Binary Neutron Star Merger Remnants with Gravitational Wave Detectors. (arXiv:2311.10626v1 [gr-qc])

Exploring the Potential for Detecting Rotational Instabilities in Binary Neutron Star Merger Remnants with Gravitational Wave Detectors. (arXiv:2311.10626v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Sasli_A/0/1/0/all/0/1">Argyro Sasli</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Karnesis_N/0/1/0/all/0/1">Nikolaos Karnesis</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Stergioulas_N/0/1/0/all/0/1">Nikolaos Stergioulas</a>

We explore the potential for detecting rotational instabilities in the
post-merger phase of binary neutron star mergers using different network
configurations of upgraded and next-generation gravitational wave detectors.
Our study employs numerically generated post-merger waveforms, which reveal the
re-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 colored
Gaussian noise and performing a reconstruction as a sum of wavelets using
Bayesian inference. Computing the overlap between the reconstructed and
injected signal, restricted to the instability part of the post-merger phase,
we find that one could infer the presence of rotational instabilities with a
network of planned 3rd-generation detectors, depending on the total mass and
distance to the source. For a recently suggested high-frequency detector
design, we find that the instability part would be detectable even at 200 Mpc,
significantly increasing the anticipated detection rate. For a network
consisting of the existing HLV detectors, but upgraded to twice the A+
sensitivity, we confirm that the peak frequency of the whole post-merger
gravitational-wave emission could be detectable with a network signal-to-noise
ratio of 8 at a distance of 40Mpc.

We explore the potential for detecting rotational instabilities in the
post-merger phase of binary neutron star mergers using different network
configurations of upgraded and next-generation gravitational wave detectors.
Our study employs numerically generated post-merger waveforms, which reveal the
re-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 colored
Gaussian noise and performing a reconstruction as a sum of wavelets using
Bayesian inference. Computing the overlap between the reconstructed and
injected signal, restricted to the instability part of the post-merger phase,
we find that one could infer the presence of rotational instabilities with a
network of planned 3rd-generation detectors, depending on the total mass and
distance to the source. For a recently suggested high-frequency detector
design, we find that the instability part would be detectable even at 200 Mpc,
significantly increasing the anticipated detection rate. For a network
consisting of the existing HLV detectors, but upgraded to twice the A+
sensitivity, we confirm that the peak frequency of the whole post-merger
gravitational-wave emission could be detectable with a network signal-to-noise
ratio of 8 at a distance of 40Mpc.

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