Kavli Affiliate: Lijing Shao
| First 5 Authors: Garvin Yim, Lijing Shao, Renxin Xu, ,
| Summary:
Glitching pulsars are expected to be important sources of gravitational
waves. In this paper, we explore six different models that propose the emission
of transient continuous waves, lasting days to months, coincident with
glitches. The maximal gravitational wave energy is calculated for each model,
which is then used to determine whether associated gravitational waves could be
detectable with LIGO-Virgo-KAGRA’s O4 detectors. We provide an analytical
approximation to calculate the signal-to-noise ratio which includes information
about the source’s sky position, improving on previous estimates that assume
isotropic or sky and orientation averaged sensitivities. By analysing the
entire glitching population, we find that certain models predict detectable
signals in O4, whereas others do not. We also rank glitching pulsars by
signal-to-noise ratio, based on archival data, and we find that for all models,
the Vela pulsar (PSR J0835$-$4510) would provide the strongest signal.
Moreover, PSR J0537$-$6910 is not expected to yield a detectable signal in O4,
but will start becoming relevant for next generation detectors. Our analysis
also extends to the entire pulsar population, regardless of whether they have
glitched, and we provide a list of pulsars that would present a significant
signal, if they were to glitch. Finally, we apply our analysis to the April
2024 Vela glitch and find that a signal should be detectable under certain
models. The non-detection of a supposedly detectable signal would provide an
efficiency factor that quantifies a model’s contribution to gravitational wave
emission, eventually leading to a differentiation of models and independent
constraints on physical parameters.
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