Searches for continuous gravitational waves from neutron stars: A twenty-year retrospective

Wette, Karl

doi:10.1016/j.astropartphys.2023.102880

Cited by 14 publications

(4 citation statements)

References 285 publications

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“…where f 0 is the CW frequency (twice the rotational frequency in this model), d is the distance from the NS to the detector, and I = 10 38 kg m 2 is the canonical moment of inertia of an NS around the spinning axis [52] 2 . The results from this section could also be re-interpreted assuming other other emission mechanisms, such as r-modes or free precession [2,53].…”

Section: An Optimistic Cw Sourcementioning

confidence: 90%

“…The statistical properties of P are well-known. Assuming Gaussian noise, P α is the sum of the squares of two zero-mean unitary-variance Gaussian random variables; thus, chi-squared distribution with two degrees of freedom P α ∼ χ 2 2 follows. P, on the other hand, is the average of N SFT identical and independent random variables, with usually N SFT ∼ O(10 3 − 10 4 ).…”

Section: Characterizing the Visibility Of Continuous-wave Signalsmentioning

confidence: 99%

“…Continuous gravitational waves (CWs) are long-lasting gravitational wave (GW) signals whose detection remains, so far, unattained [1,2]. Among the expected sources, we find rapidly spinning non-axisymmetric neutron stars (NSs) [3], but also other more exotic ones such as evaporating boson clouds formed around spinning black holes [4,5], or planetary-mass compact binary systems [6,7].…”

Section: Introductionmentioning

confidence: 98%

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Assessing the Similarity of Continuous Gravitational-Wave Signals to Narrow Instrumental Artifacts

Jaume,

Tenorio,

Sintes

2024

Universe

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Continuous gravitational-wave (CW) signals are long-lasting quasi-monochromatic gravitational-wave signals expected to be emitted by rapidly rotating non-axisymmetric neutron stars. Depending on the rotational frequency and sky location of the source, certain CW signals may behave in a similar manner to narrow-band artifacts present in ground-based interferometric detectors. Part of the detector characterization tasks in the current generation of interferometric detectors (Advanced LIGO, Advanced Virgo, and KAGRA) aim at understanding the origin of these narrow artifacts, commonly known as "spectral lines". It is expected that similar tasks will continue after the arrival of next-generation detectors (e.g., Einstein Telescope and Cosmic Explorer). Typically, a fraction of the observed lines in a given detector can be associated to one or more instrumental causes; others, however, have an unknown origin. In this work, we assess the similarity of CW signals to spectral lines in order to understand whether a CW signal may be mistaken for a noise artifact. Albeit astrophysically unlikely, our results do not rule out the possibility of a CW signal being visible in the detector’s power spectrum.

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Section: An Optimistic Cw Sourcementioning

confidence: 90%

Section: Characterizing the Visibility Of Continuous-wave Signalsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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Assessing the Similarity of Continuous Gravitational-Wave Signals to Narrow Instrumental Artifacts

Jaume,

Tenorio,

Sintes

2024

Universe

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“…Continuous GW emission will help reveal properties of NSs such as composition (EoS), internal magnetic field, and viscosity, in addition to unveiling NSs that cannot be observed electromagnetically (e.g., Bonazzola and Gourgoulhon, 1996;Bildsten, 1998;Owen et al, 1998;Andersson and Kokkotas, 2001;Owen, 2005;Glampedakis and Gualtieri, 2018;Gittins et al, 2021;Morales and Horowitz, 2022;Riles, 2023, and references therein). Current searches for continuous GWs produced by spinning NSs with asymmetries improve with every LIGO-Virgo-KAGRA run (e.g., Abbott et al, 2022c) and dozens of known millisecond pulsars could come into the reach of nextgeneration GW detectors (Woan et al, 2018;Gupta et al, 2023a;Evans et al, 2023), with the potential of many more thanks to upcoming or next-generation electromagnetic facilities such as the next-generation Very Large Array (ngVLA; Murphy and ngVLA Science Advisory Council, 2020) and the Square Kilometre Array (Kalogera et al, 2019;Evans et al, 2023;Pagliaro et al, 2023;Riles, 2023;Wette, 2023). Detection by next-generation instruments also looks promising for bright low mass X-ray binaries such as Scorpius X-1 (Gupta et al, 2023a;Evans et al, 2023).…”

Section: New Frontiers In Mmamentioning

confidence: 99%

Multi-messenger astrophysics of black holes and neutron stars as probed by ground-based gravitational wave detectors: from present to future

Corsi,

Barsotti,

Berti

et al. 2024

Front. Astron. Space Sci.

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The ground-based gravitational wave (GW) detectors LIGO and Virgo have enabled the birth of multi-messenger GW astronomy via the detection of GWs from merging stellar-mass black holes (BHs) and neutron stars (NSs). GW170817, the first binary NS merger detected in GWs and all bands of the electromagnetic spectrum, is an outstanding example of the impact that GW discoveries can have on multi-messenger astronomy. Yet, GW170817 is only one of the many and varied multi-messenger sources that can be unveiled using ground-based GW detectors. In this contribution, we summarize key open questions in the astrophysics of stellar-mass BHs and NSs that can be answered using current and future-generation ground-based GW detectors, and highlight the potential for new multi-messenger discoveries ahead.

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Gravitational waves from neutron-star mountains

Gittins

2024

Class. Quantum Grav.

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Rotating neutron stars that support long-lived, non-axisymmetric deformations known as mountains have long been considered potential sources of gravitational radiation. However, the amplitude from such a source is very weak and current gravitational-wave interferometers have yet to witness such a signal. The lack of detections has provided upper limits on the size of the involved deformations, which are continually being constrained. With expected improvements in detector sensitivities and analysis techniques, there is good reason to anticipate an observation in the future. This review concerns the current state of the theory of neutron-star mountains. These exotic objects host the extreme regimes of modern physics, which are related to how they sustain mountains. We summarise various mechanisms that may give rise to asymmetries, including crustal strains built up during the evolutionary history of the neutron star, the magnetic field distorting the star's shape and accretion episodes gradually constructing a mountain. Moving beyond the simple rotating model, we also discuss how precession affects the dynamics and modifies the gravitational-wave signal. We describe the prospects for detection and the challenges moving forward.

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Searches for continuous gravitational waves from neutron stars: A twenty-year retrospective

Cited by 14 publications

References 285 publications

Assessing the Similarity of Continuous Gravitational-Wave Signals to Narrow Instrumental Artifacts

Assessing the Similarity of Continuous Gravitational-Wave Signals to Narrow Instrumental Artifacts

Multi-messenger astrophysics of black holes and neutron stars as probed by ground-based gravitational wave detectors: from present to future

Gravitational waves from neutron-star mountains

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