Continuous gravitational waves from Galactic neutron stars: demography, detectability and prospects

Gianluca, Pagliaro,; Papa, M. A.; Jiang, Ming; Lian, Jianhui; Tsuna, D.; Maraston, Claudia; Thomas, Daniel

doi:10.48550/arxiv.2303.04714

Cited by 2 publications

(3 citation statements)

References 109 publications

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“…Depending on the assumptions, the nearest unknown neutron star could be as close as ≈10 pc (Dergachev & Papa 2020;Pagliaro et al 2023), where this search probes the interesting region of ellipticities between 10 −7 and 10 −9 for sufficiently Overall, ellipticities at the level of 10 −6 are usually considered reasonable, and the reach of this search for objects with this deformation and rotating faster than 150 Hz is 1 kpc.…”

Section:  -mentioning

confidence: 99%

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Deep Einstein@Home All-sky Search for Continuous Gravitational Waves in LIGO O3 Public Data

Steltner

Papa

Eggenstein

et al. 2023

ApJ

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We present the results of an all-sky search for continuous gravitational waves in the public LIGO O3 data. The search covers signal frequencies 20.0 Hz ≤ f ≤ 800.0 Hz and a spin-down range down to −2.6 × 10−9 Hz s−1, motivated by detectability studies on synthetic populations of Galactic neutron stars. This search is the most sensitive all-sky search to date in this frequency/spin-down region. The initial search was performed using the first half of the public LIGO O3 data (O3a), utilizing graphical processing units provided in equal parts by the volunteers of the Einstein@Home computing project and by the ATLAS cluster. After a hierarchical follow-up in seven stages, 12 candidates remain. Six are discarded at the eighth stage, by using the remaining O3 LIGO data (O3b). The surviving six can be ascribed to continuous-wave fake signals present in the LIGO data for validation purposes. We recover these fake signals with very high accuracy with our last stage search, which coherently combines all O3 data. Based on our results, we set upper limits on the gravitational-wave amplitude h 0 and translate these into upper limits on the neutron star ellipticity and on the r-mode amplitude. The most stringent upper limits are at 203 Hz, with h 0 = 8.1 × 10−26 at the 90% confidence level. Our results exclude isolated neutron stars rotating faster than 5 ms with ellipticities greater than 5 × 10 − 8 d 100 pc within a distance d from Earth and r-mode amplitudes α ≥ 10 − 5 d 100 pc for neutron stars spinning faster than 150 Hz.

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Section:  -mentioning

confidence: 99%

“…´--, carried out on the distributed computing volunteer project Einstein@Home and the ATLAS supercomputer at the Max Planck Institute (MPI) for Gravitational Physics in Hannover. The frequency-spin-down range is based on the predictions of Pagliaro et al (2023), according to which more than 95% of the potentially detectable sources lie in this range.…”

mentioning

confidence: 99%

Deep Einstein@Home All-sky Search for Continuous Gravitational Waves in LIGO O3 Public Data

Steltner

Papa

Eggenstein

et al. 2023

ApJ

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“…With the model for the spin and magnetic field evolution of neutron stars described above, we now consider the effect of such a model on several neutron star properties and observables through a series of simulations. For each of our simulations, we draw the initial spin-period P 0 and initial magnetic field B p,0 from astrophysically motivated distributions p (Igoshev et al 2022;Pagliaro et al 2023)…”

Section: Simulationmentioning

confidence: 99%

Confronting the Neutron Star Population with Inverse Cascades

Sarin

Brandenburg

Haskell

2023

ApJL

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The origin and evolution of magnetic fields of neutron stars from birth have long been a source of debate. Here, motivated by recent simulations of the Hall cascade with magnetic helicity, we invoke a model where the large-scale magnetic field of neutron stars grows as a product of small-scale turbulence through an inverse cascade. We apply this model to a simulated population of neutron stars at birth and show how this model can account for the evolution of such objects across the P P ̇ diagram, explaining both pulsar and magnetar observations. Under the assumption that small-scale turbulence is responsible for large-scale magnetic fields, we place a lower limit on the spherical harmonic degree of the energy-carrying magnetic eddies of ≈40. Our results favor the presence of a highly resistive pasta layer at the base of the neutron star crust. We further discuss the implications of this paradigm on direct observables, such as the nominal age and braking index of pulsars.

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Continuous gravitational waves from Galactic neutron stars: demography, detectability and prospects

Cited by 2 publications

References 109 publications

Deep Einstein@Home All-sky Search for Continuous Gravitational Waves in LIGO O3 Public Data

Deep Einstein@Home All-sky Search for Continuous Gravitational Waves in LIGO O3 Public Data

Confronting the Neutron Star Population with Inverse Cascades

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