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  New searches for continuous gravitational waves from seven fast pulsars

Ashok, A., Beheshtipour, B., Papa, M. A., Freire, P. C. C., Steltner, B., Machenschalk, B., et al. (in preparation). New searches for continuous gravitational waves from seven fast pulsars.

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2107.09727.pdf (Preprint), 3MB
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 Creators:
Ashok, Anjana1, Author              
Beheshtipour, Banafsheh1, Author              
Papa, Maria Alessandra2, Author              
Freire , Paulo C. C., Author
Steltner, Benjamin1, Author              
Machenschalk, Bernd1, Author              
Behnke, Oliver3, Author              
Allen, Bruce3, Author              
Prix, Reinhard1, Author              
Affiliations:
1Searching for Continuous Gravitational Waves, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2630691              
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              
3Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
 Abstract: We conduct searches for continuous gravitational waves from seven pulsars, that have not been targeted in continuous wave searches of Advanced LIGO data before. We target emission at exactly twice the rotation frequency of the pulsars and in a small band around such frequency. The former search assumes that the gravitational wave quadrupole is changing phase-locked with the rotation of the pulsar. The search over a range of frequencies allows for differential rotation between the component emitting the radio signal and the component emitting the gravitational waves, for example the crust or magnetosphere versus the core. Timing solutions derived from the Arecibo 327-MHz Drift-Scan Pulsar Survey (AO327) observations are used. No evidence of a signal is found and upper limits are set on the gravitational wave amplitude. For one of the pulsars we probe gravitational wave intrinsic amplitudes just a factor of 3.8 higher than the spin-down limit, assuming a canonical moment of inertia of $10^{38}$ kg m$^2$. Our tightest ellipticity is $1.7 \times 10^{-8}$, which is a value well within the range of what a neutron star crust could support.

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 Dates: 2021-07-202021-07-28
 Publication Status: Not specified
 Pages: Submitted to The Astrophysical Journal
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 Table of Contents: -
 Rev. Type: -
 Identifiers: arXiv: 2107.09727
 Degree: -

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