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Constraining the p-mode--g-mode tidal instability with GW170817

The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., et al. (2019). Constraining the p-mode--g-mode tidal instability with GW170817. Physical Review Letters, 122: 061104. doi:10.1103/PhysRevLett.122.061104.

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### Creators

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Creators:
The LIGO Scientific Collaboration, Author
The Virgo Collaboration, Author
Abbott, B. P., Author
Abbott, R., Author
Abbott, T. D., Author
Acernese, F., Author
Ackley, K., Author
Affeldt, C.1, Author
Agarwal, B., Author
Agathos, M., Author
Agatsuma, K., Author
Aggarwal, N., Author
Aguiar, O. D., Author
Aiello, L., Author
Ain, A., Author
Affiliations:
1Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24010
2Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011
3Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290
4Searching for Continuous Gravitational Waves, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2630691
5Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2461691
6Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
Abstract: We analyze the impact of a proposed tidal instability coupling $p$-modes and $g$-modes within neutron stars on GW170817. This non-resonant instability transfers energy from the orbit of the binary to internal modes of the stars, accelerating the gravitational-wave driven inspiral. We model the impact of this instability on the phasing of the gravitational wave signal using three parameters per star: an overall amplitude, a saturation frequency, and a spectral index. Incorporating these additional parameters, we compute the Bayes Factor ($\ln B^{pg}_{!pg}$) comparing our $p$-$g$ model to a standard one. We find that the observed signal is consistent with waveform models that neglect $p$-$g$ effects, with $\ln B^{pg}_{!pg} = 0.03^{+0.70}_{-0.58}$ (maximum a posteriori and 90% credible region). By injecting simulated signals that do not include $p$-$g$ effects and recovering them with the $p$-$g$ model, we show that there is a $\simeq 50\%$ probability of obtaining similar $\ln B^{pg}_{!pg}$ even when $p$-$g$ effects are absent. We find that the $p$-$g$ amplitude for 1.4 $M_\odot$ neutron stars is constrained to $\lesssim \text{few}\times10^{-7}$, with maxima a posteriori near $\sim 10^{-7}$ and $p$-$g$ saturation frequency $\sim 70\, \mathrm{Hz}$. This suggests that there are less than a few hundred excited modes, assuming they all saturate by wave breaking. For comparison, theoretical upper bounds suggest a $p$-$g$ amplitude $\lesssim 10^{-6}$ and $\lesssim 10^{3}$ modes saturating by wave breaking. Thus, the measured constraints only rule out extreme values of the $p$-$g$ parameters. They also imply that the instability dissipates $\lesssim 10^{51}\, \mathrm{ergs}$ over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves.

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Dates: 2018-08-262018-09-192019
Publication Status: Published in print
Pages: 7 pages, 2 figures
Publishing info: -
Rev. Type: -
Identifiers: arXiv: 1808.08676
DOI: 10.1103/PhysRevLett.122.061104
URI: http://arxiv.org/abs/1808.08676
Degree: -

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### Source 1

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Title: Physical Review Letters
Abbreviation : Phys. Rev. Lett.
Source Genre: Journal
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Publ. Info: Woodbury, N.Y. : American Physical Society
Pages: - Volume / Issue: 122 Sequence Number: 061104 Start / End Page: - Identifier: ISSN: 0031-9007
CoNE: https://pure.mpg.de/cone/journals/resource/954925433406_1