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1811086379775426560
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Massachusetts Institute of Technology. Department of Physics
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Massachusetts Institute of Technology. Department of Physics
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MIT
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We analyze the impact of a proposed tidal instability coupling p modes and g modes within neutron stars on GW170817. This nonresonant 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[subscript !pg][superscript 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[subscript !pg][superscript pg]=0.03[subscript -0.58][superscript +0.70] (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 ≃50% probability of obtaining similar ln B[subscript !pg][superscript pg] even when p-g effects are absent. We find that the p-g amplitude for 1.4 M[⊙] stars is constrained to less than a few tenths of the theoretical maximum, with maxima a posteriori near one-Tenth this maximum and p-g saturation frequency ∼70 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 10[superscript 3] modes saturate by wave breaking. Thus, the measured constraints only rule out extreme values of the p-g parameters. They also imply that the instability dissipates ≲ 10[superscript 51] erg over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves.
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2024-09-23T13:25:04Z
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Article
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mit-1721.1/124453
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Massachusetts Institute of Technology
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2024-09-23T13:25:04Z
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2020
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American Physical Society
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dspace
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mit-1721.1/1244532022-10-01T15:08:19Z Constraining the p-Mode–g-Mode Tidal Instability with GW170817 Massachusetts Institute of Technology. Department of Physics LIGO (Observatory : Massachusetts Institute of Technology) MIT Kavli Institute for Astrophysics and Space Research We analyze the impact of a proposed tidal instability coupling p modes and g modes within neutron stars on GW170817. This nonresonant 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[subscript !pg][superscript 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[subscript !pg][superscript pg]=0.03[subscript -0.58][superscript +0.70] (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 ≃50% probability of obtaining similar ln B[subscript !pg][superscript pg] even when p-g effects are absent. We find that the p-g amplitude for 1.4 M[⊙] stars is constrained to less than a few tenths of the theoretical maximum, with maxima a posteriori near one-Tenth this maximum and p-g saturation frequency ∼70 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 10[superscript 3] modes saturate by wave breaking. Thus, the measured constraints only rule out extreme values of the p-g parameters. They also imply that the instability dissipates ≲ 10[superscript 51] erg over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves. National Science Foundation (U.S.) 2020-03-31T18:01:19Z 2020-03-31T18:01:19Z 2019-02 2018-10 2019-03-20T18:27:24Z Article http://purl.org/eprint/type/JournalArticle 0031-9007 1079-7114 https://hdl.handle.net/1721.1/124453 Abbott, B. P. et al. “Constraining the p-Mode–g-Mode Tidal Instability with GW170817.” Physical Review Letters 122, 6 (February 2019): 061104. © 2019 American Physical Society. http://dx.doi.org/10.1103/PhysRevLett.122.061104 Physical Review Letters Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf American Physical Society APS
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| spellingShingle |
Constraining the p-Mode–g-Mode Tidal Instability with GW170817
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| title |
Constraining the p-Mode–g-Mode Tidal Instability with GW170817
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| title_full |
Constraining the p-Mode–g-Mode Tidal Instability with GW170817
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| title_fullStr |
Constraining the p-Mode–g-Mode Tidal Instability with GW170817
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| title_full_unstemmed |
Constraining the p-Mode–g-Mode Tidal Instability with GW170817
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| title_short |
Constraining the p-Mode–g-Mode Tidal Instability with GW170817
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| title_sort |
constraining the p mode g mode tidal instability with gw170817
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| url |
https://hdl.handle.net/1721.1/124453
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