New dynamical tide constraints from current and future gravitational wave detections of inspiralling neutron stars
New dynamical tide constraints from current and future gravitational wave detections of inspiralling neutron stars
Previous theoretical works using the premerger orbital evolution of coalescing neutron stars to constrain properties of dense nuclear matter assume a gravitational wave phase uncertainty of a few radians, or about a half cycle. However, recent studies of the signal from GW170817 and next-generation detector sensitivities indicate actual phase uncertainties at least twenty times better. Using these refined estimates, we show that future observations of nearby sources like GW170817 may be able to reveal neutron star properties beyond just radius and tidal deformability, such as the matter composition and/or presence of a superfluid inside neutron stars, via tidal excitation of g-mode oscillations. Data from GW170817 already limits the amount of orbital energy that is transferred to the neutron star to <2×1047 erg and the g-mode tidal coupling to Qα<10-3 at 50 Hz (5×1048 erg and 4×10-3 at 200 Hz), and future observations and detectors will greatly improve upon these constraints. In addition, analysis using general parametrization models that have been applied to the so-called p-g instability show that the instability already appears to be restricted to regimes where the mechanism is likely to be inconsequential; in particular, we show that the number of unstable modes is 100 at 100 Hz, and next generation detectors will essentially rule out this mechanism (assuming that the instability remains undetected). Finally, we illustrate that measurements of tidal excitation of r-mode oscillations in nearby rapidly rotating neutron stars are within reach of current detectors and note that even nondetections will limit the inferred inspiralling neutron star spin rate to <20 Hz, which will be useful when determining other parameters such as neutron star mass and tidal deformability.
Ho, Wynn C.G.
048456cd-c2f9-4c47-96e7-a415b04715dc
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
3 August 2023
Ho, Wynn C.G.
048456cd-c2f9-4c47-96e7-a415b04715dc
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Ho, Wynn C.G. and Andersson, Nils
(2023)
New dynamical tide constraints from current and future gravitational wave detections of inspiralling neutron stars.
Physical Review D, 108 (4), [043003].
(doi:10.1103/PhysRevD.108.043003).
Abstract
Previous theoretical works using the premerger orbital evolution of coalescing neutron stars to constrain properties of dense nuclear matter assume a gravitational wave phase uncertainty of a few radians, or about a half cycle. However, recent studies of the signal from GW170817 and next-generation detector sensitivities indicate actual phase uncertainties at least twenty times better. Using these refined estimates, we show that future observations of nearby sources like GW170817 may be able to reveal neutron star properties beyond just radius and tidal deformability, such as the matter composition and/or presence of a superfluid inside neutron stars, via tidal excitation of g-mode oscillations. Data from GW170817 already limits the amount of orbital energy that is transferred to the neutron star to <2×1047 erg and the g-mode tidal coupling to Qα<10-3 at 50 Hz (5×1048 erg and 4×10-3 at 200 Hz), and future observations and detectors will greatly improve upon these constraints. In addition, analysis using general parametrization models that have been applied to the so-called p-g instability show that the instability already appears to be restricted to regimes where the mechanism is likely to be inconsequential; in particular, we show that the number of unstable modes is 100 at 100 Hz, and next generation detectors will essentially rule out this mechanism (assuming that the instability remains undetected). Finally, we illustrate that measurements of tidal excitation of r-mode oscillations in nearby rapidly rotating neutron stars are within reach of current detectors and note that even nondetections will limit the inferred inspiralling neutron star spin rate to <20 Hz, which will be useful when determining other parameters such as neutron star mass and tidal deformability.
Text
2307.10721
- Accepted Manuscript
Available under License Other.
Text
PhysRevD.108.043003
- Version of Record
Available under License Other.
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Accepted/In Press date: 17 July 2023
Published date: 3 August 2023
Additional Information:
Funding Information:
The authors are grateful to Bruce Edelman, Ben Farr, and Jocelyn Read for providing the phase uncertainties from their works (and shown in Fig. ) and to Jocelyn Read for her work and discussions. The authors thank Andrew Counsell for sharing his numerical g-mode results with us. N. A. gratefully acknowledges support from Science and Technology Facility Council (STFC) via Grant No. ST/V000551/1.
Identifiers
Local EPrints ID: 482017
URI: http://eprints.soton.ac.uk/id/eprint/482017
ISSN: 2470-0010
PURE UUID: e920c70f-9e24-4f32-9f27-ed6cabf43421
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Date deposited: 15 Sep 2023 16:33
Last modified: 18 Mar 2024 02:49
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Author:
Wynn C.G. Ho
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