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Using gravitational-wave data to constrain dynamical tides in neutron star binaries

Using gravitational-wave data to constrain dynamical tides in neutron star binaries
Using gravitational-wave data to constrain dynamical tides in neutron star binaries
We discuss the role of dynamical tidal effects for inspiralling neutron star binaries, focussing on features that may be considered "unmodelled" in gravitational-wave searches. In order to cover the range of possibilities, we consider i) individual oscillation modes becoming resonant with the tide, ii) the elliptical instability, where a pair of inertial modes exhibit a nonlinear resonance with the tide, and iii) the non-resonant p-g instability which may arise as high order p- and g-modes in the star couple nonlinearly to the tide. In each case, we estimate the amount of additional energy loss that needs to be associated with the dynamical tide in order for the effect to impact on an observed gravitational-wave signal. We explore to what extent the involved neutron star physics may be considered known and how one may be able to use observational data to constrain theory.
2470-0029
023016-[14pp]
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45

Andersson, Nils and Ho, Wynn C.G. (2018) Using gravitational-wave data to constrain dynamical tides in neutron star binaries. Physical Review D, 97 (2), 023016-[14pp]. (doi:10.1103/PhysRevD.97.023016).

Record type: Article

Abstract

We discuss the role of dynamical tidal effects for inspiralling neutron star binaries, focussing on features that may be considered "unmodelled" in gravitational-wave searches. In order to cover the range of possibilities, we consider i) individual oscillation modes becoming resonant with the tide, ii) the elliptical instability, where a pair of inertial modes exhibit a nonlinear resonance with the tide, and iii) the non-resonant p-g instability which may arise as high order p- and g-modes in the star couple nonlinearly to the tide. In each case, we estimate the amount of additional energy loss that needs to be associated with the dynamical tide in order for the effect to impact on an observed gravitational-wave signal. We explore to what extent the involved neutron star physics may be considered known and how one may be able to use observational data to constrain theory.

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More information

Accepted/In Press date: 20 December 2017
e-pub ahead of print date: 24 January 2018
Published date: January 2018

Identifiers

Local EPrints ID: 416268
URI: https://eprints.soton.ac.uk/id/eprint/416268
ISSN: 2470-0029
PURE UUID: 928d2cb5-207d-461f-baf2-6474e13a2ac5
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836

Catalogue record

Date deposited: 11 Dec 2017 17:30
Last modified: 06 Oct 2018 00:33

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