Tidal effects in the gravitational-wave phase evolution of compact binary systems to next-to-next-to-leading post-Newtonian order

Henry, Quentin; Faye, Guillaume; Blanchet, Luc

doi:10.1103/physrevd.102.044033

Cited by 55 publications

(36 citation statements)

References 70 publications

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“…The remaining O(v 14 ) terms have been obtained from a small-velocity expansion of our 2PM result, and in order to get a complete result at that PN order one would need to include also the 3PM corrections to the potential generated by cubic and tidal interactions 6 . We have also compared the contribution to the energy from the η 1,2 corrections to [71], finding agreement (after mapping their coefficients µ (2) A to ours) 7 . Next, we compute the leading-order gravitational-wave flux using the quadrupole formula…”

Section: Power Radiated By the Gravitational Wavessupporting

confidence: 57%

“…We also explain this result by constructing an explicit field redefinition relating the two couplings. For the PN-expanded result of the tidal corrections to the mass quadrupole we find agreement with [69][70][71]. The remaining tasks consist in using the corrected quadrupole moment to compute the modifications compared to EH gravity to the power emitted by the radiated gravitational waves, and the corresponding corrections to the waveforms in the Stationary Phase Approximation (SPA) 3 .…”

Section: Introductionmentioning

confidence: 55%

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From amplitudes to gravitational radiation with cubic interactions and tidal effects

Huber,

Brandhuber,

De Angelis

et al. 2020

Preprint

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We study the effect of cubic and tidal interactions on the spectrum of gravitational waves emitted in the inspiral phase of the merger of two non-spinning objects. There are two independent parity-even cubic interaction terms, which we take to beβ . The latter has vanishing pure graviton amplitudes but modifies mixed scalar/graviton amplitudes which are crucial for our study. Working in an effective field theory set-up, we compute the modifications to the quadrupole moment due to I 1 , G 3 and tidal interactions, from which we obtain the power of gravitational waves radiated in the process to first order in the perturbations and leading order in the post-Minkowskian expansion. The I 1 predictions are novel, and we find that our results for G 3 are related to the known quadrupole corrections arising from tidal perturbations, although the physical origin of the G 3 coupling is unrelated to the finite-size effects underlying tidal interactions. We show this by recomputing such tidal corrections and by presenting an explicit field redefinition. In the post-Newtonian expansion our results are complete at leading order, which for the gravitational-wave flux is 5PN for G 3 and tidal interactions, and 6PN for I 1 . Finally, we compute the corresponding modifications to the waveforms.

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Section: Power Radiated By the Gravitational Wavessupporting

confidence: 57%

Section: Introductionmentioning

confidence: 55%

From amplitudes to gravitational radiation with cubic interactions and tidal effects

Huber,

Brandhuber,

De Angelis

et al. 2020

Preprint

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“…From Refs. [99][100][101][102][103][104][105][106], we obtain the frequency-domain gravitational-wave phasing, up to 3.5PN order for pointparticle contributions, up to 3PN for spin terms, and up to 2.5PN for an adiabatic, f-mode tide. Here are the terms in addition to the leading Newtonian phasing Ψ N :…”

Section: Appendix A: Justification For Ignoring the Pp Precessionmentioning

confidence: 86%

“…5PN6 [99], Ψ SO is the spin-orbit coupling term[100][101][102][103], and Ψ¯λð1Þ f and Ψ¯λð2Þ f are f-mode tidal effects from m 1 and m 2 , respectively[104][105][106]. We have ignored the spin-spin coupling and the spin precession because their effects are negligible (see Appendix A).…”

mentioning

confidence: 99%

Detecting resonant tidal excitations of Rossby modes in coalescing neutron-star binaries with third-generation gravitational-wave detectors

Chen

2021

Phys. Rev. D

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Rossby modes (r-modes) of rotating neutron stars can be excited by the gravitomagnetic forces in coalescing binary systems. A previous study by Flanagan and Racine [Phys. Rev. D 75, 044001 (2007)] showed that this kind of dynamical tide (DT) can induce phase shifts of ∼0.1 rad on gravitational waveforms, which is detectable by third-generation (3G) detectors. We study the impact of this DT on measuring neutron-star parameters in the era of 3G detectors. We incorporate two universal relations among neutron-star properties predicted by different equations of state: (i) the well-known I-Love relation between momentum of inertia and (f-mode) tidal Love number, and (ii) a relation between the r-mode overlap and tidal Love number, which we newly explore. We find that r-mode DT will provide rich information about slowly rotating neutron stars with frequency 10-100 Hz and spin inclination angle 18°-110°. For a binary neutron-star system (with a signal-to-noise ratio ∼1500 in the Cosmic Explorer), the spin frequency of each individual neutron star can be constrained to 6% (fractional error) in the best-case scenario. The degeneracy between the Love numbers of individual neutron stars is dramatically reduced: each individual Love number can be constrained to around 20% in the best case, while the fractional error for both symmetric and antisymmetric Love numbers are reduced by factors of around 300. Furthermore, DT also allows us to measure the spin inclination angles of the neutron stars, to 0.09 rad in the best case, and thus place constraints on neutron-star natal kicks and supernova explosion models. In addition to parameter estimation, we also develop a semianalytic method that accurately describes detailed features of the binary evolution that arise due to the DT.

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“…In this paper we investigate the effects of tidal deformations [93][94][95] on the conservative two-body Hamiltonian during the inspiral phase, focusing on their structure in the post-Minkowskian expansion. The tidal deformations offer a window into the equation of state of neutrons stars [96][97][98][99] and test our understanding of black holes [83,[100][101][102][103][104][105][106][107] and of possible exotic physics [108][109][110][111][112][113][114]. While tidal effects are expected to vanish for black holes in general relativity [97,[115][116][117][118], they are of crucial importance for understanding the equation of state of neutron stars.…”

Section: Introductionmentioning

confidence: 99%

Leading nonlinear tidal effects and scattering amplitudes

Bern¹,

Parra-Martinez

Roiban

et al. 2021

J. High Energ. Phys.

100

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We present the two-body Hamiltonian and associated eikonal phase, to leading post-Minkowskian order, for infinitely many tidal deformations described by operators with arbitrary powers of the curvature tensor. Scattering amplitudes in momentum and position space provide systematic complementary approaches. For the tidal operators quadratic in curvature, which describe the linear response to an external gravitational field, we work out the leading post-Minkowskian contributions using a basis of operators with arbitrary numbers of derivatives which are in one-to-one correspondence with the worldline multipole operators. Explicit examples are used to show that the same techniques apply to both bodies interacting tidally with a spinning particle, for which we find the leading contributions from quadratic in curvature tidal operators with an arbitrary number of derivatives, and to effective field theory extensions of general relativity. We also note that the leading post-Minkowskian order contributions from higher-dimension operators manifest double-copy relations. Finally, we comment on the structure of higher-order corrections.

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Tidal effects in the gravitational-wave phase evolution of compact binary systems to next-to-next-to-leading post-Newtonian order

Cited by 55 publications

References 70 publications

From amplitudes to gravitational radiation with cubic interactions and tidal effects

From amplitudes to gravitational radiation with cubic interactions and tidal effects

Detecting resonant tidal excitations of Rossby modes in coalescing neutron-star binaries with third-generation gravitational-wave detectors

Leading nonlinear tidal effects and scattering amplitudes

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