Impact of high-order tidal terms on binary neutron-star waveforms

Forteza, Xisco Jiménez; Abdelsalhin, Tiziano; Pani, Paolo; Gualtieri, Leonardo

doi:10.1103/physrevd.98.124014

Cited by 43 publications

(46 citation statements)

References 108 publications

(218 reference statements)

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“…We note that there are higher-order spin-tidal coupling effects that have recently been computed [21,22]. However, as outlined in [23], these terms will be unmeasurable in the advanced GW detector era. Therefore, we do not include them in the current description to avoid unnecessary computational costs.…”

Section: A the Basic Idea Of Nrtidalmentioning

confidence: 82%

“…Over the last years, there has been significant progress modeling the GW signal associated with the BNS coalescence, including the computation of higher-order tidal corrections or spin-tidal coupling, e.g., Refs. [18][19][20][21][22][23], and improved accuracy of BNS numerical relativity (NR) simulations [24][25][26][27][28][29]. However, although the analytical progress has improved the performance of post-Newtonian (PN) waveform approximants, PN models still become increasingly inaccurate towards the merger, e.g.…”

Section: Introductionmentioning

confidence: 99%

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Improving the NRTidal model for binary neutron star systems

Dietrich¹,

Samajdar²,

et al. 2019

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Accurate and fast gravitational waveform (GW) models are essential to extract information about the properties of compact binary systems that generate GWs. Building on previous work, we present an extension of the NRTidal model for binary neutron star (BNS) waveforms. The upgrades are: (i) a new closed-form expression for the tidal contribution to the GW phase which includes further analytical knowledge and is calibrated to more accurate numerical relativity data than previously available; (ii) a tidal correction to the GW amplitude; (iii) an extension of the spinsector incorporating equation-of-state-dependent finite size effects at quadrupolar and octupolar order; these appear in the spin-spin tail terms and cubic-in-spin terms, both at 3.5PN. We add the new description to the precessing binary black hole waveform model IMRPhenomPv2 to obtain a frequency-domain precessing binary neutron star model. In addition, we extend the SEOBNRv4_ROM and IMRPhenomD aligned-spin binary black hole waveform models with the improved tidal phase corrections. Focusing on the new IMRPhenomPv2_NRTidalv2 approximant, we test the model by comparing with numerical relativity waveforms as well as hybrid waveforms combining tidal effective-one-body and numerical relativity data. We also check consistency against a tidal effective-one-body model across large regions of the BNS parameter space.

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Section: A the Basic Idea Of Nrtidalmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 99%

Improving the NRTidal model for binary neutron star systems

Dietrich¹,

Samajdar²,

et al. 2019

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“…We compare the 90% credible interval presented in Fig. 5 of [17] for GW150914 signal to the Fisher matrix calculations using the approximate relation ∆ 90% ≈ 1.64 × σ Fisher 10 [35][36][37]. We see that the Fisher matrix underestimates the errors considerably 11 .…”

Section: A On the Statistical Errormentioning

confidence: 88%

Ringdown overtones, black hole spectroscopy, and no-hair theorem tests

et al. 2020

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Validating the black-hole no-hair theorem with gravitational-wave observations of compact binary coalescences provides a compelling argument that the remnant object is indeed a black hole as described by the general theory of relativity. This requires performing a spectroscopic analysis of the post-merger signal and resolving the frequencies of either different angular modes or overtones (of the same angular mode). For a nearly-equal mass binary black-hole system, only the dominant angular mode (l = m = 2) is sufficiently excited and the overtones are instrumental to perform this test. Here we investigate the robustness of modelling the post-merger signal of a binary black hole coalescence as a superposition of overtones. Further, we study the bias expected in the recovered frequencies as a function of the start time of a spectroscopic analysis and provide a computationally cheap procedure to choose it based on the interplay between the expected statistical error due to the detector noise and the systematic errors due to waveform modelling. Moreover, since the overtone frequencies are closely spaced, we find that resolving the overtones is particularly challenging and requires a loud ringdown signal. Rayleigh's resolvability criterion suggests that -in an optimistic scenario -a ringdown signal-to-noise ratio larger than ∼ 30 (achievable possibly with LIGO at design sensitivity and routinely with future interferometers such as Einstein Telescope, Cosmic Explorer, and LISA) is necessary to resolve the overtone frequencies. We then conclude by discussing some conceptual issues associated with black-hole spectroscopy with overtones.

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“…The fmtidal model derived in this paper can be directly included in any frequency domain point-particle baseline model for a binary inspiral. Other matter effects such as spin-induced multipoles, gravitomagnetic tides, spin-tidal interactions, and tidal heating are already known and enter separately into these models [47][48][49][50][51][52][53]. The fmtidal model can easily be improved with inputs from NR for the behavior at higher frequencies, where other physics may become important.…”

Section: Introductionmentioning

confidence: 99%

Frequency domain model of f -mode dynamic tides in gravitational waveforms from compact binary inspirals

Schmidt

Hinderer

2019

Phys. Rev. D

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The recent detection of gravitational waves (GWs) from the neutron star binary inspiral GW170817 has opened a unique avenue to probe matter and fundamental interactions in previously unexplored regimes. Extracting information on neutron star matter from the observed GWs requires robust and computationally efficient theoretical waveform models. We develop an approximate frequency-domain GW phase model of a main GW signature of matter: dynamic tides associated with the neutron stars' fundamental oscillation modes (f -modes). We focus on nonspinning objects on circular orbits and demonstrate that, despite its mathematical simplicity, the new "f -mode tidal" (fmtidal) model is in good agreement with the effective-one-body dynamical tides model up to GW frequencies of 1 kHz and gives physical meaning to part of the phenomenology captured in tidal models tuned to numerical-relativity. The advantages of the fmtidal model are that it makes explicit the dependence of the GW phasing on the characteristic equation-of-state parameters, i.e., tidal deformabilities and f -mode frequencies, is computationally efficient, and can readily be added to any frequency-domain baseline waveform. The fmtidal model is easily amenable to future improvements and provides the means for a first step towards independently measuring additional fundamental properties of neutron star matter beyond the tidal deformability as well as performing novel tests of General Relativity from GW observations. PACS numbers: 04.80.Nn, 95.85.Sz, 04.30.Tv, 97.60.Jd, 26.60.Kp * pschmidt@star.sr.bham.ac.uk † t.hinderer@uva.nl 1 Oscillation modes are characterized by three integers (n, , m),where n denotes the number of radial nodes in the mode function and m is the azimuthal integer. In the nonspinning case, the mode frequency is independent of m, and for the f -modes n = 0, hence our notation ω n m | f −mode = ω . arXiv:1905.00818v1 [gr-qc]

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Impact of high-order tidal terms on binary neutron-star waveforms

Cited by 43 publications

References 108 publications

Improving the NRTidal model for binary neutron star systems

Improving the NRTidal model for binary neutron star systems

Ringdown overtones, black hole spectroscopy, and no-hair theorem tests

Frequency domain model of f -mode dynamic tides in gravitational waveforms from compact binary inspirals

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