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Aligned-spin neutron-star-black-hole waveform model based on the effective-one-body approach and numerical-relativity simulations

MPS-Authors
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Matas,  Andrew
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Dietrich,  Tim
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Buonanno,  Alessandra
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Hinderer,  Tanja
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Pürrer,  Michael
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Pfeiffer,  Harald
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

2004.10001.pdf
(Preprint), 4MB

PhysRevD.102.043023.pdf
(Publisher version), 4MB

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Citation

Matas, A., Dietrich, T., Buonanno, A., Hinderer, T., Pürrer, M., Foucart, F., et al. (2020). Aligned-spin neutron-star-black-hole waveform model based on the effective-one-body approach and numerical-relativity simulations. Physical Review D, 102(4): 043023. doi:10.1103/PhysRevD.102.043023.


Cite as: http://hdl.handle.net/21.11116/0000-0006-96F5-C
Abstract
After the discovery of gravitational waves from binary black holes (BBHs) and binary neutron stars (BNSs) with the LIGO and Virgo detectors, neutron-star--black-holes (NSBHs) are the natural next class of binary systems to be observed. In this work, we develop a waveform model for aligned-spin neutron-star--black-holes (NSBHs) combining a binary black-hole baseline waveform (available in the effective-one-body approach) with a phenomenological description of tidal effects (extracted from numerical-relativity simulations), and correcting the amplitude during the late inspiral, merger and ringdown to account for the NS's tidal disruption. In particular, we calibrate the amplitude corrections using NSBH waveforms obtained with the numerical-relativity spectral Einstein code (SpEC) and the SACRA code. Based on the simulations used, and on checking that sensible waveforms are produced, we recommend our model to be employed with NS's mass in the range $1-3 M_\odot$, tidal deformability $0\mbox{-}5000$, and (dimensionless) BH's spin magnitude up to $0.9$. We also validate our model against two new, highly accurate NSBH waveforms with BH's spin 0.9 and mass ratios 3 and 4, characterized by tidal disruption, produced with SpEC, and find very good agreement. Furthermore, we compute the unfaithfulness between waveforms from NSBH, BBH, and BNS systems, finding that it will be challenging for the advanced LIGO-Virgo--detector network at design sensitivity to distinguish different source classes. We perform a Bayesian parameter-estimation analysis on a synthetic numerical-relativity signal in zero noise to study parameter biases. Finally, we reanalyze GW170817, with the hypothesis that it is a NSBH. We do not find evidence to distinguish the BNS and NSBH hypotheses, however the posterior for the mass ratio is shifted to less equal masses under the NSBH hypothesis.