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Journal Article

New and robust gravitational-waveform model for high-mass-ratio binary neutron star systems with dynamical tidal effects

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

/persons/resource/persons192099

Dietrich,  Tim
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Multi-messenger Astrophysics of Compact Binaries, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons127862

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

/persons/resource/persons144501

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

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2311.07456.pdf
(Preprint), 10MB

PhysRevD.109.024062.pdf
(Publisher version), 17MB

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Citation

Abac, A., Dietrich, T., Buonanno, A., Steinhoff, J., & Ujevic, M. (2024). New and robust gravitational-waveform model for high-mass-ratio binary neutron star systems with dynamical tidal effects. Physical Review D, 109(2): 024062. doi:10.1103/PhysRevD.109.024062.


Cite as: https://hdl.handle.net/21.11116/0000-000E-02A6-4
Abstract
For the analysis of gravitational-wave signals, fast and accurate
gravitational-waveform models are required. These enable us to obtain
information on the system properties from compact binary mergers. In this
article, we introduce the NRTidalv3 model, which contains a closed-form
expression that describes tidal effects, focusing on the description of binary
neutron star systems. The model improves upon previous versions by employing a
larger set of numerical-relativity data for its calibration, by including
high-mass ratio systems covering also a wider range of equations of state. It
also takes into account dynamical tidal effects and the known post-Newtonian
mass-ratio dependence of individual calibration parameters. We implemented the
model in the publicly available LALSuite software library by augmenting
different binary black hole waveform models (IMRPhenomD, IMRPhenomX, and
SEOBNRv5_ROM). We test the validity of NRTidalv3 by comparing it with
numerical-relativity waveforms, as well as other tidal models. Finally, we
perform parameter estimation for GW170817 and GW190425 with the new tidal
approximant and find overall consistent results with respect to previous
studies.