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Leveraging NRTidalv3 to develop gravitational waveform models with higher-order modes for binary neutron star systems

Adrian Abac1,2,*, Felip A. Ramis Vidal3, Marta Colleoni3, Anna Puecher2, Alejandra Gonzalez3, and Tim Dietrich2,1

  • *Contact author: adrian.abac@aei.mpg.de
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Phys. Rev. D 112, 104026 – Published 12 November, 2025

DOI: https://doi.org/10.1103/hzn7-39js

Abstract

Accurate and reliable gravitational waveform models are crucial in determining the properties of compact binary mergers. In particular, next-generation gravitational-wave detectors will require more accurate waveforms to avoid biases in the analysis. In this work, we extend the recent NRTidalv3 model to account for higher-mode corrections in the tidal phase contributions for binary neutron star systems. The higher-mode, multipolar NRTidalv3 model is then attached to several binary-black-hole baselines, such as the phenomenological IMRPhenomXHM and IMRPhenomXPHM models, and the effective-one-body-based model SEOBNRv5HM_ROM. We test the performance and validity of the newly developed models by comparing them with numerical-relativity simulations and other tidal models. Finally, we employ them in parameter estimation analyses on simulated signals from both comparable-mass and high-mass-ratio systems, as well as on the gravitational-wave event GW170817, for which we find consistent results with respect to previous analyses.

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Corrections

17 December, 2025

Correction: Missing support statements have been added to the Acknowledgments.

Article Text

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Phys. Rev. D 112, 104026– Published 12 November, 2025
  • Received 30 July 2025
  • Revised 2 October 2025
  • Accepted 17 October 2025
  • Corrected 17 December 2025
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