{
  "abstract": "Gravitational-wave observations of binary neutron star mergers probe the neutron star equation of state through finite-size effects on the waveform. These include the tidal deformation of the stars due to their respective companion, but for spinning neutron stars also include the spin-induced quadrupole moment of the stars. Typically, to avoid introducing additional equation of state dependent parameters, waveform models relate this quadrupole moment to the tidal deformability through so-called quasi-universal relations. These are derived under the slow-rotation approximation, which at larger spins, i.e., for millisecond pulsars, becomes unreliable. We attempt to extend the existing quasi-universal relations by explicitly accounting for the spin, calibrating it against numerically computed quadrupole moments across a broad set of equations of state and spins $0.15 \\leq |χ| \\leq 0.6$ with the $χ\\rightarrow 0$ limit enforced by construction. The resulting spin-extended relation reduces the median absolute percentage error relative to the slow-rotation relation by 66\\% across this range. Parameter estimation using the spin-extended relation reduces biases in recovered intrinsic parameters in some cases, though biases from mass-spin degeneracies dominate largely when a population is considered. These results provide a more accurate description of the spin-induced quadrupole moment for spinning neutron star binaries, relevant for waveform modelling with third-generation gravitational-wave detectors.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2609.19975",
  "author_total": 2,
  "authors": [
    {
      "name": "Natalie Williams"
    },
    {
      "name": "Tim Dietrich"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/en1pded0wgpzy.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2609.19975",
  "fulltext_url": null,
  "id": "en1pded0wgpzy",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2609.19975",
  "language": null,
  "licence": "CC-BY-4.0",
  "licence_label": "CC BY 4.0",
  "licence_source": "article",
  "licence_url": "http://creativecommons.org/licenses/by/4.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "gr-qc"
    ],
    [
      "openalex",
      "3103|Pulsars and Gravitational Waves Research"
    ]
  ],
  "openalex": "W7213592465",
  "pdf_url": "https://arxiv.org/pdf/2609.19975",
  "pmcid": null,
  "pmid": null,
  "published": "2026-09-17",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/en1pded0wgpzy.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:22:19Z",
      "native_id": "2609.19975",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2609.19975"
    }
  ],
  "subjects": [
    {
      "field": "physics",
      "origin": "arxiv:gr-qc",
      "subfield": "gravitation"
    }
  ],
  "title": "Extending the Love-Q Relation to Rapidly Rotating Neutron Stars for Gravitational-Waveform Modelling",
  "title_text": "Extending the Love-Q Relation to Rapidly Rotating Neutron Stars for Gravitational-Waveform Modelling",
  "type": "preprint",
  "updated_at": "2026-10-30T12:22:19Z",
  "url": "https://research.draconitic.com/paper/en1pded0wgpzy",
  "venue": "arXiv",
  "versions": []
}