{
  "abstract": "The waveform is obtained from one balance of energy and radiation on Helmholtz orbits of the retarded mass kernel, with a spherical-Bessel flux. That balance follows from the Dirac--Maxwell equation with a modified vertex, the single $U(1)$ coupling being replaced by the eight operators of the source interaction. After contact that balance is the energy loss of one packet: a bounded well for a black-hole remnant and the Coulomb ladder of one star for a neutron-star remnant. Ringdown starts from the spherical projection of that end state, which contains its spin. The comparisons use model waveforms at the published parameters. For GW250114, at the Coulomb-radius contact and after a shift of $-16\\,\\mathrm{ms}$, the noise-weighted norm ratio against the NRSur7dq4 median in $100$--$200\\,\\mathrm{Hz}$ stays between $1.36$ and $1.94$ across the published distance interval. Stopping at $2.4$ times that radius lowers the ratio to $1.11$, which the same interval moves from $0.94$ to $1.35$. With contact placed on the published merger time and with no time shift, that ratio is $3.32$ at the Coulomb radius and $2.30$ at $2.4$ times that radius. At the larger radius, the unretarded limit of this balance, with unit spherical-Bessel weights, reaches contact at $94\\,\\mathrm{Hz}$, and in $20$--$100\\,\\mathrm{Hz}$ the norm ratio to the Helmholtz balance is $1.12$ after a shift of $+27\\,\\mathrm{ms}$. For GW170817, $|h_{+}|$ near $100\\,\\mathrm{Hz}$ is $8.0\\times10^{-23}$, and the mismatch against the $2.5$PN inspiral is a difference in phasing.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2609.40168",
  "author_total": 1,
  "authors": [
    {
      "name": "Hong-Bo Jin"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/1t6dy9bpp4asj.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2609.40168",
  "fulltext_url": null,
  "id": "1t6dy9bpp4asj",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2609.40168",
  "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",
      "astro-ph.HE"
    ],
    [
      "openalex",
      "3103|Pulsars and Gravitational Waves Research"
    ]
  ],
  "openalex": "W7215045800",
  "pdf_url": "https://arxiv.org/pdf/2609.40168",
  "pmcid": null,
  "pmid": null,
  "published": "2026-09-30",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/1t6dy9bpp4asj.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:25:49Z",
      "native_id": "2609.40168",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2609.40168"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    }
  ],
  "title": "A new method for inspiral-to-ringdown waveforms of compact binaries: Helmholtz orbits and spherical-Bessel flux",
  "title_text": "A new method for inspiral-to-ringdown waveforms of compact binaries: Helmholtz orbits and spherical-Bessel flux",
  "type": "preprint",
  "updated_at": "2026-10-30T12:25:49Z",
  "url": "https://research.draconitic.com/paper/1t6dy9bpp4asj",
  "venue": "arXiv",
  "versions": []
}