{
  "abstract": "Magnetic reconnection around neutron stars (NSs) forms small-scale currents while transferring energy to electron-positron pairs. These dissipating currents cover a wide range of scales, potentially leaving an imprint on time-variable X-ray bursts and pulsed radio emission. We present a reduced, planar model of internal reconnection in a magnetic flux tube with relativistic magnetization, finite resistivity, and strong guide field. Comparing with realistic NS parameters, this model represents the dynamics of a slender magnetic flux tube that is much thinner than the stellar radius. The seed current profile is smooth and does not spontaneously reconnect; instead, a discrete and localized current perturbation is introduced, representing e.g. localized energy release from a NS crust or magnetosphere. Three high-resolution relativistic magnetohydrodynamics simulations are described: one has uniform resistivity and Lundquist number such that reconnection proceeds in the plasmoid-mediated regime; the other two account for the feedback of charge starvation on the resistivity in current layers, where density is depleted; we provide a more general explanation for this depletion. All simulations produce a few dominant magnetic X-points and a secondary Kelvin-Helmholtz instability that excites high-wavenumber currents. We quantify the reconnection rate, the intermittency of dissipation, and the time profile of current spikes. We further present three-dimensional simulations confirming a limited growth of the ideal kink mode in the strong guide field regime. Applications are discussed, including to radio pulse microstructure and current damping below the magnetar surface during an X-ray flare, leading to mass loss and X-ray afterglow.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.22653",
  "author_total": 4,
  "authors": [
    {
      "name": "Michael P. Grehan"
    },
    {
      "name": "Christopher Thompson"
    },
    {
      "name": "Bart Ripperda"
    },
    {
      "name": "James R. Beattie"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/1kfz6tp6hfw7k.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.22653",
  "fulltext_url": null,
  "id": "1kfz6tp6hfw7k",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.22653",
  "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"
    ],
    [
      "arxiv",
      "physics.plasm-ph"
    ],
    [
      "openalex",
      "3103|Pulsars and Gravitational Waves Research"
    ]
  ],
  "openalex": "W7222938052",
  "pdf_url": "https://arxiv.org/pdf/2610.22653",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-15",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/1kfz6tp6hfw7k.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:30:32Z",
      "native_id": "2610.22653",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.22653"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    },
    {
      "field": "physics",
      "origin": "arxiv:physics.plasm-ph",
      "subfield": "plasma"
    }
  ],
  "title": "Sparking Dynamic, Relativistic Magnetic Reconnection in a Twisted Flux Tube",
  "title_text": "Sparking Dynamic, Relativistic Magnetic Reconnection in a Twisted Flux Tube",
  "type": "preprint",
  "updated_at": "2026-10-30T12:33:28Z",
  "url": "https://research.draconitic.com/paper/1kfz6tp6hfw7k",
  "venue": "arXiv",
  "versions": []
}