{
  "abstract": "Two-dimensional (2D) coronal seismology based on coronagraphic imaging spectroscopy has emerged as a promising method for mapping the coronal magnetic field, but the physical meaning of its inferred quantities under optically thin line-of-sight (LOS) integration remains uncertain. We investigate this problem by synthesizing coronagraphic observables from a global wave-driven magnetohydrodynamic model with a long LOS extent and a structured corona, and by applying the same analysis procedures used for observations. We compare the diagnosed density, wave propagation direction, phase speed, and magnetic-field strength with different LOS-weighted reference quantities from the model. We find that the measured density and the wave propagation direction are both well represented by LOS emissivity-weighted quantities. In contrast, the phase speed is not controlled by emissivity weighting alone: the LOS distribution of wave velocity amplitude also plays an important role. As a result, the inferred magnetic field is better represented by combining the emissivity-weighted density with an amplitude-dependent effective speed. Emissivity weighting nevertheless remains a reasonable approximation, and a useful baseline, over much of the field of view, especially where the LOS does not cross strongly structured plasma-sheet-like regions. These results clarify the physical interpretation of 2D coronal seismology and provide guidance for future coronal magnetic-field tomography and model-constrained applications.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.17433",
  "author_total": 5,
  "authors": [
    {
      "name": "Zihao Yang"
    },
    {
      "name": "Yuhong Fan"
    },
    {
      "name": "Giuliana de Toma"
    },
    {
      "name": "Sarah Gibson"
    },
    {
      "name": "Matthias Rempel"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/cjzjz20xc9hc6.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.17433",
  "fulltext_url": null,
  "id": "cjzjz20xc9hc6",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.17433",
  "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.SR"
    ],
    [
      "openalex",
      "3103|Solar and Space Plasma Dynamics"
    ]
  ],
  "openalex": "W7221810323",
  "pdf_url": "https://arxiv.org/pdf/2610.17433",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-12",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/cjzjz20xc9hc6.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:29:11Z",
      "native_id": "2610.17433",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.17433"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.SR",
      "subfield": "stellar"
    }
  ],
  "title": "What Does 2D Coronal Seismology Measure?",
  "title_text": "What Does 2D Coronal Seismology Measure?",
  "type": "preprint",
  "updated_at": "2026-10-30T12:29:11Z",
  "url": "https://research.draconitic.com/paper/cjzjz20xc9hc6",
  "venue": "arXiv",
  "versions": []
}