{
  "abstract": "Protoplanetary disc dispersal is driven by two processes usually modelled separately: photoevaporative and magnetohydrodynamic (MHD) disc winds. Global simulations indicate that in the inner disc these are not distinct outflows but a single magnetothermal wind. We assemble a closed-form, two-phase model that respects it. A single-field-line wind, whose base is fixed by the irradiated temperature and penetration column, supplies the launch and feeds a secular evolution, with photoevaporation convolved on as a sink. The flux closure $B_z\\proptoΣ^q$ is self-limiting: for $q\\le1/2$ depletion alone cannot demagnetise the disc, so dispersal requires independent flux loss, parameterised by the magnetic Reynolds number $\\mathcal{R}_m$. Integrating the coupled system yields two regimes. Efficient flux loss ($\\mathcal{R}_m\\lesssim1$) lets the magnetisation front recede by over an order of magnitude and opens a photoevaporative gap. Flux retention ($\\mathcal{R}_m\\gg1$) drives the front outward, sustains accretion, and defers dispersal by $\\approx2.7$~Myr. Deriving the base from stellar irradiation instead of prescribing it, we find that the cold-launch approximation is valid during the early stages of disc evolution: anchoring the base at plasma equipartition ($β_{\\rm base} \\sim 1$) confines irradiation's influence on the magnetic lever arm to the magnetothermal annulus, decoupling the peak accretion rate from the incident flux. Both regimes clear the disc inside-out, through either a photoevaporatively amplified cavity wall or an expanding magnetothermal front.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2609.18334",
  "author_total": 2,
  "authors": [
    {
      "name": "Giovanni Picogna"
    },
    {
      "name": "Barbara Ercolano"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/b45vj4mg8z5wh.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2609.18334",
  "fulltext_url": null,
  "id": "b45vj4mg8z5wh",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2609.18334",
  "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.EP"
    ],
    [
      "arxiv",
      "astro-ph.IM"
    ],
    [
      "openalex",
      "3103|Astrophysics and Star Formation Studies"
    ]
  ],
  "openalex": "W7213530517",
  "pdf_url": "https://arxiv.org/pdf/2609.18334",
  "pmcid": null,
  "pmid": null,
  "published": "2026-09-18",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/b45vj4mg8z5wh.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:23:03Z",
      "native_id": "2609.18334",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2609.18334"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.IM",
      "subfield": "instrumentation-methods"
    },
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.EP",
      "subfield": "planetary"
    }
  ],
  "title": "Bridging magnetothermal winds and photoevaporation to model discs dispersal",
  "title_text": "Bridging magnetothermal winds and photoevaporation to model discs dispersal",
  "type": "preprint",
  "updated_at": "2026-10-30T12:23:03Z",
  "url": "https://research.draconitic.com/paper/b45vj4mg8z5wh",
  "venue": "arXiv",
  "versions": []
}