{
  "id": "1906.01897",
  "version": "v1",
  "published": "2019-06-05T09:13:46.000Z",
  "updated": "2019-06-05T09:13:46.000Z",
  "title": "Two-fluid numerical simulations of the origin of the fast solar wind",
  "authors": [
    "D. Wójcik",
    "B. Kuźma",
    "K. Murawski",
    "A. K. Srivastava"
  ],
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "With the use of our JOANNA code, which solves radiative equations for ion + electron and neutralfluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solargranulation. These outflows exhibit physical quantities consistentto the order of magnitude with theobservational findings for mass and energy losses in the upper chromosphere, transition region andinner corona, and they may originate the fast solar wind.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2019-06-05T09:13:46.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "fast solar wind",
      "two-fluid numerical simulations",
      "transition region andinner corona",
      "joanna code",
      "physical quantities consistentto"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}