{
  "annotation_id": "520a12ba-9a3f-4bbf-a474-bf906c1600ab",
  "date_created": "2026-03-02T18:00:31.754000Z",
  "date_modified": "2026-03-02T18:00:31.754000Z",
  "file_hash": "1624500e39ab1279560c7eefc78a92a8f40acb3b3cabda625fcb041ed63634fe",
  "private": false,
  "record": {
    "abstract": "An integrated Magneto-Fluid model, that accords full treatment to the\nVelocity fields associated with the directed plasma motion, is developed to\ninvestigate the dynamics of coronal structures. It is suggested that the\ninteraction of the fluid and the magnetic aspects of plasma may be a crucial\nelement in creating so much diversity in the solar atmosphere. It is shown that\nthe structures which comprise the solar corona can be created by particle\n(plasma) flows observed near the Sun\u0027s surface - the primary heating of these\nstructures is caused by the viscous dissipation of the flow kinetic energy.",
    "arxiv_id": "physics/0009086",
    "authors": [
      "Swadesh M. Mahajan",
      "Ryszard Miklaszewski",
      "Kommunela I. Nikol\u0027skaya",
      "Nana L. Shatashvili"
    ],
    "categories": [
      "physics.plasm-ph",
      "astro-ph"
    ],
    "doi": "10.1063/1.1350670",
    "title": "Formation and Primary Heating of The Solar Corona - Theory and   Simulation",
    "url": "https://arxiv.org/abs/physics/0009086"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "a516137f-d065-4c18-834b-b3b16b256e8b",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}