{
  "annotation_id": "d47da826-d1dd-4d36-803f-8096a471569a",
  "date_created": "2026-03-02T18:00:53.177000Z",
  "date_modified": "2026-03-02T18:00:53.177000Z",
  "file_hash": "95dce84345d2eb8b24fd95f98acc2c08b36343a89d342adbdb83ca9362f1c8b7",
  "private": false,
  "record": {
    "abstract": "Rapidly rotating spherical kinematic dynamos are computed using the\ncombination of a quasi geostrophic (QG) model for the velocity field and a\nclassical spectral 3D code for the magnetic field. On one hand, the QG flow is\ncomputed in the equatorial plane of a sphere and corresponds to Rossby wave\ninstabilities of a geostrophic internal shear layer produced by differential\nrotation. On the other hand, the induction equation is computed in the full\nsphere after a continuation of the QG flow along the rotation axis.\nDifferential rotation and Rossby-wave propagation are the key ingredients of\nthe dynamo process which can be interpreted in terms of $\\alpha\\Omega$ dynamo.\nTaking into account the quasi geostrophy of the velocity field to increase its\ntime and space resolution enables us to exhibit numerical dynamos with very low\nEkman (rapidly rotating) and Prandtl numbers (liquid metals) which are\nasymptotically relevant to model planetary core dynamos.",
    "arxiv_id": "physics/0410134",
    "authors": [
      "Nathanael Schaeffer",
      "Philippe Cardin"
    ],
    "categories": [
      "physics.class-ph",
      "astro-ph",
      "physics.geo-ph"
    ],
    "title": "Quasi-geostrophic kinematic dynamos at low magnetic Prandtl number",
    "url": "https://arxiv.org/abs/physics/0410134"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "229c6c1e-6779-4417-87e9-17762ebab91c",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}