{
  "annotation_id": "364f05c5-7c29-4acb-b1e0-b6087f9ef392",
  "date_created": "2026-03-02T18:00:28.770000Z",
  "date_modified": "2026-03-02T18:00:28.770000Z",
  "file_hash": "598bf86122b43f6e2134519f16647ef6394704885aaf3788a0cbb7730dbf35f8",
  "private": false,
  "record": {
    "abstract": "A rotating system, such as a star, liquid drop, or atomic nucleus, may rotate\nas an oblate spheroid about its symmetry axis or, if the angular velocity is\ngreater than a critical value, as a triaxial ellipsoid about a principal axis.\nThe oblate and triaxial equilibrium configurations minimize the total energy, a\nsum of the rotational kinetic energy plus the potential energy. For a star or\ngalaxy the potential is the self-gravitating potential, for a liquid drop, the\nsurface tension energy, and for a nucleus, the potential is the sum of the\nrepulsive Coulomb energy plus the attractive surface energy. A simple, but\naccurate, Pad\\\u0027{e} approximation to the potential function is used for the\nenergy minimization problem that permits closed analytic expressions to be\nderived. In particular, the critical deformation and angular velocity for\nbifurcation from MacLaurin spheroids to Jacobi ellipsoids is determined\nanalytically in the approximation.",
    "arxiv_id": "nucl-th/9909074",
    "authors": [
      "Ts. Dankova",
      "G. Rosensteel"
    ],
    "categories": [
      "nucl-th"
    ],
    "doi": "10.1119/1.19050",
    "journal_ref": "Am.J.Phys. 66 (1998) 1095",
    "title": "Triaxial bifurcations of rapidly rotating spheroids",
    "url": "https://arxiv.org/abs/nucl-th/9909074"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "def2a553-14cd-4515-852d-1d4fb64bb8d1",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}