{
  "annotation_id": "82735643-93f5-4605-869b-072d15107150",
  "date_created": "2026-03-02T18:00:39.171000Z",
  "date_modified": "2026-03-02T18:00:39.171000Z",
  "file_hash": "991cdac8c0eda243e5fff65b84b79dc0a29c04f20542c23167996ad05aad8f15",
  "private": false,
  "record": {
    "abstract": "We apply the finite size scaling technique to quantify the statistical\nproperties of fluctuations in AU, AL and AE indices and in the epsilon\nparameter that represents energy input from the solar wind into the\nmagnetosphere. We find that the exponents needed to rescale the probability\ndensity functions (PDF) of the fluctuations are the same to within experimental\nerror for all four quantities. This self-similarity persists for time scales up\nto ~4 hours for AU, AL and epsilon and up to ~2 hours for AE. Fluctuations on\nshorter time scales than these are found to have similar long-tailed\n(leptokurtic) PDF, consistent with an underlying turbulent process. These\nquantitative and model-independent results place important constraints on\nmodels for the coupled solar wind-magnetosphere system.",
    "arxiv_id": "physics/0208021",
    "authors": [
      "B. Hnat",
      "S. C. Chapman",
      "G. Rowlands",
      "N. W. Watkins",
      "M. P. Freeman"
    ],
    "categories": [
      "physics.space-ph",
      "physics.data-an"
    ],
    "doi": "10.1029/2002GL016054",
    "journal_ref": "Geophys. Res. Lett., 29(22), 2078, 2002",
    "title": "Scaling of solar wind epsilon and the AU, AL and AE indices",
    "url": "https://arxiv.org/abs/physics/0208021"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "30454353-0ab3-4e93-9e7e-db04ae231cfe",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}