{
  "annotation_id": "2283202a-8cfa-4958-81bd-174ab1b8611d",
  "date_created": "2026-03-02T18:01:17.307000Z",
  "date_modified": "2026-03-02T18:01:17.307000Z",
  "file_hash": "c5db3239de85405dfe0899809b5e422dbb8489f5b554f238c808e9713094422d",
  "private": false,
  "record": {
    "abstract": "We quantify the scaling of magnetic energy density in the inertial range of\nsolar wind turbulence seen in-situ at 1AU with respect to solar activity. At\nsolar maximum, when the coronal magnetic field is dynamic and topologically\ncomplex, we find self-similar scaling in the solar wind, whereas at solar\nmimimum, when the coronal fields are more ordered, we find multifractality.\nThis quantifies the solar wind signature that is of direct coronal origin, and\ndistinguishes it from that of local MHD turbulence, with quantitative\nimplications for our understanding of coronal heating of the solar wind.",
    "arxiv_id": "physics/0702123",
    "authors": [
      "K. Kiyani",
      "S. C. Chapman",
      "B. Hnat",
      "R. M. Nicol"
    ],
    "categories": [
      "physics.space-ph",
      "physics.flu-dyn"
    ],
    "doi": "10.1103/PhysRevLett.98.211101",
    "journal_ref": "Phys. Rev. Lett. 98, 211101 (2007)",
    "title": "Self-similar signature of the active solar corona within the inertial   range of solar wind turbulence",
    "url": "https://arxiv.org/abs/physics/0702123"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "7323c43a-b286-4b9d-aa5b-7a1d707ad1f7",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}