{
  "annotation_id": "baebddc2-a641-4fa9-82d2-77eeef9d42b5",
  "date_created": "2026-03-02T18:01:06.680000Z",
  "date_modified": "2026-03-02T18:01:06.680000Z",
  "file_hash": "ff253aac3867451c337a06878c963b8bdf131306776eab48a39e6991cd0e34cb",
  "private": false,
  "record": {
    "abstract": "We study the interaction between Venus and the solar wind using a global\nthree-dimensional self-consistent quasi-neutral hybrid (QNH) model. The model\ntreats ions (H+, O+) as particles and electrons as a massless charge\nneutralising fluid. In the analysed Parker spiral interplanetary magnetic field\n(IMF) case (IMF = [8.09, 5.88, 0] nT) a notable north-south asymmetry of the\nmagnetic field and plasma exists, especially in the properties of escaping\nplanetary O+ ions. The asymmetry is associated with ion finite gyroradius\neffects. Furthermore, the IMF x-component results in a dawn-dusk asymmetry.\nOverall, the QNH model is found to reproduce the main observed plasma and\nmagnetic field regions (the bow shock, the magnetosheath, the magnetic barrier\nand the magnetotail), implying the potential of the developed model to study\nthe Venusian plasma environment and especially the non-thermal ion escape.",
    "arxiv_id": "physics/0603243",
    "authors": [
      "E. Kallio",
      "R. Jarvinen",
      "P. Janhunen"
    ],
    "categories": [
      "physics.space-ph"
    ],
    "doi": "10.1016/j.pss.2006.04.030",
    "title": "Venus-Solar Wind Interaction: Asymmetries and the Escape of O+ Ions",
    "url": "https://arxiv.org/abs/physics/0603243"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "71b2248b-2142-4ccc-bdbd-cfb6ccd95ac4",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}