{
  "annotation_id": "e46006cf-77da-4b7c-8491-ef4eb4ec512e",
  "date_created": "2026-03-02T18:00:22.306000Z",
  "date_modified": "2026-03-02T18:00:22.306000Z",
  "file_hash": "6032e06ba6f18cd492bcb09d34ae7c4f77e818d031bbee5a3955ef3e003d8c45",
  "private": false,
  "record": {
    "abstract": "We construct the equation of state (EOS) of nuclear matter at finite\ntemperature and density with various proton fractions within the relativistic\nmean field (RMF) theory for the use in the supernova simulations. The\nThomas-Fermi approximation is adopted to describe the non-uniform matter where\nwe consider nucleus, alpha-particle, proton and neutron in equilibrium. We\ntreat the uniform matter and non-uniform matter consistently using the RMF\ntheory. We tabulate the outcome as the pressure, free energy, entropy etc, with\nenough mesh points in wide ranges of the temperature, proton fraction, and\nbaryon mass density.",
    "arxiv_id": "nucl-th/9806095",
    "authors": [
      "H. Shen",
      "H. Toki",
      "K. Oyamatsu",
      "K. Sumiyoshi"
    ],
    "categories": [
      "nucl-th",
      "astro-ph"
    ],
    "doi": "10.1143/PTP.100.1013",
    "journal_ref": "Prog. Theor. Phys. 100 (1998) 1013",
    "title": "Relativistic Equation of State of Nuclear Matter for Supernova Explosion",
    "url": "https://arxiv.org/abs/nucl-th/9806095"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "a5bf23c2-4972-47d7-9275-4b37125727b8",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}