{
  "annotation_id": "62851f3f-3b2d-4e51-87ab-d9da064b24fb",
  "date_created": "2026-03-02T18:00:22.254000Z",
  "date_modified": "2026-03-02T18:00:22.254000Z",
  "file_hash": "b39c049d596869715a3fc87f4b987bb61d2317d9ed8ea5b6c1b23b24ebce54f5",
  "private": false,
  "record": {
    "abstract": "We construct the equation of state (EOS) of nuclear matter using the\nrelativistic mean field (RMF) theory in the wide density, temperature range\nwith various proton fractions for the use of supernova simulation and the\nneutron star calculations. We first construct the EOS of homogeneous nuclear\nmatter. We use then the Thomas-Fermi approximation to describe inhomogeneous\nmatter, where heavy nuclei are formed together with free nucleon gas. We\ndiscuss the results on free energy, pressure and entropy in the wide range of\nastrophysical interest. As an example, we apply the resulting EOS on the\nneutron star properties by using the Oppenheimer-Volkoff equation.",
    "arxiv_id": "nucl-th/9805035",
    "authors": [
      "H. Shen",
      "H. Toki",
      "K. Oyamatsu",
      "K. Sumiyoshi"
    ],
    "categories": [
      "nucl-th",
      "astro-ph"
    ],
    "doi": "10.1016/S0375-9474(98)00236-X",
    "journal_ref": "Nucl.Phys. A637 (1998) 435-450",
    "title": "Relativistic Equation of State of Nuclear Matter for Supernova and   Neutron Star",
    "url": "https://arxiv.org/abs/nucl-th/9805035"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "3fd2f060-2d38-486c-a41b-523628a9059b",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}