{
  "annotation_id": "0f359423-de93-47d8-b65f-4229013132e8",
  "date_created": "2026-03-02T18:00:11.714000Z",
  "date_modified": "2026-03-02T18:00:11.714000Z",
  "file_hash": "219f1794f35f6ec82590732e2e77bcb0eba328c581bbf4322f90a4ced724ca3a",
  "private": false,
  "record": {
    "abstract": "An equation of state (EOS) for uniform nuclear matter is constructed at zero\nand finite temperatures with the variational method starting from the realistic\nnuclear Hamiltonian composed of the Argonne V18 and UIX potentials. The energy\nis evaluated in the two-body cluster approximation with the three-body-force\ncontribution treated phenomenologically so as to reproduce the empirical\nsaturation conditions. The obtained energies for symmetric nuclear matter and\nneutron matter at zero temperature are in fair agreement with those by Akmal,\nPandharipande and Ravenhall, and the maximum mass of the neutron star is 2.2\nMsolar. At finite temperatures, a variational method by Schmidt and\nPandharipande is employed to evaluate the free energy, which is used to derive\nvarious thermodynamic quantities of nuclear matter necessary for supernova\nsimulations. The result of this variational method at finite temperatures is\nfound to be self-consistent.",
    "arxiv_id": "nucl-th/0701069",
    "authors": [
      "H. Kanzawa",
      "K. Oyamatsu",
      "K. Sumiyoshi",
      "M. Takano"
    ],
    "categories": [
      "nucl-th",
      "astro-ph"
    ],
    "doi": "10.1016/j.nuclphysa.2007.01.098",
    "journal_ref": "Nucl.Phys.A791:232-250,2007",
    "title": "Variational Calculation for the Equation of State of Nuclear Matter at   Finite Temperatures",
    "url": "https://arxiv.org/abs/nucl-th/0701069"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "3a174ea1-eada-4b6e-8474-ed74ba16f6d2",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}