{
  "annotation_id": "ff3cdfb5-9022-423a-b5c7-f806b54bb3f4",
  "date_created": "2026-03-02T18:00:29.339000Z",
  "date_modified": "2026-03-02T18:00:29.339000Z",
  "file_hash": "b772a73f8e5aa2cb4a54be9826703c4cfb0960de62e0b89888d948f8d08996f2",
  "private": false,
  "record": {
    "abstract": "In the framework of the Brueckner-Bethe-Goldstone theory, we determine a\nfully microscopic equation of state for asymmetric and $\\beta$-stable nuclear\nmatter containing $\\sim$ and $\\la$ hyperons. We use the Paris and the new\nArgonne $Av_{18}$ two-body nucleon interaction, whereas the nucleon-hyperon\ninteraction is described by the Njimegen soft-core model. We stress the role\nplayed by the three-body nucleon interaction, which produces a strong repulsion\nat high densities. This enhances enormously the hyperon population, and\nproduces a strong softening of the equation of state, which turns out almost\nindependent on the nucleon-nucleon interaction. We use the new equation of\nstate in order to calculate the structure of static neutron stars. We obtain a\nmaximum mass configuration with $M_{\\rm max}$ = 1.26 (1.22) when the Paris\n($Av_{18}$) nucleon potential is adopted. Central densities are about 10 times\nnormal nuclear matter density. Stellar rotations, treated within a perturbative\napproach, increase the value of the limiting mass by about 12%.",
    "arxiv_id": "nucl-th/9912066",
    "authors": [
      "M. Baldo",
      "G. F. Burgio",
      "H. -J. Schulze"
    ],
    "categories": [
      "nucl-th",
      "astro-ph"
    ],
    "doi": "10.1103/PhysRevC.61.055801",
    "journal_ref": "Phys.Rev.C61:055801,2000",
    "title": "Hyperon stars in the Brueckner-Bethe-Goldstone theory",
    "url": "https://arxiv.org/abs/nucl-th/9912066"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "893a075f-39cf-4c64-bcb2-313abd4e5c71",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}