{
  "annotation_id": "c6b551f7-d938-4880-98ef-ee7b960be688",
  "date_created": "2026-03-02T18:00:22.046000Z",
  "date_modified": "2026-03-02T18:00:22.046000Z",
  "file_hash": "181098572d394a4dd2a919ad74cf92eb3969a5043574b09250518de80e77f343",
  "private": false,
  "record": {
    "abstract": "We study the properties of static and rotating neutron stars adopting\nnon-relativistic equations of state (EOS) for asymmetric nuclear matter based\non the Brueckner-Hartree-Fock (BHF) scheme. The BHF calculation, with the\ncontinuous choice for the single particle potential, appears to be very close\nto the full EOS, which includes the three-hole line contribution calculated by\nsolving the Bethe-Fadeev equations within the gap choice for the single\nparticle potential. Three-body forces are included in order to reproduce the\ncorrect saturation point for nuclear matter. A comparison with fully\nrelativistic many-body calculations of nuclear matter EOS is made.",
    "arxiv_id": "nucl-th/9802055",
    "authors": [
      "M. Baldo",
      "G. F. Burgio",
      "H. Q. Song",
      "F. Weber"
    ],
    "categories": [
      "nucl-th",
      "astro-ph"
    ],
    "title": "Neutron star properties with nuclear BHF equations of state",
    "url": "https://arxiv.org/abs/nucl-th/9802055"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "9b0fac7c-4a57-49da-99a4-a61847a01bc4",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}