{
  "annotation_id": "4c71128d-fd71-490a-9d81-04b7f65b365e",
  "date_created": "2026-03-02T18:00:07.959000Z",
  "date_modified": "2026-03-02T18:00:07.959000Z",
  "file_hash": "671849f0c20d1b0acee4298640d0565a096ca9e8b97cacfa4094e1100942f3f0",
  "private": false,
  "record": {
    "abstract": "To investigate the stability of the protoneutron stars in their early\nevolution, the minimum gravitational mass plays a fundamental role. This\nquantity depends upon the temperature profile assumed. We study within a static\napproach the stability of a protoneutron star. In particular we focus on a\nsuitable temperature profile suggested by dynamical calculations. We consider a\nprotoneutron star as composed of an isothermal core and an isentropic outer\npart. To describe physical properties of the interior we employ a\nmicroscopically derived equation of state for nuclear matter. For the outer\npart we employ the Lattimer-Swesty equation of state. The global structure is\nstudied. The assumed temperature profile turns out to give a range of stability\nwhich supports temperature values in line with those coming from dynamical\ncalculations. The maximum mass instead depends only upon the equation of state\nemployed.",
    "arxiv_id": "nucl-th/0607055",
    "authors": [
      "O. E. Nicotra"
    ],
    "categories": [
      "nucl-th",
      "astro-ph"
    ],
    "title": "Structure of protoneutron stars within a static approach",
    "url": "https://arxiv.org/abs/nucl-th/0607055"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "fa862bca-46b4-4f87-9d48-c29dfcff8c4e",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}