{
  "annotation_id": "1eaf9938-280d-410b-8e63-2cdfe4f7903c",
  "date_created": "2026-03-02T18:00:18.210000Z",
  "date_modified": "2026-03-02T18:00:18.210000Z",
  "file_hash": "72ed18922dfce503bc0618d69312b9ec802a37fc16746824c5e9c9e0d868eaaa",
  "private": false,
  "record": {
    "abstract": "A protoneutron star is formed immediately after the gravitational collapse of\nthe core of a massive star. At birth, the hot and high density matter in such a\nstar contains a large number of neutrinos trapped during collapse. Trapped\nneutrinos generally inhibit the presence of exotic matter -- hyperons, a kaon\ncondensate, or quarks. However, as the neutrinos diffuse out in about 10-15 s,\nthe threshold for the appearance of strangeness is reduced; hence, the\ncomposition and the structure of the star can change significantly. The effect\nof exotic, negatively-charged, strangeness-bearing components is always to\nsoften the equation of state, and the possibility exists that the star\ncollapses to a black hole at this time. This could explain why no neutron star\nhas yet been seen in the remnant of supernova SN1987A, even though one\ncertainly existed when neutrinos were detected on Feb. 23, 1987. With new\ngeneration neutrino detectors it is feasible to test different theoretical\nscenarios observationally.",
    "arxiv_id": "nucl-th/9607031",
    "authors": [
      "M. Prakash",
      "S. Reddy",
      "J. M. Lattimer",
      "P. J. Ellis"
    ],
    "categories": [
      "nucl-th",
      "astro-ph",
      "hep-ph"
    ],
    "doi": "10.1007/BF03155623",
    "journal_ref": "Heavy Ion Phys.4:271-292,1996",
    "title": "Strangeness in Stellar Matter",
    "url": "https://arxiv.org/abs/nucl-th/9607031"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "e95442ef-af59-417e-a37d-954d44856a90",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}