{
  "annotation_id": "3f41f937-a9f7-474a-ad9a-ed2787c5b9f4",
  "date_created": "2026-03-02T18:00:08.484000Z",
  "date_modified": "2026-03-02T18:00:08.484000Z",
  "file_hash": "29c785fcf3293520079e8d59de2f19584213acef1ec3419ee8533154b750f40e",
  "private": false,
  "record": {
    "abstract": "The effects of vector-isovector terms predicted by relativistic mean field\nmodels based on effective field theory on the equation of state and the\nneutrino mean free path in neutron stars have been studied. Using a procedure\nsimilar to Ref. [1] in treating the isovector sector, a parameter set (G2*)\nthat predicts a much smaller proton fraction than the standard one (G2) can be\nobtained. We found that the G2* has a softer equation of state compared to the\nG2 at higher densities and the disappearance of the anomalous behavior of the\nneutrino mean free path in neutron star does not depend on the proton fraction.",
    "arxiv_id": "nucl-th/0512095",
    "authors": [
      "A. Sulaksono",
      "P. T. P. Hutauruk",
      "C. K. Williams",
      "T. Mart"
    ],
    "categories": [
      "nucl-th",
      "astro-ph",
      "hep-ph"
    ],
    "title": "Relativistic Mean Field Models at High Densities",
    "url": "https://arxiv.org/abs/nucl-th/0512095"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "a4b39f7e-2a16-45e9-ae93-a0689f6d78af",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}