{
  "annotation_id": "cd658994-9579-4b02-b67b-44aecbdb1434",
  "date_created": "2026-03-02T18:00:15.416000Z",
  "date_modified": "2026-03-02T18:00:15.416000Z",
  "file_hash": "749ecf219ea0f756276b4ae8a893bd29aebdb578ef1841b3669cdd65b18b2e30",
  "private": false,
  "record": {
    "abstract": "An equation of state(EOS) of nuclear matter with explicit inclusion of a\nspin-isospin dependent force is constructed from a finite range, momentum and\ndensity dependent effective interaction. This EOS is found to be in good\nagreement with those obtained from more sophisticated models for unpolarised\nnuclear matter. Introducing spin degrees of freedom, it is found that at\ndensity about 2.5 times the density of normal nuclear matter the neutron matter\nundergoes a ferromagnetic transition. The maximum mass and the radius of the\nneutron star agree favourably with the observations. Since finding quark matter\nrather than spin polarised nuclear matter at the core of neutron stars is more\nprobable, the proposed EOS is also applied to the study of hybrid stars. It is\nfound using the bag model picture that one can in principle describe both the\nmass and size as well as the surface magnetic field of hybrid stars\nsatisfactorily.",
    "arxiv_id": "nucl-th/9604042",
    "authors": [
      "V. S. Uma Maheswari",
      "D. N. Basu",
      "J. N. De",
      "S. K. Samaddar"
    ],
    "categories": [
      "nucl-th"
    ],
    "doi": "10.1016/S0375-9474(97)00002-X",
    "journal_ref": "Nucl.Phys. A615 (1997) 516-536",
    "title": "Spin polarised nuclear matter and its application to neutron stars",
    "url": "https://arxiv.org/abs/nucl-th/9604042"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "aa693025-4f47-4416-b0b5-7d0f558fd146",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}