{
  "annotation_id": "42844057-ad54-429b-a21c-bf59e3ba068b",
  "date_created": "2026-03-02T18:00:04.284000Z",
  "date_modified": "2026-03-02T18:00:04.284000Z",
  "file_hash": "596ebd2e896e5a114b5efea5b43d9fe529940932057d87925636843770cf4295",
  "private": false,
  "record": {
    "abstract": "An accurately calibrated relativistic parametrization is introduced to\ncompute the ground state properties of finite nuclei, their linear response,\nand the structure of neutron stars. While similar in spirit to the successful\nNL3 parameter set, it produces an equation of state that is considerably softer\n-- both for symmetric nuclear matter and for the symmetry energy. This\nsoftening appears to be required for an accurate description of several\ncollective modes having different neutron-to-proton ratios. Among the\npredictions of this model are a symmetric nuclear-matter incompressibility of\nK=230 MeV and a neutron skin thickness in 208Pb of Rn-Rp=0.21 fm. Further, the\nimpact of such a softening on the properties of neutron stars is as follows:\nthe model predicts a limiting neutron star mass of Mmax=1.72 Msun, a radius of\nR=12.66 km for a ``canonical\u0027\u0027 M=1.4 Msun neutron star, and no (nucleon) direct\nUrca cooling in neutrons stars with masses below M=1.3 Msun.",
    "arxiv_id": "nucl-th/0504034",
    "authors": [
      "B. G. Todd-Rutel",
      "J. Piekarewicz"
    ],
    "categories": [
      "nucl-th",
      "astro-ph",
      "nucl-ex"
    ],
    "doi": "10.1103/PhysRevLett.95.122501",
    "journal_ref": "Phys. Rev. Lett. 95, 122501 (2005)",
    "title": "Neutron-Rich Nuclei in Heaven and Earth",
    "url": "https://arxiv.org/abs/nucl-th/0504034"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "286c5e5c-3016-4179-960a-fa3f702b25b9",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}