{
  "annotation_id": "4663d7b2-b68b-4c89-93ad-165476d88c29",
  "date_created": "2026-03-02T18:00:11.659000Z",
  "date_modified": "2026-03-02T18:00:11.659000Z",
  "file_hash": "2a14ed374192536cf0899e23e4413a9bc9d161f8ed86cd25b474cd59fee84d2c",
  "private": false,
  "record": {
    "abstract": "We have examined the properties of neutron-rich matter and finite nuclei in\nthe modified relativistic Hartree approximation for several values of the\nrenormalization scale, $\\mu$, around the standard choice of $\\mu$ equal to the\nnucleon mass $M$. Observed neutron star masses do not effectively constrain the\nvalue of $\\mu$. However for finite nuclei the value $\\mu/M=0.79$, suggested by\nnuclear matter data, provides a good account of the bulk properties with a\nsigma mass of about 600 MeV. This value of $\\mu/M$ renders the effective three\nand four body scalar self-couplings to be zero at 60\\% of equilibrium nuclear\nmatter density, rather than in the vacuum. We have also found that the matter\npart of the exchange diagram has little impact on the bulk properties of\nneutron stars.",
    "arxiv_id": "nucl-th/9307006",
    "authors": [
      "M. Prakash",
      "P. J. Ellis",
      "E. K. Heide",
      "S. Rudaz"
    ],
    "categories": [
      "nucl-th"
    ],
    "doi": "10.1016/0375-9474(94)90376-X",
    "title": "Neutron Stars and Nuclei in the Modified Relativistic Hartree   Approximation",
    "url": "https://arxiv.org/abs/nucl-th/9307006"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "e60fa049-5ce7-4cb9-81dc-bc3a60cc22e4",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}