{
  "annotation_id": "c1594e19-0f83-4b8a-87d6-1749fa36203c",
  "date_created": "2026-03-02T18:00:11.966000Z",
  "date_modified": "2026-03-02T18:00:11.966000Z",
  "file_hash": "f79ab647a57ac00a9a37f6642c41d9e603a08da8dd429386a9f9b534a9762a97",
  "private": false,
  "record": {
    "abstract": "We consider the neutron matter quark matter phase transition along with\npossible existence of hybrid quark stars. The equation of state for neutron\nmatter is obtained using a nonperturbative method with pion dressing of the\nneutron matter and an analysis similar to that of symmetric nuclear matter. The\nquark matter sector is treated perturbatively in the small distance domain. For\nbag constant $B^{1/4}$=148 MeV, a first order phase transition is seen. In the\ncontext of neutron quark hybrid stars, Tolman-Oppenheimer-Volkoff equations are\nsolved using the equations of state for quark matter and for neutron matter\nwith a phase transition as noted earlier. Stable solutions for such stars are\nobtained with the Chandrasekhar limit as 1.58 $M_\\odot$ and radius around 10\nkm. The bulk of the star is quark matter with a thin crust of neutron matter of\nless than a kilometer.",
    "arxiv_id": "nucl-th/9301003",
    "authors": [
      "H. Mishra",
      "S. P. Misra",
      "P. K. Panda",
      "B. K. Parida"
    ],
    "categories": [
      "nucl-th"
    ],
    "doi": "10.1142/S0218301393000212",
    "journal_ref": "Int.J.Mod.Phys.E2:547-564,1993",
    "title": "Neutron matter - Quark matter phase transition and Quark star",
    "url": "https://arxiv.org/abs/nucl-th/9301003"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "8bc221bc-9cdf-460a-9cb0-a085abe86b02",
    "id": "arXiv Dataset IDs",
    "type": "Model",
    "variant": "snapshot-2026-03-01",
    "version": "0.1.0"
  },
  "user_id": 1000002
}