{
  "annotation_id": "9d35acae-8a2c-49f5-9c80-44c4d2a5b3ea",
  "date_created": "2026-02-17T05:53:12.643000Z",
  "date_modified": "2026-02-17T05:53:12.643000Z",
  "file_hash": "7a219d315585535a123b55954a9e6a6e9143c240cf677ca7b7f33f3d8e18bd53",
  "private": false,
  "record": {
    "abstract": "Rapidly rotating, strongly magnetized neutron stars (``millisecond proto-magnetars\u0027\u0027) formed in stellar core-collapse, neutron star mergers, and white dwarf accretion-induced collapse have long been proposed as central engines of gamma-ray bursts (GRB) and accompanying supernovae/kilonovae. However, during the first few seconds after birth, neutrino heating drives baryon-rich winds from the neutron star surface, potentially limiting the magnetization and achievable Lorentz factors of the outflow and casting doubt on whether proto-magnetars can launch ultra-relativistic jets at early times, as needed to power short-duration GRB. We present 3D general-relativistic magnetohydrodynamic simulations of neutrino-heated proto-magnetar winds that incorporate M0 neutrino transport. While the global wind properties broadly agree with previous analytic estimates calibrated to one-dimensional models, our simulations reveal essential multidimensional effects. For rapidly rotating models with spin periods P = 1 ms, centrifugal forces strongly enhance mass loss near the rotational equator, producing a dense, sub-relativistic outflow ( ~0.1c). This equatorial wind naturally confines and collimates less baryon-loaded outflows emerging from higher latitudes, leading to the formation of a structured bipolar jet with a peak magnetization up to ~ 30-100 along the pole, sufficient to reach bulk Lorentz factors ~ 100 on larger scales. The resulting angular stratification of the outflow energy into ultra-relativistic polar and sub-relativistic equatorial components is broadly consistent with the observed partition between beaming-corrected GRB energies and supernova/kilonova ejecta. Our results demonstrate that millisecond proto-magnetars can launch relativistic jets within seconds of formation and highlight their potential role in powering the diverse electromagnetic counterparts of compact-object explosions.",
    "arxiv_id": "2601.07918",
    "authors": [
      "Dhruv K. Desai",
      "Luciano Combi",
      "Daniel M. Siegel",
      "Brian D. Metzger"
    ],
    "categories": [
      "astro-ph.HE",
      "gr-qc"
    ],
    "license": "http://creativecommons.org/licenses/by/4.0/",
    "title": "Relativistic jets from millisecond proto-magnetars",
    "url": "https://arxiv.org/abs/2601.07918",
    "version": "v2"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "58d535ff-a968-433f-bf34-0c90b1b5e02d",
    "id": "arXiv Dataset",
    "type": "Model",
    "variant": "snapshot-2026-01-17",
    "version": "0.1.0"
  },
  "user_id": 1000002
}