{
  "abstract": "The outcome of core-collapse supernova simulations depends sensitively on the multi-dimensional structure of the progenitor star at the onset of collapse. We perform three-dimensional simulations of the final ~10-15 minutes of stellar evolution for five non-rotating solar-metallicity progenitors with zero-age main-sequence masses of 20, 21.5, 24.5, 26, and 29 solar masses, mapped from one-dimensional MESA models into the FLASH hydrodynamics code. Convection develops in the oxygen-rich layers of all five models, with convective velocities reaching several hundred km/s, and in some models strong convection also develops in the inner silicon- and oxygen-burning shells. For the 24.5 solar mass progenitor, we carry out three core-collapse simulations: one initialised from the fully three-dimensional model, one from its angle-averaged counterpart, and one from the original one-dimensional MESA progenitor. We find that the multi-dimensional progenitor leads to 35 to 50% higher non-radial kinetic energy in the post-shock region and an average shock radius 5 to 10% larger than in the angle-averaged model, and shows the earliest shock revival of the three. The gravitational-wave emission is similar in all three models and strengthens after shock revival, driven by a change in the downflows reaching the protoneutron star rather than by progenitor asymmetries.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2608.28358",
  "author_total": 4,
  "authors": [
    {
      "name": "Haakon Andresen"
    },
    {
      "name": "Evan P. O'Connor"
    },
    {
      "name": "C. E. Fields"
    },
    {
      "name": "Sean M. Couch"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/fcekwc9yfgcrp.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2608.28358",
  "fulltext_url": null,
  "id": "fcekwc9yfgcrp",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2608.28358",
  "language": null,
  "licence": "LicenseRef-arXiv-nonexclusive-1.0",
  "licence_label": "arXiv licence",
  "licence_source": "article",
  "licence_url": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "astro-ph.HE"
    ],
    [
      "arxiv",
      "astro-ph.SR"
    ],
    [
      "openalex",
      "3103|Gamma-ray bursts and supernovae"
    ]
  ],
  "openalex": "W7204770945",
  "pdf_url": "https://arxiv.org/pdf/2608.28358",
  "pmcid": null,
  "pmid": null,
  "published": "2026-08-28",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/fcekwc9yfgcrp.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:17:22Z",
      "native_id": "2608.28358",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2608.28358"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    },
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.SR",
      "subfield": "stellar"
    }
  ],
  "title": "Three-dimensional Core-Collapse Supernova Simulations: From shell burning to shock revival",
  "title_text": "Three-dimensional Core-Collapse Supernova Simulations: From shell burning to shock revival",
  "type": "preprint",
  "updated_at": "2026-10-30T12:17:22Z",
  "url": "https://research.draconitic.com/paper/fcekwc9yfgcrp",
  "venue": "arXiv",
  "versions": []
}