{
  "id": "2107.03568",
  "version": "v1",
  "published": "2021-07-08T02:10:14.000Z",
  "updated": "2021-07-08T02:10:14.000Z",
  "title": "Nuclear fission chain reaction in cooling white dwarf stars",
  "authors": [
    "C. J. Horowitz",
    "M. E. Caplan"
  ],
  "comment": "8 pages, 4 figures",
  "categories": [
    "astro-ph.SR",
    "astro-ph.HE",
    "nucl-th"
  ],
  "abstract": "The first solids that form as a white dwarf (WD) starts to crystallize are expected to be greatly enriched in actinides. Previously [PRL 126, 1311010] we found that these solids might support a nuclear fission chain reaction that could ignite carbon burning and provide a new Type Ia supernova (SN Ia) mechanism involving an {\\it isolated} WD. Here we explore this fission mechanism in more detail and calculate the final temperature and density after the chain reaction and discuss a number of open physics questions.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-07-08T02:10:14.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "nuclear fission chain reaction",
      "cooling white dwarf stars",
      "type ia supernova",
      "open physics questions",
      "ignite carbon"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 8,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}