dorsal/arxiv
View SchemaSupernova Neutrino-Nucleus Physics and the r-process
| Authors | W. C. Haxton |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/0406012 |
| URL | https://arxiv.org/abs/nucl-th/0406012 |
| DOI | 10.1142/9789812702470_0009 |
Abstract
This talk reviews three inputs important to neutrino-induced nucleosynthesis in a supernova: 1) "standard" properties of the supernova neutrino flux, 2) effects of phenomena like neutrino oscillations on that flux, and 3) nuclear structure issues in estimating cross sections for neutrino-nucleus interactions. The resulting possibilities for neutrino-induced nucleosynthesis -- the neutrino-process -- in massive stars are discussed. This includes two relatively recent extensions of neutrino-process calculations to heavier nuclei, one focused on understanding the origin of 138La and 180Ta and the second on the effects following r-process freezeout. From calculations of the neutrino post-processing of the r-process distribution, limits can be placed on the neutrino fluence after freezeout and thus on the dynamic timescale for the expansion of the "hot bubble."
{
"annotation_id": "a3980491-20e5-481d-85aa-1f62d4a18425",
"date_created": "2026-03-02T18:00:01.136000Z",
"date_modified": "2026-03-02T18:00:01.136000Z",
"file_hash": "7965b933ab6a5447a1f6e0007bc73d1a8ebab5f0ec31c0452e068ca188950728",
"private": false,
"record": {
"abstract": "This talk reviews three inputs important to neutrino-induced nucleosynthesis\nin a supernova: 1) \"standard\" properties of the supernova neutrino flux, 2)\neffects of phenomena like neutrino oscillations on that flux, and 3) nuclear\nstructure issues in estimating cross sections for neutrino-nucleus\ninteractions. The resulting possibilities for neutrino-induced nucleosynthesis\n-- the neutrino-process -- in massive stars are discussed. This includes two\nrelatively recent extensions of neutrino-process calculations to heavier\nnuclei, one focused on understanding the origin of 138La and 180Ta and the\nsecond on the effects following r-process freezeout. From calculations of the\nneutrino post-processing of the r-process distribution, limits can be placed on\nthe neutrino fluence after freezeout and thus on the dynamic timescale for the\nexpansion of the \"hot bubble.\"",
"arxiv_id": "nucl-th/0406012",
"authors": [
"W. C. Haxton"
],
"categories": [
"nucl-th",
"astro-ph",
"hep-ph"
],
"doi": "10.1142/9789812702470_0009",
"title": "Supernova Neutrino-Nucleus Physics and the r-process",
"url": "https://arxiv.org/abs/nucl-th/0406012"
},
"schema_id": "dorsal/arxiv",
"source": {
"execution_id": "14c5f079-1d33-4fe1-8c86-00b63e7231ab",
"id": "arXiv Dataset IDs",
"type": "Model",
"variant": "snapshot-2026-03-01",
"version": "0.1.0"
},
"user_id": 1000002
}