{
  "id": "2106.01679",
  "version": "v1",
  "published": "2021-06-03T08:25:56.000Z",
  "updated": "2021-06-03T08:25:56.000Z",
  "title": "Impact of hypernova νp-process nucleosynthesis on the galactic chemical evolution of Mo and Ru",
  "authors": [
    "Hirokazu Sasaki",
    "Yuta Yamazaki",
    "Toshitaka Kajino",
    "Motohiko Kusakabe",
    "Takehito Hayakawa",
    "Myung-Ki Cheoun",
    "Heamin Ko",
    "Grant J. Mathews"
  ],
  "comment": "12 pages, 3 figures",
  "categories": [
    "astro-ph.GA",
    "astro-ph.HE",
    "astro-ph.SR"
  ],
  "abstract": "We calculate Galactic Chemical Evolution (GCE) of Mo and Ru by taking into account the contribution from $\\nu p$-process nucleosynthesis. We estimate yields of $p$-nuclei such as $^{92,94}\\mathrm{Mo}$ and $^{96,98}\\mathrm{Ru}$ through the $\\nu p$-process in various supernova (SN) progenitors based upon recent models. In particular, the $\\nu p$-process in energetic hypernovae produces a large amount of $p$-nuclei compared to the yield in ordinary core-collapse SNe. Because of this the abundances of $^{92,94}\\mathrm{Mo}$ and $^{96,98}\\mathrm{Ru}$ in the Galaxy are significantly enhanced at [Fe/H]=0 by the $\\nu p$-process. We find that the $\\nu p$-process in hypernovae is the main contributor to the elemental abundance of $^{92}$Mo at low metallicity [Fe/H$]<-2$. Our theoretical prediction of the elemental abundances in metal-poor stars becomes more consistent with observational data when the $\\nu p$-process in hypernovae is taken into account.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-06-03T08:25:56.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "galactic chemical evolution",
      "elemental abundance",
      "energetic hypernovae produces",
      "ordinary core-collapse sne",
      "observational data"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 12,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}