{
  "id": "1709.08619",
  "version": "v1",
  "published": "2017-09-25T17:59:07.000Z",
  "updated": "2017-09-25T17:59:07.000Z",
  "title": "Galactic evolution of Copper in the light of NLTE computations",
  "authors": [
    "S. Andrievsky",
    "P. Bonifacio",
    "E. Caffau",
    "S. Korotin",
    "M. Spite",
    "F. Spite",
    "L. Sbordone",
    "A. V. Zhukova"
  ],
  "comment": "To be published in MNRAS",
  "categories": [
    "astro-ph.SR",
    "astro-ph.GA"
  ],
  "abstract": "We have developed a model atom for Cu with which we perform statistical equilibrium computations that allow us to compute the line formation of Cu I lines in stellar atmospheres without assuming Local Thermodynamic Equilibrium (LTE). We validate this model atom by reproducing the observed line profiles of the Sun, Procyon and eleven metal-poor stars. Our sample of stars includes both dwarfs and giants. Over a wide range of stellar parameters we obtain excellent agreement among different Cu I lines. The eleven metal-poor stars have iron abundances in the range -4.2 <= [Fe/H] <= -1.4, the weighted mean of the [Cu/Fe] ratios is -0.22 dex, with a scatter of -0.15 dex. This is very different from the results from LTE analysis (the difference between NLTE and LTE abundances reaches 1 dex) and in spite of the small size of our sample it prompts for a revision of the Galactic evolution of Cu.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-09-25T17:59:07.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "galactic evolution",
      "nlte computations",
      "metal-poor stars",
      "model atom",
      "perform statistical equilibrium computations"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}