{
  "id": "1906.07804",
  "version": "v1",
  "published": "2019-06-18T20:43:50.000Z",
  "updated": "2019-06-18T20:43:50.000Z",
  "title": "Chemical evolution models for the Galactic disk based on H II region abundances derived from a direct method and a temperature independent method",
  "authors": [
    "L. Carigi",
    "M. Peimbert",
    "A. Peimbert"
  ],
  "comment": "6 pages, 2 figures. Contributed talk given in the II workshop on Chemical Abundances in Gaseous Nebulae, held between 11-14 March 2019 in Sao Jose dos Campos, Sao Paulo, Brazil",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We present two chemical evolution models of our galaxy, both models are built to fit the O/H ratios derived from H II regions, using two different methods. One model is based on abundances obtained from the [O III] 4363/5007 temperatures (direct method, DM) and the other on abundances obtained from the recombination line ratios of [O II/H I] (temperature independent method, TIM). The differences between the O/H values obtained from these two methods are about 0.25 dex. We find that the model based on the TIM values produces an excellent fit to the observational stellar constraints (B-stars, Cepheids, and the Sun), while the model based on the DM fails to reproduce each of them. Moreover, the TIM model can explain the flattening of the O/H gradient observed in the inner disk due to the assumption of an inside-out star formation quenching, in the 3 - 6 kpc galactocentric range, starting ~ 9 Gyr ago.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2019-06-18T20:43:50.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "temperature independent method",
      "chemical evolution models",
      "direct method",
      "region abundances",
      "galactic disk"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}