{
  "id": "2209.01007",
  "version": "v1",
  "published": "2022-09-02T12:44:26.000Z",
  "updated": "2022-09-02T12:44:26.000Z",
  "title": "Mass loss and the Eddington parameter",
  "authors": [
    "Joachim M. Bestenlehner"
  ],
  "comment": "6 pages, 3 figures, Proceedings for IAU Symposium 361 \"Massive Stars Near and Far\" (eds. Nicole St-Louis, Jorick Vink, Jonathan Mackey)",
  "categories": [
    "astro-ph.SR",
    "astro-ph.HE"
  ],
  "abstract": "Mass loss through stellar winds plays a dominant role in the evolution of massive stars. Very massive stars (VMSs, $> 100 M_{\\odot}$) display Wolf-Rayet spectral morphologies (WNh) whilst on the main-sequence. Bestenlehner (2020) extended the elegant and widely used stellar wind theory by Castor, Abbott & Klein (1975) from the optically thin (O star) to the optically thick main-sequence (WNh) wind regime. The new mass-loss description is able to explain the empirical mass-loss dependence on the Eddington parameter and is suitable for incorporation into stellar evolution models for massive and very massive stars. The prescription can be calibrated with the transition mass-loss rate defined in Vink & Gr\\\"afener (2012). Based on the stellar sample presented in Bestenlehner et al. (2014) we derive a mass-loss recipe for the Large Magellanic Cloud using the new theoretical mass-loss prescription of Bestenlehner (2020).",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-09-02T12:44:26.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "eddington parameter",
      "mass loss",
      "massive stars",
      "display wolf-rayet spectral morphologies",
      "transition mass-loss rate"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}