{
  "id": "1112.0936",
  "version": "v1",
  "published": "2011-12-05T14:28:13.000Z",
  "updated": "2011-12-05T14:28:13.000Z",
  "title": "Wind Models for Very Massive Stars in the Local Universe",
  "authors": [
    "Jorick S. Vink",
    "J. M. Bestenlehner",
    "G. Graefener",
    "A. de Koter",
    "N. Langer"
  ],
  "comment": "To appear in Four Decades of Research on Massive Stars, ASP Conf. Ser. 5 pages, 2 figures",
  "categories": [
    "astro-ph.SR",
    "astro-ph.CO",
    "astro-ph.GA"
  ],
  "abstract": "Some studies have claimed the existence of a stellar upper-mass limit of 150 Msun. A factor that is often overlooked concerns the issue that there might be a significant difference between the present-day and the initial mass of the most massive stars - as a result of mass loss. The upper-mass limit may be substantially higher, possibly exceeding 200 Msun. The issue of the upper mass-limit will however remain uncertain as long as there is only limited quantitative knowledge of mass loss in close proximity to the Eddington (= Gamma) limit. For this reason, we present mass-loss predictions from Monte Carlo radiative transfer models for very massive stars up to 300 Msun. Using our new dynamical approach, we find an upturn or \"kink\" in the mass-loss versus Gamma dependence, at the point where our model winds become optically thick. These are the first mass-loss predictions where the transition from optically thin O-star winds to optically thick Wolf-Rayet winds has been resolved.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2011-12-05T14:28:13.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "massive stars",
      "local universe",
      "wind models",
      "upper-mass limit",
      "mass-loss predictions"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 5,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1080028,
      "adsabs": "2012ASPC..465..207V"
    }
  }
}