{
  "id": "0902.4573",
  "version": "v1",
  "published": "2009-02-26T12:49:04.000Z",
  "updated": "2009-02-26T12:49:04.000Z",
  "title": "Evolution of Very Massive Population III Stars with Mass Accretion from Pre-Main Sequence to Collapse",
  "authors": [
    "Takuya Ohkubo",
    "Ken'ichi Nomoto",
    "Hideyuki Umeda",
    "Naoki Yoshida",
    "Sachiko Tsuruta"
  ],
  "comment": "24 pages, 11 figures (15 figure files)",
  "journal": "Astrophys.J.706:1184-1193,2009",
  "doi": "10.1088/0004-637X/706/2/1184",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "We calculate the evolution of zero-metallicity Population III (Pop III) stars whose mass grows from the initial mass of $\\sim 1M_{\\odot}$ by accreting the surrounding gases. Our calculations cover a whole evolutionary stages from the pre-main sequence, via various nuclear burning stages, through the final core collapse or pair-creation instability phases. We adopt the following stellar mass-dependent accretion rates which are derived from cosmological simulations of early structure formation based on the low mass dark matter halos at redshifts $z \\sim 20$: (1) the accretion rates for the first generation (Pop III.1) stars and (2) the rates for zero-metallicity but the second generation (Pop III.2) stars which are affected by radiation from the Pop III.1 stars. For comparison, we also study the evolution with the mass-dependent accretion rates which are affected by radiatibe feedback. We show that the final mass of Pop III.1 stars can be as large as $\\sim 1000M_{\\odot}$, beyond the mass range ($140 - 300M_{\\odot}$) for the pair-instability supernovae. Such massive stars undergo core-collapse to form intermediate-mass black holes, which may be the seeds for merger trees to supermassive black holes. On the other hand, Pop III.2 stars become less massive ($\\lsim 40 - 60M_{\\odot}$), being in the mass range of ordinary iron core-collapse stars. Such stars explode and eject heavy elements to contribute to chemical enrichment of the early universe as observed in the abundance patterns of extremely metal-poor stars in the Galactic halo.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2009-02-26T12:49:04.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "pre-main sequence",
      "mass accretion",
      "massive population",
      "low mass dark matter halos",
      "ordinary iron core-collapse stars"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "journal": "The Astrophysical Journal",
      "year": 2009,
      "month": "Dec",
      "volume": 706,
      "number": 2,
      "pages": 1184
    },
    "note": {
      "typesetting": "TeX",
      "pages": 24,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 814251,
      "adsabs": "2009ApJ...706.1184O"
    }
  }
}