Cosmological impact of population III binaries

Ke-Jung Chen, Volker Bromm, Alexander Heger, Myoungwon Jeon, Stanford E Woosley

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We present the results of the stellar feedback from Population III (Pop III) binaries by employing improved, more realistic Pop III evolutionary stellar models. To facilitate a meaningful comparison, we consider a fixed mass of 60 MO incorporated in Pop III stars, either contained in a single star, or split up in binary stars of 30 MO each or an asymmetric case of one 45 and one 15 MO star. Whereas the sizes of the resulting H II regions are comparable across all cases, the He III regions around binary stars are significantly smaller than that of the single star. Consequently, the He+ 1640 ? recombination line is expected to become much weaker. Supernova (SN) feedback exhibits great variety due to the uncertainty in possible explosion pathways. If at least one of the component stars dies as a hypernova about 10 times more energetic than conventional core-collapse SNe, the gas inside the host minihalo is effectively blown out, chemically enriching the intergalactic medium (IGM) to an average metallicity of 104-103 ZO4 3 , out to ?2 kpc. The single star, however, is more likely to collapse into a black hole, accompanied by at most very weak explosions. The effectiveness of early chemical enrichment would thus be significantly reduced, in contrast to the lower mass binary stars, where at least one component is likely to contribute to heavy element production and dispersal. Important new feedback physics is also introduced if close binaries can form high-mass X-ray binaries, leading to the pre-heating and -ionization of the IGM beyond the extent of the stellar H II regions.
Original languageEnglish
Pages (from-to)1-15
Number of pages15
JournalThe Astrophysical Journal
Issue number1
Publication statusPublished - 2015


  • early universe
  • galaxies: formation
  • radiative transfer
  • stars: formation
  • stars: Population III
  • supernovae: general

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