The evolution of supermassive population III stars

Lionel Haemmerlé, Tyrone E. Woods, Ralf S. Klessen, Alexander Heger, Daniel J. Whalen

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Abstract

Supermassive primordial stars forming in atomically-cooled halos at z∼15−20 are currently thought to be the progenitors of the earliest quasars in the Universe. In this picture, the star evolves under accretion rates of 0.1−1 M yr−1 until the general relativistic instability triggers its collapse to a black hole at masses of ∼105 M. However, the ability of the accretion flow to sustain such high rates depends crucially on the photospheric properties of the accreting star, because its ionising radiation could reduce or even halt accretion. Here we present new models of supermassive Population III protostars accreting at rates 0.001−10 M yr−1, computed with the GENEVA stellar evolution code including general relativistic corrections to the internal structure. We use the polytropic stability criterion to estimate the mass at which the collapse occurs, which has been shown to give a lower limit of the actual mass at collapse in recent hydrodynamic simulations. We find that at accretion rates higher than 0.001 M yr−1 the stars evolve as red, cool supergiants with surface temperatures below 104 K towards masses >105M, and become blue and hot, with surface temperatures above 105 K,only for rates ≲0.001 M yr−1. Compared to previous studies, our results extend the range of masses and accretion rates at which the ionising feedback remains weak, reinforcing the case for direct collapse as the origin of the first quasars.
Original languageEnglish
Pages (from-to)2757-2773
Number of pages17
JournalMonthly Notices of the Royal Astronomical Society
Volume474
Issue number2
Early online date16 Nov 2017
DOIs
Publication statusPublished - 21 Feb 2018

Keywords

  • astro-ph.SR
  • RCUK
  • STFC
  • ST/P000509/1
  • quasars: supermassive black holes
  • early universe
  • dark ages, reionization, first stars
  • stars: Population III
  • galaxies: high-redshift
  • stars: massive

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