<i>ONE HUNDRED FIRST STARS</i>: PROTOSTELLAR EVOLUTION AND THE FINAL MASSES

Hirano, Shingo; Hosokawa, Takashi; Yoshida, Naoki; Umeda, Hideyuki; Omukai, Kazuyuki; Chiaki, Gen; Yorke, H. W.

doi:10.1088/0004-637x/781/2/60

Cited by 564 publications

(670 citation statements)

References 88 publications

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“…In the "PopIII star remnants" scenario, BHs are predicted to form in mini-haloes (M h ≈ 10 5 M ) with gas below a critical metallicity (Z < 10 −3.5 Z , Bromm et al 2001;Schneider et al 2002) at redshift z = 30 − 20 from the remnants of the first generation of stars (PopIII, Madau & Rees 2001;Volonteri, Madau & Haardt 2003). Observational evidence on the initial mass function (IMF) of PopIII stars are lacking, but theoretical studies suggest that they could have masses in the range 10 − 1000 M (Bromm & Yoshida 2011;Hirano et al 2014). A massive star M 260M can lead to the formation of a BH seed of ≈ 100 M (Fryer, Woosley & Heger 2001), retaining half the mass of the star.…”

Section: Introductionmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

246

223

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Massive black holes (BHs) inhabit local galaxies, including the Milky Way and some dwarf galaxies. BH formation, occurring at early cosmic times, must account for the properties of BHs in today's galaxies, notably why some galaxies host a BH, and others do not. We investigate the formation, distribution and growth of BH 'seeds' by using the adaptive mesh refinement code Ramses. We develop an implementation of BH formation in dense, low-metallicity environments, as advocated by models invoking the collapse of the first generation of stars, or of dense nuclear star clusters. The seed masses are computed one-by-one on-the-fly, based on the star formation rate and the stellar initial mass function. This self-consistent method to seed BHs allows us to study the distribution of BHs in a cosmological context and their evolution over cosmic time. We find that all high-mass galaxies tend to host a BH, whereas low-mass counterparts have a lower probability of hosting a BH. After the end of the epoch of BH formation, this probability is modulated by the growth of the galaxy. The simulated BHs connect to low-redshift observational samples, and span a similar range in accretion properties as Lyman-Break Analogs. The growth of BHs in low-mass galaxies is stunted by strong supernova feedback. The properties of BHs in dwarf galaxies thus remain a testbed for BH formation. Simulations with strong supernova feedback, which is able to quench BH accretion in shallow potential wells, produce galaxies and BHs in better agreement with observational constraints.

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Section: Introductionmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

246

223

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“…Obviously, statistical studies are needed to study the overall mass distribution of primordial stars. Our previous work (Hirano et al 2014, hereafter Paper I) achieves this goal with more than one hundred cosmological samples of primordial star-forming clouds. We first follow the early evolution until the formation of the protostellar core with three-dimensional (3D) cosmological simulations.…”

Section: Introductionmentioning

confidence: 99%

Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution

Hirano

Hosokawa

Yoshida

et al. 2015

Monthly Notices of the Royal Astronomical Society

333

313

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We perform a large set of cosmological simulations of early structure formation and follow the formation and evolution of 1540 star-forming gas clouds to derive the mass distribution of primordial stars. The star formation in our cosmological simulations is characterized by two distinct populations, the so-called Population III.1 stars and primordial stars formed under the influence of far-ultraviolet (FUV) radiation (Population III.2 D stars). In this work, we determine the stellar masses by using the dependences on the physical properties of star-forming cloud and/or the external photodissociating intensity from nearby primordial stars, which are derived from the results of 2D radiation hydrodynamic simulations of protostellar feedback. The characteristic mass of the Pop III stars is found to be a few hundred solar masses at z ∼ 25, and it gradually shifts to lower masses with decreasing redshift. At high redshifts z > 20, about half of the star-forming gas clouds are exposed to intense FUV radiation and thus give birth to massive Pop III.2 D stars. However, the local FUV radiation by nearby Pop III stars becomes weaker at lower redshifts, when typical Pop III stars have smaller masses and the mean physical separation between the stars becomes large owing to cosmic expansion. Therefore, at z < 20, a large fraction of the primordial gas clouds host Pop III.1 stars. At z 15, the Pop III.1 stars are formed in relatively cool gas clouds due to efficient radiative cooling by H 2 and HD molecules; such stars have masses of a few ×10 M ⊙ . Since the stellar evolution and the final fate are determined by the stellar mass, Pop III stars formed at different epochs play different roles in the early Universe.

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“…However, recent simulations found that the protostellar disk forming in the minihalo fragments into multiple clumps (Clark et al 2011;Greif et al 2012;Stacy et al 2012;Latif et al 2013b; and leads to the formation of multiple stars. In the case of a single star per halo, they may still reach up to a thousand solar masses at z=25 (Hirano et al 2014), but feedback from the black hole itself shuts its own accretion and limits its growth (Johnson & Bromm 2007;Alvarez et al 2009). Perhaps, as suggested by Madau et al (2014), they may still grow under prolonged episodes of super-Eddington accretion.…”

Section: Introductionmentioning

confidence: 99%

Assessing inflow rates in atomic cooling haloes: implications for direct collapse black holes

Latif

Volonteri

2015

Mon. Not. R. Astron. Soc.

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Supermassive black holes are not only common in the present-day galaxies, but billion solar masses black holes also powered z ≥ 6 quasars. One efficient way to form such black holes is the collapse of a massive primordial gas cloud into a so-called direct collapse black hole. The main requirement for this scenario is the presence of large accretion rates of ≥ 0.1 M ⊙ /yr to form a supermassive star. It is not yet clear how and under what conditions such accretion rates can be obtained. The prime aim of this work is to determine the mass accretion rates under non-isothermal collapse conditions. We perform high resolution cosmological simulations for three primordial halos of a few times 10 7 M ⊙ illuminated by an external UV flux, J 21 = 100 − 1000. We find that a rotationally supported structure of about parsec size is assembled, with an aspect ratio between 0.25−1 depending upon the thermodynamical properties. Rotational support, however, does not halt collapse, and mass inflow rates of ∼ 0.1 M ⊙ /yr can be obtained in the presence of even a moderate UV background flux of strength J 21 ≥ 100. To assess whether such large accretion rates can be maintained over longer time scales, we employed sink particles, confirming the persistence of accretion rates of ∼ 0.1 M ⊙ /yr. We propose that complete isothermal collapse and molecular hydrogen suppression may not always be necessary to form supermassive stars, precursors of black hole seeds. Sufficiently high inflow rates can be obtained for UV flux J 21 = 500 − 1000, at least for some cases. This value brings the estimate of the abundance of direct collapse black hole seeds closer to that high redshift quasars.

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ONE HUNDRED FIRST STARS: PROTOSTELLAR EVOLUTION AND THE FINAL MASSES

Cited by 564 publications

References 88 publications

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution

Assessing inflow rates in atomic cooling haloes: implications for direct collapse black holes

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