ONE HUNDRED FIRST STARS: PROTOSTELLAR EVOLUTION AND THE FINAL MASSES

By S. Hirano, T. Hosokawa, Naoki Yoshida, H. Umeda, K. Omukai, G. Chiaki, H. Yorke. 2013

352 citations recorded by the source corpus.

We perform a large set of radiation hydrodynamic simulations of primordial star formation in a fully cosmological context. Our statistical sample of 100 First Stars shows that the first generation of stars has a wide mass distribution MpopIII = 10 ∼ 1000 M☉. We first run cosmological simulations to generate a set of primordial star-forming gas clouds. We then follow protostar formation in each gas cloud and the subsequent protostellar evolution until the gas mass accretion onto the protostar is halted by stellar radiative feedback. The accretion rates differ significantly among the primordial gas clouds that largely determine the final stellar masses. For low accretion rates, the growth of a protostar is self-regulated by radiative feedback effects, and the final mass is limited to several tens of solar masses. At high accretion rates the protostar's outer envelope continues to expand, and the effective surface temperature remains low; such protostars do not exert strong radiative feedback and can grow in excess of 100 solar masses. The obtained wide mass range suggests that the first stars play a variety of roles in the early universe, by triggering both core-collapse supernovae and pair-instability supernovae as well as by leaving stellar mass black holes. We find certain correlations between the final stellar mass and the physical properties of the star-forming cloud. These correlations can be used to estimate the mass of the first star from the properties of the parent cloud or of the host halo without following the detailed protostellar evolution.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/93aecaa61860acf17e5677bde89d683ac6614949

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Citations in the corpus

• EVIDENCE FOR PopIII-LIKE STELLAR POPULATIONS IN THE MOST LUMINOUS Lyα EMITTERS AT THE EPOCH OF REIONIZATION: SPECTROSCOPIC CONFIRMATION (2015, background): “…to begin to sample the potential IMF of PopIII stars, finding a distribution which is very flat or top-heavy, with masses ranging from 10 to 1000 M (e.g. Hirano et al. 2014), although the PopIII IMF is extremely uncertain (e.g. Greif et al. 2011) and only observations will be able to constrain it.”
• THE MASS SPECTRUM OF THE FIRST STARS (2014, background): “Hirano et al. (2014) have shown that such a condition could also be satisfied even in the collapsing minihalos of 105–106 M .”
• Blossoms from black hole seeds: properties and early growth regulated by supernova feedback (2016, background): “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).”
• Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “Similarly, Hirano et al. (2014) find a reasonably flat distribution over the range of 10M⊙ to 1000M⊙, based on 100 first stars simulations.”
• Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes (2018, result): “Cosmological simulations for the formation of the first stars show that Pop III stars can also be very massive, M∗ ≈ 10–1 000M (Hosokawa et al. 2011; Hirano et al. 2014, 2015), a prediction that is consistent with the Pop III IMF constraints inferred with Milky Way halo stars (de Bennassuti et al.…”
• Early galaxy formation and its large-scale effects (2018, background): “We note that the Hirano et al 2014 minihaloes were studied in two dimensions and could not follow three-dimensional fragmentation. emit X-rays that could ionize more distant gas and influence more distant star formation as well as reionization (e.g. Jeon et al. 2012, 2014).”
• Rates of compact object coalescences (2021, background): “(2009); Tsang (2013); Hoang et al. (2020); Rasskazov and Kocsis (2019) explored direct gravitational-wave bremsstrahlung captures from 2-body scattering. Meanwhile, Bellovary et al. (2016); Bartos et al.”
• Building up the Population III initial mass function from cosmological initial conditions (2016, methodology): “Hirano et al. (2014) additionally include ionization feedback, but cannot follow three-dimensional fragmentation.”
• The birth of a galaxy – III. Propelling reionization with the faintest galaxies (2014, background): “However, a recent paper by Hirano et al. (2014) studied 100 instances of Pop III protostar evolution with axisymmetric radiation hydrodynamics simulations that were initialized from a cosmological simulation.”
• Observational evidence for intermediate-mass black holes (2017, background): “If H2 dominates the cooling rate, the primordial gas can cool down to ∼100 K and collapse into protostars (known as Pop III stars) of typically a few hundreds of solar masses (e.g., Bromm & Larson 2004) and up to ∼ 103 M (e.g., Hirano et al. 2014).”
• Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution (2015, background): “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.”
• Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave (2014, methodology): “We set the mass range of 10 M ≤ M1 ≤ 100 M to the mass of the primary star, as suggested by the recent numerical simulations (Hirano et al. 2014).”
• Formation of Supermassive Black Hole Seeds (2016, background): “Moreover, higher rotation decreases the mass accretion onto a protostar and consequently the final stellar mass gets reduced (Hirano et al. 2014; Dutta 2016).”
• Feedback-regulated star formation and escape of LyC photons from mini-haloes during reionization (2016, background): “…reducing the characteristic mass to ∼ 40 M (Turk et al. 2009; Greif et al. 2012) However, recent radiationhydrodynamics simulations report that several tens to a thousand solar masses of gas may collapse to form a Pop III star (Hirano et al. 2014; Hosokawa et al. 2015, c.f., Lee & Yoon 2016).”
• Hyper-Eddington accretion flows on to massive black holes (2015, background): “…of Population III (Pop III) stars with typical mass of ∼ 100 M⊙ (Yoshida, Omukai & Hernquist 2008; Hosokawa et al. 2011; Stacy, Greif & Bromm 2012; Hirano et al. 2014; Hosokawa et al. 2015), which grow up to SMBHs via continuous gas accretion or frequent ⋆ E-mail: inayoshi@astro.columbia.edu †…”