One hundred first stars: Protostellar evolution and the final masses

Journal Article · Sat Feb 01 04:00:00 EST 2014 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/781/2/60· OSTI ID:22348143

Hirano, Shingo; Umeda, Hideyuki ^[1]; Hosokawa, Takashi ^[2]; Yoshida, Naoki; Chiaki, Gen ^[3]; Omukai, Kazuyuki ^[4]

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1. Department of Astronomy, School of Science, University of Tokyo, Bunkyo, Tokyo 113-0033 (Japan)
2. Department of Physics and Research Center for the Early Universe, University of Tokyo, Bunkyo, Tokyo 113-0033 (Japan)
3. Department of Physics, School of Science, University of Tokyo, Bunkyo, Tokyo 113-0033 (Japan)
4. Astronomical Institute, Tohoku University, Sendai, Miyagi 980-8578 (Japan)

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 M {sub popIII} = 10 ∼ 1000 M {sub ☉}. 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.

• OSTI ID: 22348143
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 781; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ACCRETION DISKS
BLACK HOLES
CORRELATIONS
FEEDBACK
INSTABILITY
MASS
MASS DISTRIBUTION
PROTOSTARS
SIMULATION
STAR EVOLUTION
SUPERNOVAE
SURFACES
UNIVERSE