scholarly journals The masses of Population III stars

1989 ◽  
Vol 239 (2) ◽  
pp. 371-380 ◽  
Author(s):  
J. C. N. de Araujo ◽  
R. Opher
Keyword(s):  
Population Iii Stars ◽  
The Masses ◽  
Population Iii

scholarly journals Formation sites of Population III star formation: The effects of different levels of rotation and turbulence on the fragmentation behaviour of primordial gas

2020 ◽  
Vol 494 (2) ◽  
pp. 1871-1893 ◽  
Author(s):  
Katharina M J Wollenberg ◽  
Simon C O Glover ◽  
Paul C Clark ◽  
Ralf S Klessen
Keyword(s):  
Star Formation ◽  
Initial Conditions ◽  
Turbulent Energy ◽  
Star Forming ◽  
Wide Range ◽  
Population Iii Stars ◽  
The Individual ◽  
The Masses ◽  
Different Levels ◽  
Population Iii

ABSTRACT We use the moving-mesh code arepo to investigate the effects of different levels of rotation and turbulence on the fragmentation of primordial gas and the formation of Population III stars. We consider nine different combinations of turbulence and rotation and carry out five different realizations of each setup, yielding one of the largest sets of simulations of Population III star formation ever performed. We find that fragmentation in Population III star-forming systems is a highly chaotic process and show that the outcomes of individual realizations of the same initial conditions often vary significantly. However, some general trends are apparent. Increasing the turbulent energy promotes fragmentation, while increasing the rotational energy inhibits fragmentation. Within the ∼1000 yr period that we simulate, runs including turbulence yield flat protostellar mass functions while purely rotational runs show a more top-heavy distribution. The masses of the individual protostars are distributed over a wide range from a few $10^{-3} \, {\rm M_{\odot }}$ to several tens of M⊙. The total mass growth rate of the stellar systems remains high throughout the simulations and depends only weakly on the degree of rotation and turbulence. Mergers between protostars are common, but predictions of the merger fraction are highly sensitive to the criterion used to decide whether two protostars should merge. Previous studies of Population III star formation have often considered only one realization per set of initial conditions. However, our results demonstrate that robust trends can only be reliably identified by considering averages over a larger sample of runs.

Long duration X-ray flash from low mass population III stars

2012 ◽  
Author(s):  
Daisuke Nakauchi ◽  
Yudai Suwa ◽  
Kazumi Kashiyama ◽  
Takashi Nakamura
Keyword(s):  
X Ray ◽  
Long Duration ◽  
Low Mass ◽  
Population Iii Stars ◽  
Population Iii

scholarly journals Unique signatures of Population III stars in the global 21-cm signal

2018 ◽  
Vol 478 (4) ◽  
pp. 5591-5606 ◽  
Author(s):  
Jordan Mirocha ◽  
Richard H Mebane ◽  
Steven R Furlanetto ◽  
Krishma Singal ◽  
Donald Trinh
Keyword(s):  
Population Iii Stars ◽  
Population Iii

Blocking metal accretion onto low-mass population III stars by stellar wind

2018 ◽  
Author(s):  
Shuta J. Tanaka ◽  
Gen Chiaki ◽  
Nozomu Tominaga ◽  
Hajime Susa
Keyword(s):  
Stellar Wind ◽  
Low Mass ◽  
Population Iii Stars ◽  
Population Iii

scholarly journals Imprint of Gravitational Lensing by Population III Stars in Gamma‐Ray Burst Light Curves

2006 ◽  
Vol 650 (1) ◽  
pp. 252-260 ◽  
Author(s):  
Y. Hirose ◽  
M. Umemura ◽  
A. Yonehara ◽  
J. Sato
Keyword(s):  
Gravitational Lensing ◽  
Gamma Ray ◽  
Light Curves ◽  
Gamma Ray Burst ◽  
Population Iii Stars ◽  
Population Iii
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