scholarly journals The Persistence of Population III Star Formation

2018 ◽  
Vol 479 (4) ◽  
pp. 4544-4559 ◽  
Author(s):  
Richard H Mebane ◽  
Jordan Mirocha ◽  
Steven R Furlanetto
Keyword(s):  
Star Formation ◽  
Population Iii

scholarly journals Effect of Population III multiplicity on dark star formation

2012 ◽  
pp. no-no ◽  
Author(s):  
Athena Stacy ◽  
Andreas H. Pawlik ◽  
Volker Bromm ◽  
Abraham Loeb
Keyword(s):  
Star Formation ◽  
Population Iii

scholarly journals When did Population III star formation end?

2020 ◽  
Vol 497 (3) ◽  
pp. 2839-2854 ◽  
Author(s):  
Boyuan Liu ◽  
Volker Bromm
Keyword(s):  
Star Formation ◽  
Direct Detection ◽  
Analytical Models ◽  
Space Telescopes ◽  
Detection Rates ◽  
Metal Free ◽  
Detection And Identification ◽  
Future Space ◽  
Study Population ◽  
Population Iii

ABSTRACT We construct a theoretical framework to study Population III (Pop III) star formation in the post-reionization epoch (z ≲ 6) by combining cosmological simulation data with semi-analytical models. We find that due to radiative feedback (i.e. Lyman–Werner and ionizing radiation) massive haloes ($M_{\rm halo}\gtrsim 10^{9}\ \rm M_{\odot }$) are the major (≳90 per cent) hosts for potential Pop III star formation at z ≲ 6, where dense pockets of metal-poor gas may survive to form Pop III stars, under inefficient mixing of metals released by supernovae. Metal mixing is the key process that determines not only when Pop III star formation ends, but also the total mass, MPopIII, of active Pop III stars per host halo, which is a crucial parameter for direct detection and identification of Pop III hosts. Both aspects are still uncertain due to our limited knowledge of metal mixing during structure formation. Current predictions range from early termination at the end of reionization (z ∼ 5) to continuous Pop III star formation extended to z = 0 at a non-negligible rate $\sim \!10^{-7}\ \rm M_{\odot }\ yr^{-1}\ Mpc^{-3}$, with $M_{\rm PopIII}\sim 10^{3}-10^{6}\ \rm M_{\odot }$. This leads to a broad range of redshift limits for direct detection of Pop III hosts, zPopIII ∼ 0.5–12.5, with detection rates $\lesssim 0.1-20\ \rm arcmin^{-2}$, for current and future space telescopes (e.g. HST, WFIRST, and JWST). Our model also predicts that the majority (≳90 per cent) of the cosmic volume is occupied by metal-free gas. Measuring the volume-filling fractions of this metal-free phase can constrain metal-mixing parameters and Pop III star formation.

scholarly journals The effects of population III radiation backgrounds on the cosmological 21-cm signal

2020 ◽  
Vol 493 (1) ◽  
pp. 1217-1226 ◽  
Author(s):  
Richard H Mebane ◽  
Jordan Mirocha ◽  
Steven R Furlanetto
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Radio Emission ◽  
Formation Rate ◽  
Fine Tuning ◽  
Absorption Feature ◽  
Simulation Code ◽  
X Ray ◽  
Neutral Gas ◽  
Population Iii

ABSTRACT We investigate the effects of Population III (Pop III) stars and their remnants on the cosmological 21-cm global signal. By combining a semi-analytic model of Pop III star formation with a global 21-cm simulation code, we investigate how X-ray and radio emission from accreting Pop III black holes may affect both the timing and depth of the 21-cm absorption feature that follows the initial onset of star formation during the Cosmic Dawn. We compare our results to the findings of the EDGES experiment, which has reported the first detection of a cosmic 21-cm signal. In general, we find that our fiducial Pop III models, which have peak star formation rate densities of ∼10−4 M⊙ yr−1 Mpc−3 between z ∼ 10 and z ∼ 15, are able to match the timing of the EDGES signal quite well, in contrast to models that ignore Pop III stars. To match the unexpectedly large depth of the EDGES signal without recourse to exotic physics, we vary the parameters of emission from accreting black holes (formed as Pop III remnants) including the intrinsic strength of X-ray and radio emission as well as the local column density of neutral gas. We find that models with strong radio emission and relatively weak X-ray emission can self-consistently match the EDGES signal, though this solution requires fine-tuning. We are only able to produce signals with sharp features similar to the EDGES signal if the Pop III IMF is peaked narrowly around $140 \, \mathrm{M}_\odot$.

scholarly journals Magnetohydrodynamics of Population III Star Formation

2010 ◽  
Author(s):  
Masahiro N. Machida ◽  
Kazuyuki Omukai ◽  
Tomoaki Matsumoto ◽  
Daniel J. Whalen ◽  
Volker Bromm ◽  
...  
Keyword(s):  
Star Formation ◽  
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.

scholarly journals CONFINED POPULATION III ENRICHMENT AND THE PROSPECTS FOR PROMPT SECOND-GENERATION STAR FORMATION

2012 ◽  
Vol 761 (1) ◽  
pp. 56 ◽  
Author(s):  
Jeremy S. Ritter ◽  
Chalence Safranek-Shrader ◽  
Orly Gnat ◽  
Miloš Milosavljević ◽  
Volker Bromm
Keyword(s):  
Star Formation ◽  
Second Generation ◽  
Population Iii

scholarly journals MAGNETIC FIELDS IN POPULATION III STAR FORMATION

2012 ◽  
Vol 745 (2) ◽  
pp. 154 ◽  
Author(s):  
Matthew J. Turk ◽  
Jeffrey S. Oishi ◽  
Tom Abel ◽  
Greg L. Bryan
Keyword(s):  
Star Formation ◽  
Magnetic Fields ◽  
Population Iii

scholarly journals Dark-matter halo mergers as a fertile environment for low-mass Population III star formation

2014 ◽  
Vol 441 (3) ◽  
pp. 2181-2187 ◽  
Author(s):  
S. Bovino ◽  
M. A. Latif ◽  
T. Grassi ◽  
D. R. G. Schleicher
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Dark Matter Halo ◽  
Low Mass ◽  
Population Iii
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