Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars

@article{Tominaga2007SupernovaNI,
  title={Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars},
  author={Nozomu Tominaga and Hideyuki Umeda and Ken’ichi Nomoto},
  journal={The Astrophysical Journal},
  year={2007},
  volume={660},
  pages={516 - 540}
}
We perform hydrodynamic and nucleosynthesis calculations of core-collapse supernovae (SNe) and hypernovae (HNe) of Population (Pop) III stars. We provide new yields for the main-sequence mass of MMS = 13-50 M☉ and the explosion energy of E = (1–40) × 1051 ergs to apply to chemical evolution studies. Our HN yields based on the mixing-fallback model of explosions reproduce the observed abundance patterns of extremely metal-poor (EMP) stars (-4 < [Fe/H] < -3), while those of very metal-poor (VMP… 
Supernova Nucleosynthesis in the early universe
Abstract The first metal enrichment in the universe was made by supernova (SN) explosions of population (Pop) III stars. The history of chemical evolution is recorded in abundance patterns of
EXPLOSIVE NUCLEOSYNTHESIS OF WEAK r-PROCESS ELEMENTS IN EXTREMELY METAL-POOR CORE-COLLAPSE SUPERNOVAE
There have been attempts to fit the abundance patterns of extremely metal-poor (EMP) stars with supernova (SN) nucleosynthesis models for the elements lighter than Zn. Observations have revealed the
ABUNDANCE PROFILING OF EXTREMELY METAL-POOR STARS AND SUPERNOVA PROPERTIES IN THE EARLY UNIVERSE
After the big bang nucleosynthesis, the first heavy element enrichment in the universe was made by a supernova (SN) explosion of a population (Pop) III star (Pop III SN). The abundance ratios of
Faint Population III supernovae as the origin of the most iron-poor stars
The most iron-poor stars in the Milky Way provide important observational clues to the astrophysical objects that enriched the primordial gas with heavy elements. Among them, the recently discovered
NUCLEOSYNTHESIS IN HIGH-ENTROPY HOT BUBBLES OF SUPERNOVAE AND ABUNDANCE PATTERNS OF EXTREMELY METAL-POOR STARS
There have been suggestions that the abundance of extremely metal-poor (EMP) stars can be reproduced by hypernovae (HNe), not by normal supernovae (SNe). However, recently it was also suggested that
The Initial Mass Function of the First Stars Inferred from Extremely Metal-poor Stars
We compare the elemental abundance patterns of ∼200 extremely metal-poor (EMP; [Fe/H] < −3) stars to the supernova yields of metal-free stars, in order to obtain insights into the characteristic
NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS
The evolution and explosion of metal-free stars with masses 10–100 M☉ are followed, and their nucleosynthetic yields, light curves, and remnant masses determined. Such stars would have been the first
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS
We examine nucleosynthesis in the electron capture supernovae of progenitor asymptotic giant branch stars with an O–Ne–Mg core (with the initial stellar mass of 8.8 M☉). Thermodynamic trajectories
THE NUCLEOSYNTHETIC IMPRINT OF 15–40 M☉ PRIMORDIAL SUPERNOVAE ON METAL-POOR STARS
The inclusion of rotationally induced mixing in stellar evolution can alter the structure and composition of pre-supernova stars. We survey the effects of progenitor rotation on nucleosynthetic
ν-Process Nucleosynthesis in Population III Core-Collapse Supernovae
We investigate the effects of neutrino-nucleus interactions (the ν-process) on the production of iron-peak elements in Population III core-collapse supernovae. The ν-process and the following proton
...
...

References

SHOWING 1-10 OF 122 REFERENCES
Variations in the Abundance Pattern of Extremely Metal-Poor Stars and Nucleosynthesis in Population III Supernovae
We calculate nucleosynthesis in Population III supernovae (SNe) and compare the yields with various abundance patterns of extremely metal-poor (EMP) stars. We assume that the observed EMP stars are
Nucleosynthesis in Type II supernovae and the abundances in metal-poor stars
We explore the effects on nucleosynthesis in Type II supernovae of various parameters (mass cut, neutron excess, explosion energy, progenitor mass) in order to explain the observed trends of the
Fossil Imprints of the First-Generation Supernova Ejecta in Extremely Metal-deficient Stars
Using the results of nucleosynthesis calculations for theoretical core-collapse supernova models with various progenitor masses, it is shown that the abundance patterns of C, Mg, Si, Ca, and H that
Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars
We calculate nucleosynthesis in core collapse explosions of massive Population III stars and compare the results with abundances of metal-poor halo stars to constrain the parameters of Population III
Bipolar Supernova Explosions: Nucleosynthesis and Implications for Abundances in Extremely Metal-Poor Stars
Hydrodynamics and explosive nucleosynthesis in bipolar supernova explosions are examined to account for some peculiar properties of hypernovae as well as peculiar abundance patterns of metal-poor
The Explosive Yields Produced by the First Generation of Core Collapse Supernovae and the Chemical Composition of Extremely Metal Poor Stars
We present a detailed comparison of an extended set of elemental abundances observed in some of the most metal poor stars presently known and the ejecta produced by a generation of primordial core
Barium Abundances in Extremely Metal-poor Stars
New, improved, barium abundances for 33 extremely metal-poor halo stars from the 1995 sample of McWilliam et al. have been computed. The mean [Ba/Eu] ratio for stars with [Fe/H] ≤ -2.4 is -0.69 ±
Peculiar Chemical Abundances in the Starburst Galaxy M82 and Hypernova Nucleosynthesis
X-ray observations have shown that the chemical abundance in the starburst galaxy M82 is quite rich in Si and S compared to oxygen. Such an abundance pattern cannot be explained with any combination
First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star
TLDR
It is inferred that the first-generation supernovae came mostly from explosions of ∼20–130 M[circdot] stars; some of these produced iron-poor but carbon- and oxygen-rich ejecta, and low-mass second-generation stars, like HE0107–5240, could form because the carbon and oxygen provided pathways for the gas to cool.
...
...