Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars

By H. Umeda, Ken'ichi Nomoto. 2001

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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 supernovae. We focus on iron peak elements, and, in particular, we try to reproduce the large [Zn/Fe] observed in extremely metal-poor stars. The interesting trends of the observed ratios [Zn, Co, Mn, Cr, V/Fe] can be related to the variation of the relative mass of the complete and incomplete Si-burning regions in supernova ejecta. We find that [Zn/Fe] is larger for deeper mass cuts, smaller neutron excess, and larger explosion energies. The large [Zn/Fe] and [O/Fe] observed in the very metal-poor halo stars suggest deep mixing of complete Si-burning material and a significant amount of fallback in Type II supernovae. Furthermore, large explosion energies (E51 ≳ 2 for M ~ 13 M☉ and E51 ≳ 20 for M ≳ 20 M☉) are required to reproduce [Zn/Fe] ~ 0.5. The observed trends of the abundance ratios among the iron peak elements are better explained with this high-energy ("hypernova") model than with the simple "deep" mass cut effect because the overabundance of Ni can be avoided in the hypernova models. We also present the yields of pair instability supernova explosions of M ≃ 130-300 M☉ stars and discuss that the abundance features of very metal-poor stars cannot be explained by pair instability supernovae.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/646e9de9d6239eb9bcc5eb41f9d7a4e1764d146f

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Citations in the corpus

NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “In fact, all the previous models of supernova nucleosynthesis (with typical explosion energy), except for hypernovae (Umeda & Nomoto 2002), have failed to explain the solar inventory of 64Zn (which is the most abundant isotope of this element).”
HE 0107–5240, a Chemically Ancient Star. I. A Detailed Abundance Analysis (2003, methodology): “The yields of massive Population III pair-instability SNe (i.e., hypernovae) computed by Heger & Woosley (2002) or Umeda & Nomoto (2002) also offer rather good fits to our observed abundances.”
Abundances In Very Metal-Poor Dwarf Stars (2004, background): “The bulk of the production of Type II SN is α-elements; the production of Mn, Co and Cu is relatively small and, at least as modeled by Umeda & Nomoto (2002) and Umeda & Nomoto (2004), much more subject to variation given small changes in the characteristics of the the progenitor star or the SN…”
PAIR INSTABILITY SUPERNOVAE: LIGHT CURVES, SPECTRA, AND SHOCK BREAKOUT (2011, background): “But stars with initial masses between ∼ 140 and 260 M⊙ fall prey to the pair-production instability and explode completely (Barkat et al. 1967; Rakavy et al. 1967; Bond et al. 1984; Umeda & Nomoto 2002; Heger & Woosley 2002; Waldman 2008; Moriya et al. 2010; Fryer et al. 2010).”
The Evolution of the C/O Ratio in Metal-poor Halo Stars (2003, background): “However, their masses and chemical yields are still a matter of considerable speculation (e.g. Woosley & Weaver 1995; Heger & Woosley 2002; Chieffi & Limongi 2002; Limongi & Chieffi 2002; Umeda & Nomoto 2002).”
The Helium Abundances of ω Centauri (2004, methodology): “The stellar model calculations of Maeder (1992), Meynet & Maeder (2002), Timmes et al. (1995), Umeda & Nomoto (2002), and van den Hoek & Groenewegen (1997), for example, suggest that one must look to massive, as opposed to intermediate-mass, objects as the source.”
METALLICITY EVOLUTION OF DAMPED Lyα SYSTEMS OUT TO z ∼ 5 (2012, background): “While Zn is often observed to track Fe, theoretical work on the nucleosynthesis of Zn often predicts it may originate in massive stars (Woosley & Weaver 1995; Hoffman et al. 1996; Umeda & Nomoto 2002; Fenner et al. 2004).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, methodology): “For HNe, the final yields are obtained by adjusting the free parameters involved in the ‘mixing and fallback’ mechanism (Umeda & Nomoto 2002) to give [O/Fe]≃ 0.5 in the ejecta, as observed in extremely metal-poor stars.”
THE MASS SPECTRUM OF THE FIRST STARS (2014, methodology): “…signature of a pair-instability supernova (PISN) yielding a peculiar abundance pattern has been found in the metal-poor stars (Heger & Woosley 2002; Umeda & Nomoto 2002) and the abundance patterns of the metal-poor stars are well reproduced by supernova explosions of first stars as massive as the…”
The most metal-poor damped Lyα systems: insights into chemical evolution in the very metal-poor regime★ (2011, background): “These stars explode as PISN, the physics of which is well-understood (Heger & Woosley 2002; Umeda & Nomoto 2002).”
Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae (2003, methodology): “Also, in the metal-free universe very massive stars, with mass ranging from 140 to 260 M , evolve stably and explode as PISNe, in which a star is completely disrupted by a nuclearpowered explosion (Umeda & Nomoto 2002; Heger & Woosley 2002).”