Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution

By Ken'ichi Nomoto, Nozomu Tominaga, H. Umeda, C. Kobayashi, K. Maeda. 2006

544 citations recorded by the source corpus.

Abstract We present new nucleosynthesis yields as functions of the stellar mass, metallicity, and explosion energy (corresponding to normal supernovae and hypernovae). We apply the results to the chemical evolution of the solar neighborhood. Our new yields are based on the new developments in the observational/theoretical studies of supernovae (SNe) and extremely metal-poor (EMP) stars in the halo, which have provided excellent opportunities to test the explosion models and their nucleosynthesis. We use the light curve and spectra fitting of individual SN to estimate the mass of the progenitor, explosion energy, and produced 56Ni mass. Comparison with the abundance patterns of EMP stars has made it possible to determine the model parameters of core-collapse SNe, such as mixing-fallback parameters. More specifically, we take into account the two distinct new classes of massive SNe: (1) very energetic hypernovae, whose kinetic energy (KE) is more than 10 times the KE of normal core-collapse SNe, and (2) very faint and low energy SNe (faint SNe). These two new classes of SNe are likely to be “black-hole-forming” SNe with rotating or non-rotating black holes. Nucleosynthesis in hypernovae is characterized by larger abundance ratios ( Zn , Co , V , Ti ) / Fe and smaller ( Mn , Cr ) / Fe than normal SNe, which can explain the observed trends of these ratios in EMP stars. Nucleosynthesis in faint SNe is characterized by a large amount of fall-back, which explains the abundance pattern of the most Fe-poor stars. These comparisons suggest that black-hole-forming SNe made important contributions to the early galactic (and cosmic) chemical evolution.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/32ef3733ca11e8ac805dedfbf3012e04541c3883

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Citations in the corpus

Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, methodology): “We used the mass- and metallicity-dependent yields (YX) by K06 (see also Nomoto et al. 2006), who provide yields for normal SN II as well as hypernovae.”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “Here our goal is simply to provide an estimate of the explosive contribution to stellar yields, including a general understanding on how pre-explosive abundances are modified by the explosion (e.g., Woosley & Weaver 1995; Limongi et al. 2000; Rauscher et al. 2002; Nomoto et al. 2006).”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, methodology): “…if the standard deviation of the metallicity dependence |dMZ(species)/dZprogenitor| between the models of Chieffi & Limongi (2004), Woosley & Weaver (1995), and Nomoto et al. (2006) is larger than the magnitude of the actual predicted trend |dMZ(species)/dZprogenitor| from Nomoto et al. 2006.”
Progenitors of Core-Collapse Supernovae (2009, background): “The interpretation of Nomoto et al. (2006), Zampieri et al. (2003) and Pastorello et al. (2004) is that they are initially high mass stars which result in faint explosions (see Figure 11a).”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS IN THE LEAST EVOLVED GALAXIES: URSA MAJOR II and COMA BERENICES (2009, result): “This agrees with findings by Nomoto et al. (2006), who explained the abundances of the Cayrel et al. (2004) stars with their hypernova models.”
Nebular Emission Line Ratios in z ≃ 2–3 Star-forming Galaxies with KBSS-MOSFIRE: Exploring the Impact of Ionization, Excitation, and Nitrogen-to-Oxygen Ratio (2016, background): “…S16, this means that since Z∗ effectively traces the Fe abundance in stars, a combination of low Z∗ and moderate Zneb in high-z galaxies does not require the stellar O/H to differ from O/H in the gas—because O/Fe may be enhanced relative to (O/Fe)⊙ by up to a factor of ∼ 5.5 (Nomoto et al. 2006).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “Our result confirms that electron capture supernovae produce very little 56Ni (≈ 0.002 − 0.004 M⊙, Table 1) compared to ∼ 0.1 M⊙ in the case of more massive progenitors (e.g., Nomoto et al. 2006).”
The birth of a galaxy – III. Propelling reionization with the faintest galaxies (2014, methodology): “The SN explosion energies and metal ejecta masses from Nomoto et al. (2006) and Heger et al. (2003) are used for Type II (20–40 M ) and pair instability SNe (140–260 M ), respectively.”
The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “As a result, it is found that many core-collapse supernovae (M > 20M⊙) have an explosion energy that is more than 10 times that of a regular supernova (E51 >∼ 10, Nomoto et al. 2006), as well as producing more iron and α elements (O, Mg, Si, S, Ca, and Ti).”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, methodology): “In our model we have calculated the evolution of 63 isotopes using nucleosynthesis prescription of Nomoto et al. (2006) and, for comparison, that of Woosley & Weaver (1995).”
The Evolution of Dust in the Early Universe with Applications to the Galaxy SDSS J1148+5251 (2007, background): “If all the refractory elements precipitate with a 100% efficiency from the gas, a typical 25 M⊙ SN can form about 1 M⊙ of dust (Woosley & Weaver 1995; Nomoto et al. 2006).”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, background): “The eject d mass fraction is insensitive to metallicity. yields (e.g., Maeder 1992; Woosley & Weaver 1995; Portinariet al. 1998; Rauscher et al. 2002; Hirschi et al. 2005; Nomoto et al. 2006).”
A COOL DUST FACTORY IN THE CRAB NEBULA: A HERSCHEL STUDY OF THE FILAMENTS (2012, methodology): “The total amount of heavy elements (and therefore the mass available to form dust) in the SN ejecta from a 9–12M⊙ progenitor star varies from 0.2 to 0.5M⊙ depending on the model used and the mass of the progenitor (Maeder 1992; Woosley & Weaver 1995; Limongi & Chieffi 2003; Nomoto et al. 2006).”
Feedback-regulated star formation and escape of LyC photons from mini-haloes during reionization (2016, methodology): “≤ 40 M (Nomoto et al. 2006).”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, methodology): “Several groups have provided recent versions of nucleosynthesis yields for core-collapse supernovae and hypernovae (e.g., Limongi & Chieffi 2006, 2012; Nomoto et al. 2006; Tominaga, Umeda & Nomoto 2007; Heger & Woosley 2010).”
Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, methodology): “Here we discuss the differences in the tracks of magnesium and oxygen using Nomoto et al. (2006) SNII yields and Iwamoto et al. (1999) SNIa yields.”