Galactic Chemical Evolution: Carbon through Zinc

By C. Kobayashi, H. Umeda, Ken'ichi Nomoto, Nozomu Tominaga, T. Ohkubo. 2006

609 citations recorded by the source corpus.

We calculate the evolution of heavy-element abundances from C to Zn in the solar neighborhood, adopting our new nucleosynthesis yields. Our yields are calculated for wide ranges of metallicity (Z = 0-Z☉) and the explosion energy (normal supernovae and hypernovae), based on the light-curve and spectra fitting of individual supernovae. The elemental abundance ratios are in good agreement with observations. Among the α-elements, O, Mg, Si, S, and Ca show a plateau at [Fe/H] ≲ -1, while Ti is underabundant overall. The observed abundance of Zn ([Zn/Fe] ~ 0) can be explained only by the high-energy explosion models, as it requires a large contribution of hypernovae. The observed decrease in the odd-Z elements (Na, Al, and Cu) toward low [Fe/H] is reproduced by the metallicity effect on nucleosynthesis. The iron-peak elements (Cr, Mn, Co, and Ni) are consistent with the observed mean values at -2.5 ≲ [Fe/H] ≲ -1, and the observed trend at the lower metallicity can be explained by the energy effect. We also show the abundance ratios and the metallicity distribution functions of the Galactic bulge, halo, and thick disk. Our results suggest that the formation timescale of the thick disk is ~1-3 Gyr.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fe10e57a7e6c9c8bc8e27da73f552b053a654e25

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Citations in the corpus

The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “Kobayashi et al. (2006) presented the nucleosynthesis yields of SNe II and HNe as a function of the progenitor mass (M = 13, 15, 18, 20, 25, 30, and 40M⊙) and metallicity (Z = 0, 0.001, 0.004, and 0.02).”
Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals (2015, background): “We note that although we assumed the oxygen yield as constant, the oxygen yield varies with both the stellar metallicity and initial mass function (e.g.,Maeder 1992; Woosley & Weaver 1995; Kobayashi et al. 2006; seeZahid et al. 2012for a summary).”
Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, background): “Oxygen production seems to be favored at low metallicities (e.g., Kobayashi et al. 2006).”
Simulating galaxy formation with the IllustrisTNG model (2017, methodology): “For the mass range 13 − 40 M , we use yields from Kobayashi et al. (2006).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, methodology): “Models 1 and 5, adopting the yields of Woosley & Weaver (1995) case B and Kobayashi et al. (2006) withε = 1 for massive stars, respectively, favour a nearly flat trend of [S/Fe] versus [Fe/H] in the metallicity regime−3 < [Fe/H] < −1.”
THE MOST METAL-POOR STARS. II. CHEMICAL ABUNDANCES OF 190 METAL-POOR STARS INCLUDING 10 NEW STARS WITH [Fe/H] ⩽ −3.5,, (2012, methodology): “As reported in other investigations (e.g., Kobayashi et al. 2006), the predictions for Ti and Sc are underabundant relative to the LTE measurements.”
THE CHEMICAL EVOLUTION OF THE DRACO DWARF SPHEROIDAL GALAXY (2009, methodology): “…dSph Galaxy Recent models of chemical evolution for the disk, bulge, and halo of the Milky Way based on the precepts first established by Tinsley (1973) have been presented by several groups, including Timmes, Woosley & Weaver (1995), Kobayashi et al (2006), Prantzos (2008), and Matteucci (2008).”
Using chemical tagging to redefine the interface of the Galactic disc and halo (2015, background): “However, according to Kobayashi et al. (2006), the production of those elements are strongly dependent on the initial C and N in the gas cloud that forms the stars.”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “Despite significant progress, details regarding the chemical evolution of the Galaxy remain poorly understood (e.g., Tinsley 1980; Timmes et al. 1995; Goswami & Prantzos 2000; Travaglio et al. 2004; Gibson et al. 2006; Kobayashi et al. 2006).”
s-process production in rotating massive stars at solar and low metallicities (2015, methodology): “The values for the noble gases were adopted from the GCE models of Kobayashi et al. (2006).”
Metallicity gradients in disks - Do galaxies form inside-out? (2012, background): “The chemical evolution implementation within GCD+ takes into account the metal-dependent nucleosynthetic byproducts of SNeII (Woosley & Weaver 1995), SNeIa (Iwamoto et al. 1999), and low- and intermediate-mass AGB stars (van den Hoek & Groenewegen 1997).”
NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS (2008, background): “Note that simply increasing the explosion energy is not a good solution for the cobalt underproduction (Kobayashi et al. 2006).”
Europium production: neutron star mergers versus core-collapse supernovae (2013, positive): “In particular, Cescutti et al. (2006) adoptedthe Fe yields of Woosley & Weaver (1995) for solar metallicity, whereas here we adopt the more recent yields depending on metallicity by Kobayashi et al. (2006).”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “…interstellar medium (Truran & Cameron 1971; Tinsley 1980; Matteucci & Greggio 1986; Lambert 1989; Wheeler et al. 1989; Timmes et al. 1995; Goswami & Prantzos 2000; Gibson et al. 2003; Kobayashi et al. 2006; Krumholz et al. 2007; Prantzos 2008; Romano et al. 2010; Kobayashi & Nakasato 2011).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “We adopt the Salpeter IMF that is invariant to time and metallicity with a slope x = 1.35 for 0.1–120 M , to be consistent with the Galactic chemical evolution (Kobayashi et al. 2006).”
THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, background): “Y does not depend strongly on any galaxy properties (Thomas et al. 1998; Kobayashi et al. 2006).”
Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, background): “This is consistent with the chemical evolution models in Ishimaru&Wanajo (1999), Argast et al. (2000), Tumlinson (2006), Nomoto et al. (2006), and Kobayashi et al. (2006).”
First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium (2017, methodology): “…ejected by SNIa, SNII and stellar winds have been updated such that the abundances of the 9 explicitly tracked elements more closely follow the ratios found in the Milky Way (Nomoto et al. 1997; Portinari et al. 1998; Kobayashi et al. 2006; Karakas 2010; Doherty et al. 2014; Fishlock et al. 2014).”