Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis in honor of David L. Lambert

By T. Barnes, F. Bash. 2005

599 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/287b7a561db8d507d8f754518f98bdb27e17f723

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Citations in the corpus

Nucleosynthesis and remnants in massive stars of solar metallicity (2007, background): “Recent revisions to the solar abundance set have been discussed by9 Lodders (2003) and Asplund et al. (2004).”
Rotational mixing in massive binaries - Detached short-period systems (2009, methodology): “For the remaining heavy elements we adopt solar abundances by Asplund et al. (2005) scaled down by 0.7 dex for the SMC and 0.4 dex for the LMC.”
The properties of satellite galaxies in simulations of galaxy formation (2009, background): “7, we show the oxygen- 8 Assuming the more recent values for the solar abundances given by Asplund et al. (2005) increases [Fe/H] in the simulations only by ∼ 0.16.”
Solar fusion cross sections II: the pp chain and CNO cycles (2010, background): “However, this work also reduced metallicity estimates from Z ∼ 0.0169 to ∼ 0.0122 (Asplund et al., 2005), destroying the once excellent agreement between helioseismology and the SSM.”
NEW SOLAR COMPOSITION: THE PROBLEM WITH SOLAR MODELS REVISITED (2009, unknown): “26 68 v2 [ Subject headings: Sun: helioseismology - Sun: interior - Sun: abundances - neutrinos”
The MAPPINGS III Library of Fast Radiative Shock Models (2008, methodology): “…solar and twice solar as used by DS96 and which are based on the older Anders & Grevesse (1989) abundance set; a solar abundance set based on the Asplund et al. (2005) abundances as listed in Dopita et al. (2005), which is referred to here as the ‘‘dopita2005’’ abundances; and an LMC and an SMC…”
C, N, O abundances in the most metal-poor damped Lyman alpha systems★ (2007, methodology): “…as in Figure 9.10 When the oxygen abundance is greater than about half solar, that is when log (O/H) + 12 >∼ 8.3 adopting log (O/H)⊙ + 12 = 8.66 from Asplund et al. (2005), N/O rises steeply with increasing O/H; this is the regime where N is predomi- 10 See Pettini et al. (2002a) for the sources…”
s-process production in rotating massive stars at solar and low metallicities (2015, methodology): “(i) We used for our models with solar-like composition the initial chemical composition from Asplund et al. (2005) with a metallicity Z = 0.014.”
Turbulent Mixing and the Dead Zone in Protostellar Disks (2006, background): “The composition of the material is solar (Asplund et al. 2005), with 0.085 helium and 3:39 ; 10 5 magnesium atoms per hydrogen nucleus.”
The Structure of the Local Interstellar Medium. V. Electron Densities (2007, unknown): “We present two errors based on this calculation: the first simply propagates the error in N(SII), while the second includes the errors in the solar abundances (Asplund et al. 2005) and the natural variation of depletions (Jenkins 2004).”
A census of metals and baryons in stars in the local universe (2007, background): “However, we cannot robustly assess that the gas-phase metallicity is indeed higher than the stellar one, because of uncertainties in the solar oxygen abundance scale (Asplund et al. 2005), and a potential systematic overestimate introduced by strong-line metallicity indicators (e.”