Solar System Abundances and Condensation Temperatures of the Elements

By K. Lodders. 2003

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Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/a5c333a7fbca00121d9221c107d2a82d3b582b71

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Citations in the corpus

THE REMARKABLE DEATHS OF 9–11 SOLAR MASS STARS (2015, methodology): “The solar abundance set employed was from Lodders (2003) with X = 0.711, Y = 0.274, and metallicity, Z = 0.015.”
Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets (2007, methodology): “However, in lower mass objects, the HDO and CH3D opacities 5 See http://www.astro.ku.dk/ aborysow/. must be included and these were calculated using D/H ¼ 1:94 ; 10 5 (Lodders 2003).”
INVESTIGATING THE COSMIC-RAY IONIZATION RATE IN THE GALACTIC DIFFUSE INTERSTELLAR MEDIUM THROUGH OBSERVATIONS OF H+3 (2011, background): “Oxygen abundances are typically about two times carbon abundances (Lodders 2003), such that half of all O is expected to be in the form of CO.”
Atmosphere, Interior, and Evolution of the Metal-rich Transiting Planet HD 149026b (2005, methodology): “We use the elemental abundance data of Lodders (2003) and compute chemical equilibrium compositions with the CONDOR code, following Fegley & Lodders (1994), Lodders & Fegley (2002), and Lodders (2002).”
Improved Laboratory Transition Probabilities for Nd II and Application to the Neodymium Abundances of the Sun and Three Metal-poor Stars (2003, methodology): “…reviews of solar system abundances (e.g., Anders & Grevesse 1989; Grevesse & Noels 1993; Grevesse, Noels, & Sauval 1996; Grevesse & Sauval 1998, 2002; Lodders 2003) suggest that among the rare earth elements, Nd, Tb, Ho, Tm, Yb, and Lu have large photospheric abundance uncertainties ( 0.10 dex).”
Equilibrium chemistry down to 100 K (2017, background): “…constants based on partition functions (Allard & Hauschildt 1995; Gustafsson et al. 2008; Barklem & Collet 2016; Van Eck et al. 2017), and (iii) minimisation of the system Gibbs free energy (Lodders 2003; Ackerman & Marley 2001; Miller-Ricci et al. 2009; Mbarek & Kempton 2016; Blecic et al. 2016).”
s‐Process in low‐metallicity stars – I. Theoretical predictions (2010, background): “The initial isotopic composition of the other isotopes is based on the solar meteoritic values of Anders & Grevesse (1989), except for C, N and O isotopes, which are upgraded to that of Lodders (2003).”
Near-Infrared Spectroscopy of Charon: Possible Evidence for Cryovolcanism on Kuiper Belt Objects (2006, background): “The equilibrium condensate from solar nebula gas is ADH (Lodders 2003), so Charon is not expected to possess AHH at its creation.”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “The accreted material has solar-like composition X = 0.70, Y = 0.26, and Z = 0.04 where the metal mass fractions are taken from Lodders (2003).”
Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars. II. Sulfur and Phosphorus (2005, methodology): “All calculations were done with solar system (i.e., protosolar) elemental abundances from Lodders (2003).”
Chondrules and the Protoplanetary Disk (2011, background): “Condensation calculations for trace elements are summarized by Lodders (2003).”
Semi‐empirical analysis of Sloan Digital Sky Survey galaxies – III. How to distinguish AGN hosts (2006, background): “(4) Note that these abundance ratios are different from the solar ones as compiled by Lodders (2003).”
The composition of Mars (2019, methodology): “Figure 6: Abundance of lithophile (purple), siderophile (pink) and chalcophile (blue) elements in the bulk silicate Mars (Table 5) are normalized to CI chondrites (Table 2) and plotted against log of the 50% condensation temperature (K) at 10 Pa (Lodders, 2003).”
Three-dimensional delayed-detonation models with nucleosynthesis for Type Ia supernovae (2012, methodology): “For the solar composition we use Lodders (2003).”
Abundance, distribution, and origin of 60Fe in the solar protoplanetary disk (2012, background): “2.25±0.65 M . The total mass of ISM gas in the Galaxy is 4.95109 M (Robin et al., 2003). The mass fractions of 27Al and 56Fe in the protosolar nebula are X(27Al)=6.2610-5 and X(56Fe)=1.1910-3 (Lodders 2003). These fractions represent snapshots of the ISM composition 4.5 Ga. Models of the chemical ”
Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos (2005, background): “…ið Þ X ; i : ð1Þ In this equation, the sum is over all trajectories, Xj(i) is the mass fraction of nuclide i in the jth trajectory, X ; i is the mass fraction of nuclide i in the Sun (Lodders 2003), Mj is the mass of the jth trajectory, andM ej ¼ 13:5M is the total mass ejected in the SN explosion.”
10,000 Standard Solar Models: A Monte Carlo Simulation (2005, methodology): “In recent years, determinations of the solar abundances of heavy elements have become more refined and detailed (Lodders 2003 and especially Asplund 2000; Asplund et al. 2000; Allende Prieto et al. 2001, 2002; Asplund et al. 2004, 2005).”