Solar System Abundances of the Elements

By K. Lodders. 2010

516 citations recorded by the source corpus.

Representative abundances of the chemical elements for use as a solar abundance standard in astronomical and planetary studies are summarized. Updated abundance tables for solar system abundances based on meteorites and photospheric measurements are presented.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/688c2b0584be429403f4dab0d3d42d87abbed4f3

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Citations in the corpus

Astrochemistry and compositions of planetary systems (2020, background): “The water vapor needed for this model is typically assumed to originate from a complete reset of the chemistry in the hot (>2000 K) cooling nebula model that is suggested for numerous inner solar system solids (see, e.g., McDonough and Sun 1995; Lodders 2010).”
The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “Although the problem is still unsettled and different solutions are under scrutiny (see, e.g., Vinyoles et al. 2017), we decided to adopt the solar metal mixture by Caffau et al. (2011), supplemented when necessary by the abundances given by Lodders (2010).”
26Al‐26Mg isotope systematics of the first solids in the early solar system (2013, unknown): “…is expected to be approximately 0.038& lower than the value today, assuming homogeneous initial magnesium isotope ratios, homogeneous initial aluminum isotope ratios (26Al/27Al = 5.25 9 10 5), and a bulk solar system ratio of 27Al/24Mg = 0.101 as defined by CI chondrites (Palme and Jones 2003).”
A review of the structural architecture of tellurium oxycompounds (2016, background): “element with an atomic number >40, as measured by relative number of atoms in C1 chondrite (Anders and Ebihara, 1982). Nevertheless, Te is one of the rarest elements in the Earth’s crust (0.4‒ 10 ppb; Parker, 1967; Levinson, 1974; Govett, 1983;McDonough and Sun, 1995; Reimann and de Caritat, 1998) a”
The composition of Mars (2019, methodology): “are undifferentiated assemblage of metal and silicates (Scott and Krot, 2014). Chondritic meteorites, especially the CI carbonaceous chondrites, are chemically similar to the solar photosphere (e.g., Palme et al., 2014), which is taken to reﬂect the Sun’s abundances of non-gaseous elements. At >9”
Rubidium isotopic composition of the Earth, meteorites, and the Moon: Evidence for the origin of volatile loss during planetary accretion (2017, background): “The CI-type CC have elemental abundances that closely match the composition of the solar photosphere (excluding Li, H, C, N, O, and the noble gases; Palme et al., 2014).”
Sulphur-bearing species in the coma of comet 67P/Churyumov–Gerasimenko (2016, background): “If we neglect the minor sulphur-bearing species (e.g. organo-sulphur) and the minor oxygenated species (e.g. alcohols) in the coma, we can calculate the S/O ratio in the volatile material according to S/O = nH2S + nS + nOCS + 2 · nS2 + nSO2 + 2 · nCS2 + nSO nH2O · (1.0 + 2 · 0.038) + nCO + 2 · nCO2 ”
Reference Values Following ISO Guidelines for Frequently Requested Rock Reference Materials (2016, background): “Figure 5a shows the CI chondrite-normalised (Palme et al. 2014) REE mass fractions of RMs of different rock types with smooth patterns.”