Interstellar Abundance Standards Revisited

By U. Sofia, D. Meyer. 2001

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View Paper: https://www.semanticscholar.org/paper/aa38e9f2e2570832f0a130072c65f11be5d5f243

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In Astronomy and Astrophysics

Citations in the corpus

Interstellar Carbon in Translucent Sight Lines (2004, background): “…models (Snow & Witt 1995, and references within), but can be alleviated somewhat if protosolar abundances (Lodders 2003; 288 27 C atoms per million H) or young F and G star abundances (Sofia & Meyer 2001; 358 82 C per million H) better represent the total (gas+dust) interstellar abundance.”
Galactic Metallicity Gradients Derived from a Sample of OB Stars (2004, methodology): “This assumption has been questioned in Sofia & Meyer (2001), based in part on the fact that there was a discrepancy between the abundances of OB stars and the higher solar abundances used as comparison at that time.”
A reappraisal of the chemical composition of the Orion nebula based on Very Large Telescope echelle spectrophotometry (2004, methodology): “The data for F−G and B stars have been taken from the compilations by Sofia & Meyer (2001) and Herrero (2003), respectively.”
Oxygen, carbon and nitrogen evolution in galaxies (2002, background): “This does not seem to be the case for F- and G-stars which in principle are not greatly affected by refractory depleting processes (Sofia & Meyer 2001).”
Pixie Dust: The Silicate Features in the Diffuse Interstellar Medium (2005, background): “Interstellar abundances have recently been reviewed by Sofia & Meyer (2001), who show that young ( 2 Gyr) F and G stars and the Sun provide the best representations of the interstellar abundances.”
The GALAH survey and Gaia DR2: dissecting the stellar disc’s phase space by age, action, chemistry, and location (2018, result): “They establish a high level of chemical homogeneity across the young population, in agreement with the gas phase (Sofia & Meyer 2001).”
The chemical composition of the Sun (2009, unknown): “Indeed, rather than setting constraints on the solar abundances, the Sun is often used to infer the amount in the solid phase in the interstellar medium (e.g. Sofia & Meyer 2001).”
New Observations of the Interstellar Medium in the Lyman Break Galaxy MS 1512–cB58 (2001, result): “WhenN(H i) > 1020 cm 2, the interstellar ratio N i/H i is in good agreement with the solar abundance of N (Sofia & Meyer 2001).”
Present-day cosmic abundances - A comprehensive study of nearby early B-type stars and implications for stellar and Galactic evolution and interstellar dust models (2012, background): “There is an ongoing debate which kind of objects provide the reference suited best for the comparison: young B-type stars, young F&Gtype stars, or the Sun (Sofia & Meyer 2001).”
The global dust SED: tracing the nature and evolution of dust with DustEM (2010, background): “The solar abundances are those of Asplund et al. (2009) while the F, G stars (young≤ 2 Gyr F, G disk stars) abundances are those of Sofia & Meyer (2001).”
INTERSTELLAR DUST GRAINS (2003, background): “However, recent changes in inferred solar abundances for C and O, and comparison of photospheric abundances in F and G stars with those in B stars, led Sofia & Meyer (2001) to reject the hypothesis that interstellar abundances are appreciably subsolar.”
Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, background): “We remark that studies of local early-type stars and gas phase in diffuse interstellar medium reveal indeed a high degree of homogeneity in the present-day cosmic abundances (Sofia & Meyer 2001; Nieva & Przybilla 2012).”
Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements (2003, background): “These total gas plus dust abundances are 20−30% lower than the “old” solar abundances (depend- ing on the element) (Snow & Witt 1996; Cardelli et al. 1996; Meyer et al. 1997; Sofia & Meyer 2001).”
Are PAHs precursors of small hydrocarbons in photo-dissociation regions? The Horsehead case (2005, background): “…this corresponds to a CO abundance relative to the total number of hydrogen atoms of [CO] = 5.6 × 10−5, in rather good agreement with the gas phase abundance of carbon derived from CO in warm molecular clouds, and to the carbon abundance in diffuse clouds (Lacy et al. 1994; Sofia & Meyer 2001).”