The Solar Chemical Composition

By Martin Asplund, N. Grevesse, J. Sauval. 2004

900 citations recorded by the source corpus.

Abstract We present our current knowledge of the solar chemical composition based on the recent significant downward revision of the solar photospheric abundances of the most abundant metals. These new solar abundances result from the use of a 3D hydrodynamic model of the solar atmosphere instead of the classical 1D hydrostatic models, accounting for departures from LTE, and improved atomic and molecular data. With these abundances, the new solar metallicity, Z, decreases to Z=0.012, almost a factor of two lower than earlier widely used values. We compare our values with data from other sources and analyse a number of impacts of these new photospheric abundances. While resolving a number of longstanding problems, the new 3D-based solar photospheric composition also poses serious challenges for the standard solar model as judged by helioseismology.

View Paper: https://www.semanticscholar.org/paper/3b48ab23010ea2dbe334a4c001aca203ba259d26

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Citations in the corpus

micrOMEGAs_3: A program for calculating dark matter observables (2013, methodology): “To calculate nA(r) we use the profiles given [59] and [60].”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “The reference solar abundance mixture is that of Grevesse et al. (2007).”
The elemental composition of the Sun: II. The iron group elements Sc to Ni (2014, methodology): “Manganese: Previous reference solar manganese abundances (GS98; AGS05; Grevesse et al. 2007) came from Booth et al. (1984b), who found log Mn = 5.39 ± 0.03 using the HM model and Mn i lines.”
Kinematics and history of the solar neighbourhood revisited (2009, result): “Unfortunately, this slope when combined with either the traditional values (Y , Z ) = (0.260, 0.017) or the new values (0.2486, 0.0122) of Grevesse et al. (2007) is inconsistent with the generally accepted Wilkinson Microwave Anisotropy Probe (WMAP) value Y p = 0.24815 (Spergel C© 2009 The Authors.”
Non-LTE calculations for neutral Na in late-type stars using improved atomic data (2011, methodology): “All models have a standard composition, i.e. with scaled solar abundances according to Grevesse et al. (2007), plus 0.4 dex enhancement of alpha-elements in all metal-poor models ([Fe/H] ≤ −1.0).”
SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, methodology): “We calibrated the atomic line data to the NSO solar flux atlas (Wallace et al. 4 2011) to better fit the solar spectrum, adopting an atmospheric model for the Sun (Table 4) adopting the abundances of Grevesse et al. (2007).”
Non-LTE line formation of Fe in late-type stars - II. 1D spectroscopic stellar parameters (2012, unknown): “The models all have standard composition3, i.e. scaled solar (Grevesse et al. 2007) with gradual alpha-enhancement up to 0.4 dex at [Fe/H] 6 −1.0.”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, methodology): “These standard composition MARCS models use scaled solar abundances (those by Grevesse et al. 2007), but with [α/Fe] and [O/Fe] abundance ratios increasing linearly from +0.00 to +0.40 as [Fe/H] decreases from +0.00 to -1.00.”
Accurate fundamental parameters for 23 bright solar-type stars (2010, methodology): “The model atmospheres used the recently revised Solar abundances (Grevesse et al. 2007) and includedα- lement enhancement for metal-poor stars.”