The elemental composition of the Sun - III. The heavy elements Cu to Th

By N. Grevesse, Pat Scott, Martin Asplund, A. Sauval. 2014

166 citations recorded by the source corpus.

We re-evaluate the abundances of the elements in the Sun from copper (Z = 29) to thorium (Z = 90). Our results are mostly based on neutral and singly-ionised lines in the solar spectrum. We use the latest 3D hydrodynamic solar model atmosphere, and in a few cases also correct for departures from local thermodynamic equilibrium (LTE) using non-LTE (NLTE) calculations performed in 1D. In order to minimise statistical and systematic uncertainties, we make stringent line selections, employ the highest-quality observational data and carefully assess oscillator strengths, hyperfine constants and isotopic separations available in the literature, for every line included in our analysis. Our results are typically in good agreement with the abundances in the most pristine meteorites, but there are some interesting exceptions. This analysis constitutes both a full exposition and a slight update of the relevant parts of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data that we have employed.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/19403e2960b494b3ced40c51eab0fd3978cc8cf3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Serenelli
2. M. Maltoni
3. M. Gonzalez-Garcia
4. C. Peña-Garay
5. S. Basu
6. J. Laming
7. F. Villante
8. N. Vinyoles

Citations in the corpus

• The composition of Mars (2019, background): “Therefore it is very difficult to constrain the BSM abundance of Hg. Estimates of the solar abundance of Hg (few hundred ppb) are poorly constrained and Hg is undetectable in the solar photosphere (Lauretta et al., 1999; Grevesse et al., 2015; Meier et al., 2016).”
• The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, methodology): “…1 we collect the recommended solar photospheric abundances of various commonly observed elements from Grevesse and Sauval (1998), Asplund et al. (2009), (also given in Grevesse et al., 2010) Caffau et al. (2011), and Scott et al. (2014b,a) and Grevesse et al. (2014) for comparison and reference.”
• The GALAH+ survey: Third data release (2020, unknown): “…O’Brian et al. (1991), GESB86: Blackwell et al. (1986), GESB86+BWL: Blackwell et al. (1986); O’Brian et al. (1991), GESMCHF: Froese Fischer et al. (2006), Grevesse2015: Grevesse et al. (2015), HLSC: Den Hartog et al. (2003), K06: Kurucz (2006), K07: Kurucz (2007), K08: Kurucz (2008), K09:…”
• A New Generation of Standard Solar Models (2016, result): “In a recent series of papers Scott et al. (2015a,b); Grevesse et al. (2015) (for short, AGSS15) have updated previous results from AGSS09 for all but the CNO elements (and Ne, as its abundance is linked to that of O).”