Abstract
We show why the solar chemical composition of [1] (GN93) and the similar values of [2] (AG89) and [3] (GS98), characterized by values of the metallicity of the order of 0.017 to 0.020, largely used in solar and stellar modeling, are now obsolete. They should be replaced by the new and more precise results of [4] (AGSS09), with a much lower metallicity of 0.0134.
Highlights
We know that the solar metallicity, Z, is essentially dominated by oxygen (43%), carbon (18%), neon (10%) and iron (10%)
We show why the solar chemical composition of [1] (GN93) and the similar values of [2] (AG89) and [3] (GS98), characterized by values of the metallicity of the order of 0.017 to 0.020, largely used in solar and stellar modeling, are obsolete
In the solar chemical compositions recommended by [2] (AG89), [1] (GN93) and [3] (GS98), the abundances of O and C were determined from essentially the same indicators as the ones used by [4] (AGSS09) i.e. OI and CI permitted and forbidden lines as well as molecular lines of OH, CH and C2
Summary
We know that the solar metallicity, Z, is essentially dominated by oxygen (43%), carbon (18%), neon (10%) and iron (10%). In the solar chemical compositions recommended by [2] (AG89), [1] (GN93) and [3] (GS98), the abundances of O and C were determined from essentially the same indicators as the ones used by [4] (AGSS09) i.e. OI and CI permitted and forbidden lines as well as molecular lines of OH, CH and C2. The main characteristics of the results of the three above mentioned solar mixtures and the evolution from AG89 (Z = 0.02) to GN93 (Z = 0.018) to GS98 (Z = 0.017) are the following: the results from the various indicators, permitted and forbidden atomic lines and molecular lines, agree within about 0.1 dex and the evolution from 1989 to 1998 is essentially due to progress in the atomic and molecular data used to derive the abundances
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