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Reference | ![]() |
(C/O)![]() |
(C/O)a
![]() |
Anders & Grevesse 1989 (AG89) | 0.0194 | 0.427 | 0.958 |
Grevesse & Noels 1993 (GN93) | 0.0173 | 0.479 | 0.952 |
Grevesse & Sauval 1998 (GS98) | 0.0170 | 0.490 | 0.947 |
Holweger 2001 (H01)b | 0.0149 | 0.718 | 0.937 |
Lodders 2003 (L03) | 0.0132 | 0.501 | 0.929 |
Grevesse et al. 2007 (GAS07) | 0.0122 | 0.537 | 0.929 |
Caffau et al. 2009 (C09)c | 0.0155 | 0.575 | 0.938 |
a
This abundance ratio is
defined by Eq. (35).
b The elemental abundances
are taken from Grevesse & Sauval (1998), but for
C, N, O, Ne, Mg, Si, and Fe that are modified following the revision by
Howeger (2001).
c The elemental abundances
are taken from Grevesse & Sauval (1998), but for
N, O, and Ne following the revision by Caffau et al. (2008, 2009).
For each mixture the solar total metallicity
(in mass fraction), the abundance ratios (C/O)
and (C/O)
are indicated for comparison.
The latter marks a critical boundary for the gas molecular chemistry in
the range
.
The C and O abundances are expressed as
number fractions.
For each mixture the solar total metallicity




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