Paper Presented at the 31st Annual Mid-America Regional
Astrophysical Confrence, Kansas City, MO, October 14, 2000
SOLAR ABUNDANCES OF THE ELEMENTS. O. K. Manuel, Nuclear Chemistry, University of Missouri, Rolla, MO 65401 USA (firstname.lastname@example.org).
Introduction: The 1956 compilation by Suess and Urey of the abundances of the elements  remains popular, but isotopic abundances observed in meteorites and in lunar samples seem to support the 1917 elemental abundance estimate of Harkins .
Background: In 1917,
Harkins  determined the abundances of the elements. Noting that the Earth's
crust and the Sun's gaseous envelope may not properly represent the overall
composition of these bodies, Harkins used the results of chemical analyses on
318 iron meteorites and 125 stone meteorites to conclude that iron (Fe) is the
most abundant element.
Cecilia Payne  and later Russell  used lines of different elements in the solar spectrum to show that hydrogen (H) is the most abundant element in the Sun's atmosphere. Payne regarded the high value derived for the abundance of H as "spurious" [See p. 186], and Russell regarded this as a puzzle that remained to be solved. Despite Harkins' earlier warning about using atmospheric abundances and Russell's comment that "The calculated abundance of hydrogen in the sun's atmosphere is almost incredibly great" [See p. 70], the scientific community began using line spectra of the solar photosphere to estimate the abundances of H and other light, volatile elements.
Isotopic Abundances: In 1969, the first Apollo mission returned with lunar samples and the Allende meteorite fell in Mexico. A comparison of the abundances of noble gas isotopes in lunar soil # 12001 with those in air and in a mineral separate of the Allende meteorite revealed a systematic enrichment of the lighter mass isotopes of each element implanted from the solar wind (SW). The abundances of SW-implanted He, Ne, Ar, Kr and Xe isotopes defined a smooth mass fractionation pattern , as expected if diffusion in the Sun selectively enriches lighter nuclides at the solar surface relative to heavier nuclides by a factor of (mH/mL)-4.56
Elemental Abundances: Intra-solar diffusion also explains Russell's puzzle: H is the lightest and most abundant element in the Sun's atmosphere; the second lightest element, helium (He), is the second most abundant element there. When the abundances of all elements in the solar photosphere are corrected for the diffusive mass-fractionation observed across the isotopes of SW-implanted gases, the most abundant element in the unfractionated Sun is Fe . Table 1 compares the first four abundant elements in compilations by ref. [1, 2, 5].
Harkins , Suess and Urey  Reference 
Fe H Fe
O He Ni
Ni O O
Si Ne Si
The agreement between the compilations by Harkins  and ref.  is remarkable. One is from wet chemical analyses of common meteorites; the other from line spectra of the solar photosphere and isotopic analyses of SW elements. Both indicate that the most abundant elements are those with high nuclear stability, although these exist only as trace elements in the solar photosphere.
Conclusion: The empirical equation that fits the mass-fractionation pattern of isotopes in SW-implanted He, Ne, Ar, Kr and Xe also selects from the solar photosphere the same four elements that Harkins  identified as most abundant in meteorites. The probability for the selection of any set of four different elements from the 83 in the sun would be 4! 79! /83! = 5 x 10-7 if each element had equal chance for selection and significantly less if the chance for selection depended on their atomic abundances in the photosphere. Iron (Fe) is the Sun's most abundant element.
References:  Suess H. E. and Urey H. C. (1956) Rev. Mod. Phy., 28, 5374.  Harkins W. D. (1917) J. Am. Chem. Soc., 39, 856-879.  Payne C. H. (1925) Stellar Atmospheres, Harvard Observ. Monographs # 1, 177-189.  Russell H. N. (1929) Ap. J., 70, 11-82.  Manuel O. K. and Hwaung G. (1983) Meteoritics, 18, 209-222.