Abundancia De Los Elementos

Abundances ofthe elements: Meteoritic and solar

EDWARDANDERS

Enrico Fermi Institute and Department of Chemistry, University of Chicago, Chicago, IL 60637-1433, U.S.A.

and

NKOLAS GREVESSE

Institut d’Astrophysique, Universite de Liege, B-4200 O&e-Liege, Belgium

(ReceivedJuly 14, 1988; acceptedin revisedform November 2, 1988)

Abstract-New abundance tables have been compiled for Cl chondrites and the solar photosphere and corona, based

on a critical review of the literature to mid-1988. The meteorite data are generally accurate to +5-10%. Significant

discrepancies between Sun and meteorites occur only for Fe, Mn, Ge, Pb, and W; other well-determined elements

agree to &90/oon the average. There is no evidence for group fractionations in Cl chondrites of cosmochemically

similar elements (refractories, siderophiles, volatiles, etc.), but a selective fractionation of Fe cannot be ruled out.

Abundances of odd-A n&ides between A = 65 and 209 show a generally smooth trend, with elemental abundances

conforming to the slope defined by isotopic abundances. Significant irregularities occur in the Nd-Sm-Eu region,

however, suggesting that the abundance curve is dependably smooth only down to the -20% level.

1. INTBODUCTION

THIS PAPERIS a new edition of the abundance compilations

of ANDERsand EBIHARA(1982; hereafter AE) for meteorites

and GREVESSE (1984a,b) for the solar photosphere. Although

meteoritic values have changed little, many photospheric

values, including those for C, N, 0, have improved greatly

in recent years, mainly due to the use of highly accurate tran-

sition probabilities, and thus permit a critical comparison of

solar and meteoritic abundances. In addition to better data,

our new abundance tables contain many small improvements,

such as better coupling of solar and meteoritic scales, better

Section 2 of this paper presents the new abundance tables.

Sections 3 and 4 review the elements individually for mete-

orites and the solar photosphere, showing how the values

were obtained and discussing uncertainties. Section 5 presents

values for the solar corona, from spectroscopy as well as

measurements of solar wind and solar energetic particles

(SEP). Section 6 reviews data for noble gases. Section 7 com-

pares photospheric, coronal, meteoritic, and cometary abun-

dances, as well as trends in s-process and r-process nuclides.

2. ABUNDANCE OF THE ELEMENTS AND NUCLIDES

2.1. Solar-system abundance?: Elements

Abundances on the Si = 10” scale, based mainly on Cl

chondrites, are given in Table 1, along with the values ofAE.

Columns 4 and 5 give the population

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