Chemical fractionations in meteorites--IV abundances of fourteen trace elements in L-chondrites; implications for cosmothermometry

Details Chemical fractionations in meteorites--IV abundances of fourteen trace elements in L-chondrites; implications for cosmothermometry Chemical fractionations in meteorites--IV abundances of fourteen trace elements in L-chondrites; implications for cosmothermometry

Apr 1971

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971gecoa..35..337k&link_type=abstract

Geochimica et Cosmochimica Acta, vol. 35, Issue 4, pp.337-363

Mathematics

Logic

15

Scientific paper

A neutron activation procedure for Ag, Au, Bi, Br, Cd, Cs, Cu, Ga, In, Pd, Rb, Te, Tl and Zn has been developed and applied to 12 chondrites (11 L3 to L6 and 1 LL3-4). Correlations between abundance and petrologic type were found for Bi, Br, Cs, In and Tl. These elements correlated with each other and with primordial Ar and Xe. The observed inter-element correlations generally agree with calculated curves for trace element condensation from a cosmic gas at 10 -4 ±2 atm. It appears that most fractionations of volatile elements, including noble gases, arose in the solar nebula rather than in meteorite parent bodies. A few elements (Cs, Br and Tl) sometimes are overabundant in L3,4 chondrites relative to other, less volatile elements (Cu, Ga). Either these elements became enriched in the solar nebula toward the end of accretion, or they were fractionated, presumably by volatilization, in the meteorite parent bodies. Accretion temperatures of L-chondrites were estimated from Bi and Tl contents. Petrologic types 3-6 seem to have accreted in a 100-degree interval centered on 530 +80 -60 °K. The error quoted reflects the uncertainties in total nebular pressure (10 -4±2 atm) and solubility of Bi and Tl in nickel-iron. Temperatures derived from Bi and Tl contents are generally concordant, as expected for the two-component model of and , not for the three- and multicomponent models of and and and . An equation for the fraction of In condensed ( In ) was derived from the In data, using the accretion temperatures inferred from Bi and Tl contents: log[ In /(1- In )] = (8850 ± 710)/ T - (18.82 ± 1.40).

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