Experimental partitioning of Tc, Mo, Ru, and Re between solid and liquid during crystallization in Fe-Ni-S

LDEO Publication: 
Publication Type  Journal Article
Year of Publication  2004
Authors  Lazar, C.; Walker, D.; Walker, R. J.
Journal Title  Geochimica Et Cosmochimica Acta
Volume  68
Issue  3
Pages  643-651
Journal Date  Feb
ISBN Number  0016-7037
Accession Number  ISI:000188391500017
LDEO Publication Number  6507
Key Words  siderophile elements; molybdenum; meteorites; system; fractionation; precision; nebula

Technetium isotopes Tc-97, Tc-98 and Tc-99 decay to Mo-97, Ru-98 and Ru-99, with half-lives of 2.6 My, 4.1 My, and 0.21 My respectively. If there were early solar system processes that resulted in significant fractionation of Tc from the daughter elements, decay of extant Tc could have led to the creation of Mo and Ru isotopic heterogeneities. To assess the potential of metallic core crystallization to fractionate these elements, we examine the partitioning behavior of Tc relative to Re, Mo and Ru in the Fe-Ni-S system between solid metal and liquid metal alloy. The experimental evidence shows that Tc behaves more like the modestly compatible siderophile element Ru than the more highly compatible siderophile element Re, and that Tc is substantially more compatible than Mo. We also demonstrate a pressure effect in the partitioning of Mo during the crystallization of Fe-Ni-S melts. For a sulfur concentration in the liquid fraction of the core of 10 wt% (16.3 at%), the Jones and Malvin (1990) parameter is -ln(1-2 x 1.09 x 0.163) congruent to 0.44, which yields: D(Re) congruent to 4.1; D(Ru) congruent to 2.3; D(Tc) congruent to 1.7; D(Mo)(Lo-P) congruent to 1.0; and D(Mo)(Hi-p) congruent to 0.5. Our results suggest that detectable Tc-induced isotopic anomalies (greater than or equal to0.1 e unit) in Ru and Mo could only be produced by unrealistically extreme degrees of crystallization of metal during asteroidal core fractionation, regardless of the time scales and initial Tc abundances involved. Copyright (C) 2004 Elsevier Ltd.


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URL  <Go to ISI>://000188391500017