Refractory metal nuggets within presolar graphite: First condensates from a circumstellar environment

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Abstract

Abstract Transmission electron microscope (TEM) investigations have revealed Os, Ru, Mo‐rich refractory metal nuggets within four different presolar graphites, from both the high‐density (HD) Murchison (MUR) and low‐density (LD) Orgueil (ORG) fractions. Microstructural and chemical data suggest that these are direct condensates from the gas, rather than forming later by exsolution. The presolar refractory metal nugget ( pRMN ) compositions are variable (e.g., from 8 < Os atom% < 77), but follow the same chemical fractionation trends as isolated refractory metal nuggets ( mRMN s) previously found in meteorites (Berg et al. 2009). From these compositions one can infer a temperature of last equilibration with the gas of 1405–1810 K (e.g., Berg et al. 2009 at approximately 100 dyne cm −2 pressure), which implies that the host graphites form over roughly the same range (in agreement with predictions) and that the pRMN s are chemically isolated from the gas when captured by graphite. Further, the pRMN compositions give evidence that HD graphites form at a higher T than LD ones. Chemical and phase similarities with the isolated mRMN s suggest that the mRMN s also condense directly from a gas, although from the early solar nebula rather than a presolar environment. Although the pRMN s themselves are too small for detection of isotopic anomalies, NanoSIMS isotopic measurements of their host graphites confirm a presolar origin for the assemblages. The two pRMN ‐containing LD graphites show evidence of a supernova (SN) origin, whereas the stellar origins of the pRMN s in HD graphite are unclear, because only less‐diagnostic 12 C enrichments are detectable (as is commonly true for HD graphites).

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