Alois Virag

Isotopic, optical, and trace element properties of large single SiC grains from the Murchison meteorite

Abstract Forty-one large SiC grains from the Murchison CM2 chondrite, ranging up to 15 × 26 μm, were analyzed by ion probe mass spectrometry for the isotopic compositions of C, N, Mg, and Si, and the concentrations of Al, Ti, V, Fe, Zr, and Ba. Most grains were also examined by Raman spectroscopy. The majority have large isotopic anomalies, with 13 C 12 C and 14 N 15 N up to 30X and 9X solar, and 29,30Si enriched by up to 102%.. Only two grains, characterized by extremely heavy carbon (δ13C = 28,582 and 18,883%.) give evidence for fossil 26Mg, with ( 26 Al 27 Al ) 0 ratios of 2.1 × 10−3 and 3.9 × 10−3. On the basis of C and Si isotopic composition, twenty-nine of the grains fall into three compact clusters, presumably from three discrete sources. Two of these clusters are anomalous and comprise only grains of cubic structure (according to their Raman spectra). The third, isotopically, normal cluster contains only anhedral, noncubic grains; and although contamination cannot be categorically excluded, an origin in a reducing environment in the early solar system is a viable possibility. The reality of these clusters is further supported by differences in morphology, size, N-content, and Al/N. This clustering of coarsegrained (>6 μm) SiC stands in sharp contrast to the quasicontinuous distribution af finer grained SiC and suggests that the top ~ 0.1% of the mass distribution is a distinct population. A few conclusions can be reached about the astrophysical origin of the coarse-grained SiC. The C and N isotopic compositions of the anomalous grains are not very diagnostic, being consistent with H-burning in the CNO cycle. The very existence of SiC requires C-rich stars, of C/O > 1. The Si-isotopic compositions qualitatively show the signature of neutron capture in He-burning shells of highly evolved stars, narrowing the choice to asymptotic giant branch (AGB) or Wolf-Rayet stars. AGB stars are the more likely candidates, as only they can (during their final, planetary nebula phase) provide high mass loss rates and hence the high gas densities required for growth of large SiC grains.

Al-26 and O-16 in the early solar system - Clues from meteoritic Al2O3

The study focuses on 26 Al2O3 grains up to 20 micron in size recovered from the Murchison C2 chrondite. It is observed that Mg-26/Mg-24 ranges up to 56 times the solar system ratio, but the initial Al-26/Al-27 ratios do not exceed the canonical maximum of 0.00005 in other meteoritic samples. It is concluded that this ratio represents the abundance of live Al-26 in the early solar system, not fossil radiogenic Mg-26 surviving from presolar times. The grains are shown to divide into three groups on the basis of Al-26, O-16, Ti, and V content, and distinctive correlations are found for Al-26 and O-16. An origin from at least three discrete components is suggested, two of which contained live Al-26. 24 refs.