INTERSTELLAR GRAINS IN PRIMITIVE METEORITES - DIAMOND, SILICON-CARBIDE, AND GRAPHITE

Primitive meteorites contain a few parts per million (ppm) of pristine interstellar grains that provide information on nuclear and chemical processes in stars. Their interstellar origin is proven by highly anom alous isotopic ratios, varying more than 1000-fold for elements such a s C and N. Most grains isolated thus far are stable only under highly reducing conditions (C/O > 1), and apparently are ''stardust'' formed in stellar atmospheres. Microdiamonds, of median size approximately 10 angstrom, are most abundant (approximately 400- 1800 ppm) but least u nderstood. They contain anomalous noble gases including Xe-HL, which s hows the signature of the r-and p-processes and thus apparently is der ived from supernovae. Silicon carbide, of grain size 0.2-10 mum and ab undance approximately 6 ppm, shows the signature of the s-process and apparently comes mainly from red giant carbon (AGB) stars of 1-3 solar masses. Some grains appear to be greater-than-or-equal-to 10(9) a old er than the Solar System. Graphite spherules of grain size 0.8-7 mum a nd abundance < 2 ppm, contain highly anomalous C and noble gases, as w ell as large amounts of fossil Mg-26 from the decay of extinct Al-26. They seem to come from at least three sources, probably AGB stars, nov ae, and Wolf-Rayet stars.