We have analyzed atom probe tomography reconstructions of disaggregated meteoritic material containing nanodiamonds and disordered carbon to determine whether these phases formed in the solar system or whether they predate the solar system and were formed in supernovae or the interstellar medium. We developed a method to distinguish between these two carbonaceous phases in < 100 nm diameter aggregates using the ratios of various native and contaminant molecular species. We find variations in measured 12C/13C ratios between the two phases that suggest hydrides form more readily during field evaporation of the disordered C than the nanodiamonds.

Auger spectroscopy has not found widespread application in the geological sciences, largely because specimens are often non-conductors that charge under electron beams. However, it has proven to be useful for the characterization of sub-micrometer mineral grains in certain meteorites, where sample charging issues can be mitigated. We describe the development of analytical protocols for the measurement of presolar silicate grains using Auger spectroscopy and review how this technique has helped our understanding of the stellar origin and subsequent evolution of these grains.

Presolar graphite contains a 22Ne-rich component called Ne-E(L). Noble gas studies on graphite aggregates and single grains have shown that although a dominant source of the 22Ne is 22Na, 22Ne in the He-shell of asymptotic giant branch stars have also contributed to the Ne-E(L). In addition to novae that have been considered to be a possible source of 22Na, supernovae are a likely source as well. Krypton isotopic ratios of the separates indicate that part of graphite formed in low-mass (≤3 M⊙) asymptotic giant branch stars of low metallicity (Z ≤ 0.006).