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New constraints on the abundances of silicate and oxide stardust from supernovae in the Acfer 094 meteorite

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Hoppe,  Peter
Particle Chemistry, Max Planck Institute for Chemistry, Max Planck Society;

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Leitner,  Jan
Particle Chemistry, Max Planck Institute for Chemistry, Max Planck Society;

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Kodolányi,  János
Particle Chemistry, Max Planck Institute for Chemistry, Max Planck Society;

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Citation

Hoppe, P., Leitner, J., & Kodolányi, J. (2015). New constraints on the abundances of silicate and oxide stardust from supernovae in the Acfer 094 meteorite. Astrophysical Journal, Letters, 808(1): L9. doi:10.1088/2041-8205/808/1/L9.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0029-2A21-0
Abstract
We studied about 5000 mu m(2) of fine-grained matrix material in the Acfer 094 meteorite by high-resolution (nominal 50 nm) NanoSIMS ion imaging for the presence of O-rich presolar (stardust) grains. This approach permits identifying presolar grains down to < 100 nm in size, compared to > 150 nm in lower-resolution (nominal 100 nm) ion imaging surveys. The number density of identified presolar grains is a about a factor of two to three higher than what was found by lower-resolution ion imaging studies. The abundances of grains of O isotope Group 3 and 4 are higher than previously found. None of the presolar grains shows the strong enrichments in O-16 expected from model predictions for the majority of supernova (SN) grains. Other potential O-rich SN grains, the Group 4 and some of the Group 3 grains, make up 33% by number and 19% by mass. This is clearly higher than the similar to 10% (by number) inferred before and the 5% (by mass) estimated by a model for stellar dust in the interstellar medium. Our work shows that O-rich SN grains might be more abundant among the population of presolar grains in primitive solar system materials than currently thought, even without the O-16-rich grains as predominantly expected from SN models.