Laboratory studies of primitive meteorites have been instrumental in classifying the variety of micron-scale dust condensates formed in the outflows of massive stars near the end of their life. Approximately 1% of studied presolar silicon carbide grains, known as SiC-X grains, display peculiar isotopic inclusions that pinpoint their origin to Type II supernovae. Detailed study of these supernova condensates shows a range of crystal structures and physical morphology, indicating a complex formation history within the ejecta. We model the formation of SiC molecules and condensates in the non-equlibrium ejecta using kinetic chemistry. Exploring a wide parameter space in gas density and elemental composition, shows that the formation of SiC is highly dependent on the C/O and C/Si ratios as well as the density of the ejecta.

Formation and survival of silicon carbide in supernova ejecta

ACS Fall 2021

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