Late formation of silicon carbide in type II supernovae

Abstract

We have found that individual presolar silicon carbide (SiC) dust grains from supernovae show a positive correlation between 49Ti and 28Si excesses, which is attributed to the radioactive decay of the short-lived (t1/2=330 day) 49V to 49Ti in the inner highly 28Si-rich Si/S zone. The 49V-49Ti chronometer constrains that these supernova SiC dust grains formed at least two years after their parent stars exploded. This result supports recent dust condensation calculations that predict a delayed formation of carbonaceous and SiC grains in supernovae. The astronomical observation of continuous buildup of dust in supernovae over several years can, therefore, be interpreted as a growing addition of C-rich dust to the dust reservoir in supernovae.

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• Cosmic nucleosynthesis: a multi-messenger challenge
• The Evolution of Dust Opacity in Core Collapse Supernovae and the Rapid Formation of Dust in Their Ejecta
• Cluster analysis of presolar silicon carbide grains: evaluation of their classification and astrophysical implications
• Formation, distribution, and IR emission of dust in the clumpy ejecta of Type II-P core-collapse supernovae, in isotropic and anisotropic scenarios
• New Multielement Isotopic Compositions of Presolar SiC Grains: Implications for Their Stellar Origins
• Dust Production in a Thin Dense Shell in Supernovae with Early Circumstellar Interactions
• Observational limits on the early-time dust mass in SN1987A
• Comparison between core-collapse supernova nucleosynthesis and meteoric stardust grains: investigating magnesium, aluminium, and chromium
• Slow Neutron-Capture Process: Low-mass AGB stars and presolar silicon carbide grains
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• Presolar grains
• Representation of s-process abundances for comparison to data from bulk meteorites
• Type Iax supernovae as a source of iron-rich silicate dust