Late formation of silicon carbide in type II supernovae.
basic_science · Level V
Where this comes from
- Record sourced from PubMed, PMID 29376119.
- Also identified by DOI 10.1126/sciadv.aao1054 and PMC identifier 5777395.
- Licence recorded as CC BY-NC.
- Because redistribution is not established, this page shows the abstract only. Follow the links below for the full text.
Abstract
We have found that individual presolar silicon carbide (SiC) dust grains from supernovae show a positive correlation between <sup>49</sup>Ti and <sup>28</sup>Si excesses, which is attributed to the radioactive decay of the short-lived (<i>t</i><sub>½</sub> = 330 days) <sup>49</sup>V to <sup>49</sup>Ti in the inner highly <sup>28</sup>Si-rich Si/S zone. The <sup>49</sup>V-<sup>49</sup>Ti chronometer shows that these supernova SiC dust grains formed at least 2 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.