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Research Articles
Submitted on January 10, 2005 Supernova Olivine from Cometary Dust
1 Mail Code KR, Robert M. Walker Laboratory for Space Science, NASA Johnson Space Center, Houston, Texas 77058, USA. * To whom correspondence should be addressed.
An interplanetary dust particle contains a submicrometer crystalline silicate aggregate of probable supernova origin. The grain has a pronounced enrichment in 18O/16O (13 times the solar value), and depletions in 17O/16O (1/3 times solar) and 29Si/28Si (<0.8 times solar), indicative of formation from a type II supernova. The aggregate contains olivine (Fo 83) grains <100 nm in size with microstructures that are consistent with minimal thermal alteration. This unusually Fe-rich olivine grain could have formed by equilibrium condensation from cooling supernova ejecta if several different nucleosynthetic zones mixed in the proper proportions. The supernova grain is also partially encased in 15N-rich organic matter that likely formed in a presolar cold molecular cloud.
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Science. ISSN 0036-8075 (print), 1095-9203 (online)
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