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|Title:||Extreme Mg-26 and O-17 enrichments in an Orgueil corundum: Identification of a presolar oxide grain|
|Authors:||Hutcheon, I. D.; Huss, G. R.; Fahey, A. J.; Wasserburg, G. J.|
|Affiliation:||AA(California Institute of Technology, Pasadena, CA, US), AB(California Institute of Technology, Pasadena, CA, US), AC(California Institute of Technology, Pasadena, CA, US), AD(California Institute of Technology, Pasadena, CA, US)|
|Publication:||Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 425, no. 2, p. L97-L100 (ApJL Homepage)|
|NASA/STI Keywords:||Aluminum Isotopes, Aluminum Oxides, Magnesium Isotopes, Orgueil Meteorite, Oxygen Isotopes, Solar System Evolution, Asymptotic Giant Branch Stars, Cosmic Dust, Interstellar Extinction, Red Giant Stars, Stellar Envelopes|
A corundum (Al2O3) grain from the Orgueil meteorite is greatly enriched
in O-17 and (Mg-26)*. The measured O-16/O-17 is 1028 +/- 11
compared to solar(O-16/O-17) = 2610. This is the largest O-17 excess so
far observed in any meteoritic material. The Mg-26 excess
((Mg-26)*) is most plausibly due to in situ decay of Al-26.
The inferred (Al-26/Al-27)0 ratio of 8.9 x 10-4 is
approximately 18 times larger than the 5 x 10-5 value
commonly observed in refractory inclusions formed in the solar system.
The large O-17 excess and high (Mg-26)* Al-27 ratio
unambiguously identify this corundum as a presolar oxide grain.
Enrichments in O-17 and Al-26 are characteristic of H-burning and point
to red giant or asymptotic giant branch (AGB) stars as likely sources.
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