Extreme Mg-26 and O-17 enrichments in an Orgueil corundum: Identification of a presolar oxide grain

Details Extreme Mg-26 and O-17 enrichments in an Orgueil corundum: Identification of a presolar oxide grain Extreme Mg-26 and O-17 enrichments in an Orgueil corundum: Identification of a presolar oxide grain

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...425l..97h&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 425, no. 2, p. L97-L100

Astronomy and Astrophysics

Astrophysics

74

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

Scientific paper

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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