Multi-element isotopic analyses of presolar graphite grains from the Orgueil meteorite

Details Multi-element isotopic analyses of presolar graphite grains from the Orgueil meteorite Multi-element isotopic analyses of presolar graphite grains from the Orgueil meteorite

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009phdt.........3j&link_type=abstract

Proquest Dissertations And Theses 2009. Section 0252, Part 0606 164 pages; [Ph.D. dissertation].United States -- Missouri: Wash

Physics

Asymptotic Giant Branch Stars, Born-Again Agb Stars, Nanosims, Presolar Graphite Grains, Short-Lived Radionuclides, Supernovae, Orgueil Meteorite

Scientific paper

This dissertation presents the results and implications of the isotopic analyses of presolar graphite grains from the primitive carbonaceous chondrite, Orgueil. Graphite grains from low- and high-density fractions were analyzed for C, N, O, Si, Al-Mg, K, Ca, and Ti isotopes. These analyses indicate that isotopic properties are density dependent. Most low-density grains come from supernovae as indicated by large 18 O, 15 N, 28 Si excesses, high inferred 26 Al/ 27 Al and 41 Ca/ 40 Ca ratios, and the initial presence of the short-lived radionuclide 44 Ti in some grains. Some high-density grains also show supernovae signatures, but a majority seems to originate from low-metallicity asymptotic giant branch stars. Evidence for this comes from correlated 12 C and 30 Si enrichments. In low-metallicity asymptotic giant branch stars, 12 C and 29,30 Si that are produced in the He shell are mixed into the envelope by the third dredge-up during the thermally pulsing phase. This scenario also increases the C/O ratio of the envelope and favours the condensation of graphite grains over SiC grains. A minor fraction of high-density graphite grains exhibits very low 12 C/ 13 C ratios and extremely large 42,43 Ca and 46,47,49,50 Ti excesses. These excesses are much larger than those expected in the envelopes of asymptotic giant branch stars and are as large as those predicted for pure He-shell material in those stars and the interior, O-rich zones of type II supernovae. However, these zones have almost pure 12 C, making the low 12 C/ 13 C ratios enigmatic. We propose that born-again, asymptotic giant branch stars that have undergone a very late thermal pulse, such as Sakurai's object, might be the stellar source for these grains. In such stars, limited mixing of the He-burning intershell with the thin, residual hydrogen envelope leads to the production of 13 C and enables material with s-process enrichments and low 12 C/ 13 C ratios to occur on the surface simultaneously. This study concludes that low-density graphite grains originate from supernovae while high-density graphite grains have multiple stellar sources: low- metallicity and born-again asymptotic giant branch stars, as well as supernovae.

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