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    NanoSIMS studies of Ba isotopic compositions in single presolar silicon carbide grains from AGB stars and supernovae

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    Author
    Marhas, K. K.
    Hoppe, P.
    Ott, U.
    Issue Date
    2007-01-01
    Keywords
    Silicon carbide
    presolar grains
    Supernova
    Nucleosynthesis
    
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    Citation
    Marhas, K. K., Hoppe, P., & Ott, U. (2007). NanoSIMS studies of Ba isotopic compositions in single presolar silicon carbide grains from AGB stars and supernovae. Meteoritics & Planetary Science, 42(7-8), 1077-1101.
    Publisher
    The Meteoritical Society
    Journal
    Meteoritics & Planetary Science
    URI
    http://hdl.handle.net/10150/656717
    DOI
    10.1111/j.1945-5100.2007.tb00562.x
    Additional Links
    https://meteoritical.org/
    Abstract
    We have studied 74 single presolar silicon carbide grains with sizes between 0.2 and 2.6 micrometers from the Murchison and Murray meteorites for Ba isotopic compositions using NanoSIMS. We also analyzed 7 SiC particles either consisting of sub-micron-size SiC grains or representing a morphologically and isotopically distinct subgroup. Of the 55 (likely) mainstream grains, originating from asymptotic giant branch (AGB) stars, 32 had high enough Ba contents for isotopic analysis. For 26 of them, CsHx interferences were either negligible or could be corrected with confidence. They exhibit typical s-process Ba isotopic patterns with slightly higher than solar 134Ba/136Ba and lower than solar 135,137,138Ba/136Ba ratios. Results are generally well explained in the context of neutron capture nucleosynthesis in low mass (1-3 M(sun)) AGB stars and provide constraints on AGB models, by reducing the needed 13C spread from factor of ~20 down to 2. Out of the 19 supernova X grains, three had sufficient concentrations for isotopic analysis. They tend to exhibit higher than solar 134Ba/136Ba and 138Ba/136Ba ratios, close to solar 137Ba/136Ba, and 135Ba/136Ba lower than solar but higher than in mainstream grains. This signature could indicate a mixture of n-burst type Ba with either normal Ba more s-process-rich than solar, or normal Ba plus weak s-process Ba. In the n-burst component Cs may have to be separated from Ba at ~10 years after the SN explosion. Depending on predictions for its composition, another possibility is early separation (at ~1 year) coupled with addition of some unfractionated n-burst matter. Abundances of trace elements (Sr, Zr, Cs, La, and Ce) analyzed along with Ba signify that implantation may have been an important process for their introduction.
    Type
    Article
    text
    Language
    en
    ISSN
    1945-5100
    ae974a485f413a2113503eed53cd6c53
    10.1111/j.1945-5100.2007.tb00562.x
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    Meteoritics & Planetary Science, Volume 42, Number 7-8 (2007)

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