Mathematics – Logic
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.2402n&link_type=abstract
American Astronomical Society Meeting 208, #24.02; Bulletin of the American Astronomical Society, Vol. 38, p.104
Mathematics
Logic
Scientific paper
Although most of the dust present in the protosolar molecular cloud was vaporized and homogenized during the formation of the Solar System, a small fraction of pre-existing mineral grains survived, trapped in the most primitive meteorites and interplanetary dust particles (IDPs). Extremely unusual isotopic compositions for most elements in these grains relative to all other planetary materials identify them as pristine stardust that condensed in the outflows and explosions of prior generations of stars [1]. Identified presolar grain types include silicate, oxide and carbonaceous phases. The latter include graphitic carbon, diamond and SiC. Moreover, meteorites and IDPs also contain abundant isotopically anomalous organic matter, some of which undoubtedly formed in stellar outflows and/or the interstellar medium. Comparison of presolar grain isotopic compositions with theoretical models and astronomical observations allow the parent stellar type (e.g. asymptotic giant branch star or supernova) to be identified and the grain data provide new constraints on nucleosynthesis and stellar evolution models. Chemical and mineralogical observations of the grains provide detailed information about dust condensation processes in stars and dust processing in the interstellar medium and early solar system. For example, presolar graphitic spheres have been shown to contain isotopically anomalous polycyclic aromatic hydrocarbons [2], which most likely condensed in carbon star outflows. This talk will review current knowledge on presolar grains and their astrophysical implications.[1] Clayton D. D. and Nittler L. R. (2004) ARAA, 42, 39-78.[2] Messenger S., et al. (1998) ApJ, 502, 284-295.
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