Presolar Silicates In Meteorites And Interplanetary Dust Particles

Details Presolar Silicates In Meteorites And Interplanetary Dust Particles Presolar Silicates In Meteorites And Interplanetary Dust Particles

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1001..254h&link_type=abstract

IXTH TORINO WORKSHOP ON EVOLUTION AND NUCLEOSYNTHESIS IN AGB STARS AND THE IIND PERUGIA WORKSHOP ON NUCLEAR ASTROPHYSICS. AIP C

Astronomy and Astrophysics

Astrophysics

2

Interplanetary Dust And Gas, Meteors, Meteorites And Tektites, Giant And Subgiant Stars, Supernova Remnants, Particle Emission, Solar Wind

Scientific paper

Presolar silicates remained unrecognized in primitive solar system materials for a long time and only the recent development of advanced ion probe imaging techniques led to their discovery. Silicates turned out to be the most abundant presolar mineral. To date more than 200 presolar silicates have been found. Most grains (>70%) exhibit enrichments in 17O with 17O/16O ratios of up to 25x the solar ratio, close-to-solar or slightly lower than solar 18O/16O ratios, and Si-isotopic ratios close to the SiC mainstream line, although slightly shifted to the 30Si-poor side. These grains most likely formed in the winds of 1-2.5 Msolar RGB/AGB stars. 17O/16O ratios of >3×l0-3 may be the result of mass transfer in binary systems as was recently proposed for presolar oxide grains. This scenario is also supported by the Si-isotopic ratios. Some (a few %) silicate grains have enrichments in 17O and strong depletions in l8O, probably the result of cool bottom processing during the RGB or AGB phase. Presolar silicate grains with moderate to strong excesses in l8O (~10% of all silicates) most likely have a supernova origin.

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