Stardust in Meteorites and IDPs: Current Status, Recent Advances, and Future Prospects

Details Stardust in Meteorites and IDPs: Current Status, Recent Advances, and Future Prospects Stardust in Meteorites and IDPs: Current Status, Recent Advances, and Future Prospects

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..414..148h&link_type=abstract

Cosmic Dust - Near and Far ASP Conference Series, Vol. 414, proceedings of a conference held 8-12 September 2008 in Heidelberg,

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Primitive meteorites and IDPs contain small quantities (up to several 100 ppm) of nanometer- to micrometer-sized presolar dust grains that formed in the winds of evolved stars or in the ejecta of stellar explosions. These stardust grains can be studied in the laboratory for their isotopic compositions, chemistry, mineralogy, and structure. Among the identified stardust grains are silicon carbide, graphite, silicon nitride, refractory oxides, iron oxide, and silicates. Recent advances were pushed ahead by the availability of new analytical instrumentation (NanoSIMS, RIMS) and by co-ordinated multi-analytical approaches (SIMS, RIMS, noble gas mass spectrometry, FIB, TEM, Auger spectroscopy) in the study of single grains. This has changed our knowledge on the inventory of presolar grains considerably (e.g., discovery of presolar silicates) and allowed to get much more detailed insights into all stages of the life cycle of presolar grains, from their formation around evolved stars (RGB/AGB stars, novae, supernovae) over the journey through the ISM to the incorporation into Solar System bodies.

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