Science Results from the Stardust Comet Sample Return Mission: Large Scale Mixing in the Solar Nebula and the Origin of Crystalline Silicates in Circumstellar Disks

Details Science Results from the Stardust Comet Sample Return Mission: Large Scale Mixing in the Solar Nebula and the Origin of Crystalline Silicates in Circumstellar Disks Science Results from the Stardust Comet Sample Return Mission: Large Scale Mixing in the Solar Nebula and the Origin of Crystalline Silicates in Circumstellar Disks

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.3506b&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #35.06; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

The first year of laboratory analyses of Kuiper belt materials returned to Earth by the Stardust comet sample return mission have provided important new information on: A) large-scale mixing in the solar nebula and B) the origin of crystalline silicates in circumstellar disks. Most of the >5µm solid particles collected by the mission are mineral grains or assemblages of high temperature minerals that condense at 1400K or above. The most extreme particle is a “Calcium Aluminum Inclusion” composed of refractory Ca, Al and Ti rich minerals. Like nearly identical components found in primitive meteorites, this particle shows a striking enrichment in 16O. The presence of these phases, linked by isotopic and minor element composition to rare components in meteorites, is direct evidence for radial transport of large solid grains from the center of the solar nebula to the Kuiper belt. Most of the mineral grains recovered by Stardust have solar isotopic composition and they have rather exotic minor element compositions. It appears that, like their meteoritic analogs, they formed by combinations of condensation and igneous processes and almost certainly not by the annealing of amorphous interstellar silicates, a formation process widely championed for the origin of crystalline silicate grains observed in disks and comets.

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