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What can pre-solar grains tell us about the solar nebula?

Published online by Cambridge University Press:  01 August 2006

Gary R. Huss  and
Bruce T. Draine
Gary R. Huss
Affiliation:
Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, 1680 East-West Road, Honolulu, HI 96822, USA email: ghuss@higp.hawaii.edu
Bruce T. Draine
Affiliation:
Department of Astrophysical Sciences, Princeton University, 108 Peyton Hall, Princeton, NJ 08544-1001, USA email: draine@astro.princeton.edu
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Abstract

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Several types of pre-solar grains, grains that existed prior to solar system formation, have been found in the fine-grained components of primitive meteorites, interplanetary dust particles (IDPs), and comet samples. Known pre-solar components have isotopic compositions that reflect formation from the ejecta of evolved stars. Other pre-solar materials may have isotopic compositions very similar to solar system materials, making their identification as pre-solar grains problematic. Pre-solar materials exhibit a range of chemical and thermal resistance, so their relative abundances can be used to probe the conditions in the solar nebula. Detailed information on the relative abundances of pre-solar and solar-system materials can provide information on the temperatures, radiation environment, and degree of radial mixing in the early solar system.

Keywords

pre-solar grainssolar system: formationISM: abundancesISM: dust
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Highlights of Astronomy 14: Highlights of Astronomy , August 2006 , pp. 353 - 356
Copyright
Copyright © International Astronomical Union 2007

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