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In this paper we discuss the propagation of dust through the interstellarmedium (ISM), and describe the destructive effects of stellar winds, jets, andsupernova shock waves on interstellar dust. We review the probability thatgrains formed in stellar outflows or supernovae survive processing in andpropagation through the ISM, and incorporate themselves relatively unprocessedinto meteoritic bodies in the solar system. We show that very large (radii >= 5micron) and very small grains (radii <= 100 Angstrom) with sizes similar to thepre-solar SiC and diamond grains extracted from meteorites, can survive thepassage through 100\kms shock waves relatively unscathed. High velocity (>= 250km/s) shocks destroy dust efficiently. However, a small (~10%) fraction of thestardust never encountered such fast shocks before incorporation into the solarsystem. All grains should therefore retain traces of their passage throughinterstellar shocks during their propagation through the ISM. The grainsurfaces should show evidence of processing due to sputtering and pitting dueto small grain cratering collisions on the micron-sized grains. This conclusionseems to be in conflict with the evidence from the large grains recovered frommeteorites which seem to show little interstellar processing.Comment: 19 pages, 5 figures (.eps), LaTeX, to appear in "Astrophysical  Implications of the Laboratory Study of Presolar Materials" AIP Conference  Proceedings, 1997 T.J. Bernatowicz and E. Zinner (eds.

The propagation and survival of interstellar grains