Abstract
The chemical evolution of interstellar grains is followed theoretically and observationally up to the time of the prestellar nebula. The difference in the degree of volatility of the various grain components is used to delineate their survival within the solar system. It is shown that only comets can preserve the interstellar dust in its primordial form. If the parent bodies of meteorites were formed at temperatures less than 500 K they would contain not only primordial silicate and carbon but also the complex organic molecules which are the residue products of interstellar cosmochemistry.
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Greenberg, J.M., d’Hendecourt, L.B. (1985). Evolution of Ices From Interstellar Space to the Solar System. In: Klinger, J., Benest, D., Dollfus, A., Smoluchowski, R. (eds) Ices in the Solar System. NATO ASI Series, vol 156. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5418-2_13
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