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Evolution of Interstellar Ices

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Composition and Origin of Cometary Materials

Part of the book series: Space Science Series of ISSI ((SSSI,volume 8))

Abstract

Infrared observations, combined with realistic laboratory simulations, have revolutionized our understanding of interstellar ice and dust, the building blocks of comets. Ices in molecular clouds are dominated by the very simple molecules H2O, CH3OH, NH3, CO, CO2, and probably H2CO and H2. More complex species including nitriles, ketones, and esters are also present, but at lower concentrations. The evidence for these, as well as the abundant, carbon-rich, interstellar, polycyclic aromatic hydrocarbons (PAHs) is reviewed. Other possible contributors to the interstellar/pre-cometary ice composition include accretion of gas-phase molecules and in situ photochemical processing. By virtue of their low abundance, accretion of simple gas-phase species is shown to be the least important of the processes considered in determining ice composition. On the other hand, photochemical processing does play an important role in driving dust evolution and the composition of minor species. Ultraviolet photolysis of realistic laboratory analogs readily produces H2, H2CO, CO2, CO, CH4, HCO, and the moderately complex organic molecules: CH3CH2OH (ethanol), HC(=O)NH2 (formamide), CH3C(=O)NH2 (acetamide), R-CN (nitriles), and hexamethylenetetramine (HMT, C6H12N4), as well as more complex species including amides, ketones, and polyoxymethylenes (POMs). Inclusion of PAHs in the ices produces many species similar to those found in meteorites including aromatic alcohols, quinones and ethers. Photon assisted PAH-ice deuterium exchange also occurs. All of these species are readily formed and are therefore likely cometary constituents.

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Authors and Affiliations

  1. Astrochemistry Laboratory, NASA Ames Research Center, MS 245-6, Mountain View, CA, 94035-1000, USA

    Louis J. Allamandola, Max P. Bernstein, Scott A. Sandford & Robert L. Walker

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  1. Louis J. Allamandola
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  2. Max P. Bernstein
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  3. Scott A. Sandford
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Editors and Affiliations

  1. Physikalisches Institut, Universität Bern, CH-3012, Bern, Switzerland

    K. Altwegg

  2. Leiden Observatory, 2300 RA, Leiden, The Netherlands

    P. Ehrenfreund

  3. International Space Science Institute, CH-3012, Bern, Switzerland

    J. Geiss

  4. Southwest Research Institute, San Antonio, TX, 78228-0510, USA

    W. F. Huebner

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Allamandola, L.J., Bernstein, M.P., Sandford, S.A., Walker, R.L. (1999). Evolution of Interstellar Ices. In: Altwegg, K., Ehrenfreund, P., Geiss, J., Huebner, W.F. (eds) Composition and Origin of Cometary Materials. Space Science Series of ISSI, vol 8. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4211-3_20

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  • DOI: https://doi.org/10.1007/978-94-011-4211-3_20

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