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E. D. Kagan (Syracuse University), P. A. Gerakines, R. D. Mohr, Jr. (UAB)
The UV photolysis of interstellar icy grain mantles likely provides a significant contribution to the overall chemical evolution of the Galaxy. When coupled, the analyses of observed interstellar infrared spectra, laboratory experimentation, and computer models provide a powerful means of determining the scope of this contribution. However, the technique-coupling process itself can be far from simple. This poster outlines the development of a computational model used to study the evolution of interstellar ice grains that are exposed to UV radiation. This model currently accounts for the overall bulk composition of the ice, but not the internal distribution of the various components within it. We have completed batteries of test runs - both with and without the inclusion of secondary chemical reactions - in order to determine if the computational model is ready to be compared with laboratory photolysis experiments. Results from the computer model are in general agreement with expectations, suggesting that this model generates physically realistic results. This project was funded for ten weeks during the summer of 2005 by the National Science Foundation Research Experiences for Undergraduates, grant DMR-0243640.
The author(s) of this abstract have provided an email address for comments about the abstract: degeneracypressure@gmail.com
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.