Theoretical Studies of Ice Formation in the Dynamic Interstellar Medium

Computer Science

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A part of the Spitzer legacy to interstellar medium (ISM) science will be a significant contribution to the characterization of molecular ices. Within our galaxy ice absorption features are detected by Spitzer towards every embedded protostar, stars that lie behind molecular clouds, and in absorption against the galactic infrared background. Numerous studies have focused on the carbon dioixide (CO2) molecule as the detection of its vibrational models requires space-borne platforms. Analysis of Spitzer data is providing clues to the origin of molecular ices and CO2 in particular. This has implications beyond chemistry in the ISM as interstellar and cometary ices show striking similarities in composition. However, there is little effort being placed on a theoretical underpinning of how the ice forms. We propose to take theoretical studies of ice formation, with an emphasis on CO2, in new directions by coupling recent dynamical models of molecular cloud formation to state-of-the-art gas and surface chemistry networks. In this fashion, we will constrain which ices form in abundance as low density gas condenses to form molecular clouds, thereby setting the initial chemical conditions for cloud fragmentation and star formation.

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