A new model of the chemistry of ionizing radiation in solids: CIRIS

Abstract

The collisions between high-energy ions and solids can result in significant physical and chemical changes to the material. These effects are potentially important for better understanding the chemistry of interstellar and planetary bodies, which are exposed to cosmic radiation and the solar wind, respectively, however, modeling such collisions on a detailed microscopic basis has thus far been largely unsuccessful. To that end, a new model, entitled CIRIS: the Chemistry of Ionizing Radiation in Solids, was created to calculate the physical and chemical effects of the irradiation of solid materials. With the new code, we simulate O2 ice irradiated with 100 keV protons. Our models are able to reproduce the measured ozone abundances of a previous experimental study, as well as independently predict the approximate thickness of the ice used in that work.

References in corpus (8)

• Complex Chemistry in Star-Forming Regions: An Expanded Gas-Grain Warm-up Chemical Model
• Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores
• Simulation of the Formation and Morphology of Ice Mantles on Interstellar Grains
• Desorption of CO and O2 interstellar ice analogs
• A primordial origin for molecular oxygen in comets: A chemical kinetics study of the formation and survival of O${}_2$ ice from clouds to disks
• CO diffusion into amorphous H2O ices
• Interstellar Simulations Using A Unified Microscopic-Macroscopic Monte Carlo Model with a full Gas-Grain Network including Bulk Diffusion in Ice Mantles
• A New and Simple Approach to Determine the Abundance of Hydrogen Molecules on Interstellar Ice Mantles

Cited by in corpus (4)

• Efficient Production of S${}_8$ in Interstellar Ices: The effects of cosmic ray-driven radiation chemistry and non-diffusive bulk reactions
• ALMA Detection of Interstellar Methoxymethanol (CH${}_3$OCH${}_2$OH)
• On Simulating the Proton-Irradiation of O${}_2$ and H${}_2$O Ices Using Astrochemical-type Models, with Implications for Bulk Reactivity
• Simulations of ice chemistry in cometary nuclei