Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.122c&link_type=abstract
The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole
Other
Scientific paper
The history of trapping important quantities of carbon- and oxygen-bearing molecules onto the grains is of special significance for the formation of more complex (organic) molecules in the early solar system. Among other processes, cosmic ray-induced UV photo-processes can lead to the efficient formation of OH. Using a more accurate treatment of cosmic ray-gas interactions for disks, we obtain an increased cosmic ray-induced UV photon flux. We explore the role of the enhanced OH abundance on the gas-grain chemistry in the midplane of the disk at distances of 1 AU (near the inner rim of the disk) and 10 AU (a plausible location for comet formation). We solve the chemical rate equations while based on the UMIST database for Astrochemistry, adding to it adsorption-desorption processes and correcting for the enhanced cosmic ray-induced UV field. We are able to draw two main conclusions: I. At 1 AU the revised treatment of cosmic ray-induced processes enables new OH-driven chemical pathways that lead to high abundances of SiO, O2 and atomic oxygen. The timescale for vertical transport of SiO from the midplane to the AV = 1 region is up to an order of magnitude less than its photo-dissociation timescale, which suggests that SiO may accumulate and be observable in the surfaces of the disk. II. Our chemical model yields H2O, CO, CO2 and CH4 ice abundances at 10 AU which near the end of the disk's lifetime are compatible with space-based measurements of the ice composition of cometary bodies. Such comparison provides constraints on the physical conditions in which comets were formed.
Chaparro G.
Kamp Inga
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