The Radiation Chemistry of H2O + O2 ices

Details The Radiation Chemistry of H2O + O2 ices The Radiation Chemistry of H2O + O2 ices

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6405c&link_type=abstract

American Astronomical Society, DPS meeting #38, #64.05; Bulletin of the American Astronomical Society, Vol. 38, p.613

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Molecular oxygen (O2) is known to be present on the icy Galilean satellites and is most likely formed from the radiolytic decomposition of water ice. Recent Cassini measurements have found an O2 atmosphere above Saturn's ring plane, and it is thought that this atmosphere is produced by the effect of radiation on the ring's icy particles. These observations suggest that O2 may be commonly formed in H2O ices exposed to high-energy radiation fields in the outer solar system.
In the Cosmic Ice Laboratory, we have investigated the radiation chemistry of H2O + O2 ices bombarded with 0.8 MeV protons. Using infrared spectroscopy, we have measured yields of hydrogen peroxide (H2O2) and ozone (O3), two molecules produced in our ices and identified on Galilean or Saturnian icy satellites. Absorption bands of HO2 and HO3 have been identified in our laboratory spectra for the first time. The formation, destruction, and thermal properties, of each chemical species will be discussed, and some astrobiological implications explored.
This work is supported by a NASA Postdoctoral Fellowship and NASA's Planetary Atmospheres and Planetary Geology and Geophysics programs. Support through the NASA Astrobiology Institute's Goddard Center for Astrobiology is also acknowledged.

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