Radiation Synthesis Of Carbon Dioxide From Ice-coated C-13 Foil

Details Radiation Synthesis Of Carbon Dioxide From Ice-coated C-13 Foil Radiation Synthesis Of Carbon Dioxide From Ice-coated C-13 Foil

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.4802r&link_type=abstract

American Astronomical Society, DPS meeting #42, #48.02; Bulletin of the American Astronomical Society, Vol. 42, p.969

Astronomy and Astrophysics

Astronomy

Scientific paper

We have studied the synthesis of 13CO2 from 100 keV proton irradiation of 100 nm thick amorphous water ice film on top of an amorphous 13C foil (95% isotopic purity, 50 nm thick) at 20 and 120 K using infrared spectroscopy and microbalance techniques. In contrast to previous work, we use pure carbon instead of hydrogenated carbon grains (Mennella et.al., 2004). We also sputter clean the carbon surface using 100 keV Ar+ to remove any atmospheric contaminants prior to deposition of the water ice layer.
At 20K, the production of 13CO2 increases linearly with fluence and saturates at a column density of 1 × 1015 CO2 cm-2. At 120K, the CO2 column density increases linearly with fluence at a rate 43% higher than at 20 K. Further, the rate of CO2 production doubles following a fluence of 7 × 1015 H+ cm-2. The saturation column density at 120 K is 2.7 × 1015 CO2 cm-2, nearly three times larger than at 20 K. The profile of the ν3 absorption feature due asymmetric stretch of the C-O bond indicates that the CO2 produced from radiation is dispersed in the water ice, as opposed to being in aggregates at both temperatures.
We will discuss the radiation-induced chemical processes near the water ice - carbon interface that are involved in the synthesis of carbon dioxide. In particular, the formation and trapping of O2 from radiolysis of water ice at high temperatures (Teolis et.al. 2009) could play an important role in the enhancement of CO2 production at 120K. The formation of CO2 via radiolysis of the water ice-carbon interface can contribute to the solid CO2 observed on the interstellar grains and on the surfaces of the Jovian satellites such as Ganymede and Callisto.

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