Formation of CO2, H2CO, CH3OH, HCOOH, and CH3CH2OH on an Icy Grain Analog Using Superthermal H and O Atoms

Details Formation of CO2, H2CO, CH3OH, HCOOH, and CH3CH2OH on an Icy Grain Analog Using Superthermal H and O Atoms Formation of CO2, H2CO, CH3OH, HCOOH, and CH3CH2OH on an Icy Grain Analog Using Superthermal H and O Atoms

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21440222c&link_type=abstract

American Astronomical Society, AAS Meeting #214, #402.22

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Stellar winds, bipolar outflows, and protostellar accretion infalls generate shocks in molecular clouds. Fast J-shocks are usually dissociative. They can erode dust grains and ices and thereby enhance the gas-phase abundance of the desorbed molecular species. Slower C-shocks with velocities of 5-15 km/s are too low-energy to erode grains, and yet are able to generate energetic gas-phase species that can participate in grain-surface chemistry. For example, an H-atom or O-atom accelerated to 15 km/s would provide 1.2 eV and 18.7 eV kinetic energy, respectively, to overcome energy barriers and engage in otherwise closed atom-grain reaction channels. We will present recent results using the JPL fast-atom source in which CO2, H2CO, CH3OH, HCOOH, and CH3CH2OH [1, 2] have been produced in fast H-atom and O-atom collisions with surface ices of CO and CH4 at 5 K. The reaction products are detected and analyzed using the techniques of temperature programmed desorption (TPD), quadrupole mass spectrometry (QMS). A unique random-walk procedure is used for the first time to identify the fractionation patterns of the molecular products from the patterns of other species such as H2, N2, O2, CO, H2O, CH4, and H2CO embedded in the ice blanket and devolved in the TPD/QMS process. Support of this work through NASAs Origins of Solar Systems Program is gratefully acknowledged.
[1] S. M. Madzunkov et al. Phys. Rev. A 73, 020901(R) (2006).
[2] S. M. Madzunkov et al. Ap. J. (in press).

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