Al-Halabi, A and Fraser, H J and Kroes, G J and van Dishoeck, E F (2004) Adsorption of CO on amorphous water-ice surfaces. Astronomy and Astrophysics, 422 (3). pp. 777-791. ISSN 0004-6361Full text not available in this repository. (Request a copy from the Strathclyde author)
We present the results of classical trajectory calculations of the adsorption of thermal CO on the surface of compact amorphous water ice, with a view to understanding the processes governing the growth and destruction of icy mantles on dust grains in the interstellar medium and interpreting solid CO infrared spectra. The calculations are performed at normal incidence, for E-i = 0.01 eV (116 K) and surface temperature T-s = 90 K. The calculations predict high adsorption probabilities (similar to1), with the adsorbed CO molecules having potential energies ranging from -0.15 to -0.04 eV with an average energy of -0.094 eV. In all the adsorbing trajectories, CO sits on top of the surface. No case of CO diffusion inside the ice or into a surface valley with restricted access was seen. Geometry minimizations suggest that the maximum potential energy of adsorbed CO (-0.155 eV) occurs when CO interacts with a "dangling OH" group, associated with the 2152 cm(-1) band seen in laboratory solid-state CO spectra. We show that relatively few "dangling OH" groups are present on the amorphous ice surface, potentially explaining the absence of this feature in astronomical spectra. CO also interacts with "bonded OH" groups, which we associate with the 2139 cm(-1) infrared feature of solid CO. Our results for CO adsorption on amorphous ice are compared with those previously obtained for CO adsorption to crystalline ice. The implications of the spectroscopic assignments are discussed in terms of the solid-CO infrared spectra observed in interstellar regions. Using the Frenkel model, the lifetime tau for which CO may remain adsorbed at the surface is calculated. At temperatures relevant to the interstellar medium, i.e. 10 K, it is longer than the age of the universe, but decreases dramatically with increasing T-s, such that at T-s = 90 K, tau = 300 ns. The pre-exponential factor tau(nu) used in the Frenkel model is found to be 0.95 +/- 0.02 ps. These data are compared to recent experimental results. The astrophysical implications of these calculations are discussed, with particular reference to the CO binding sites identified on amorphous ice surfaces, their adsorption energies, probabilities and lifetimes.
|Keywords:||astrochemistry, line identification, molecular data, molecular processes, molecules, lines and bands, carbon-monoxide complex, crystalline ice, dark cloud, hyperthermal energies, spectroscopy, interstellar ices, Solid state physics. Nanoscience, Astronomy and Astrophysics, Space and Planetary Science|
|Subjects:||Science > Physics > Solid state physics. Nanoscience|
|Department:||Faculty of Science > Physics|
|Depositing user:||Pure Administrator|
|Date Deposited:||24 Oct 2011 11:19|
|Last modified:||30 Sep 2016 02:29|