Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007mnras.382.1648a&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 382, Issue 4, pp. 1648-1656.
Astronomy and Astrophysics
Astronomy
12
Astrochemistry, Methods: N-Body Simulations, Ism: Atoms, Dust, Extinction, Ism: Molecules
Scientific paper
Results of classical trajectory calculations on the adsorption of H atoms to amorphous solid water (ASW) ice, at a surface temperature Ts of 10 K are presented. The calculations were performed for incidence energies Ei ranging from 10 to 1000 K, at random incidence. The adsorption probability Ps can be fitted to a simple decay function: . Our calculations predict similar adsorption probabilities for H atoms to crystalline and ASW ice, although the average binding energy Eb of the trapped H atoms calculated for ASW of 650 +/- 10 K is higher than that found for crystalline ice of 400 +/- 5 K. The binding energy distributions were fitted to Gaussian functions with full width half-maximum of 111 and 195 K for crystalline and amorphous ice surfaces, respectively. The variation of the H atom binding sites in the case of the ASW surface leads to broadening of the distribution of Eb compared to that of crystalline ice. We have also calculated the `hot-diffusion' distance travelled by the impinging atom over the surface before being thermalized, which is found to be about 30 Å long at Ei = 100 K and increases with Ei. The diffusion coefficient D of thermally trapped H atoms is calculated to be 1.09 +/- 0.04 × 10-5 cm2 s-1 at Ts = 10 K. The residence time τ of H atoms adsorbed on ASW is orders of magnitude longer than that of H atoms adsorbed on crystalline ice for the same ice Ts, suggesting that H2 formation on crystalline and non-porous ice is quite limited compared to that on porous ice. This is in good agreement with the results of experiments on H2 formation on porous and non-porous ASW surfaces. At low Ts, the long values of τ, the high values of D and the large hot distance travelled on the ASW surface before trapping the impinging H atom ensure that Langmuir-Hinshelwood and hot-atom mechanisms for H2 formation will be effective. The data presented here will be important ingredients for models to describe the formation of H2 on interstellar ices and reactions of H atoms with other species at the ice surface.
Al-Halabi Ayman
van Dishoeck Ewine F.
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