Volume 482, Number 2, May I 2008
|Page(s)||541 - 548|
|Section||Interstellar and circumstellar matter|
|Published online||18 February 2008|
Chemical and morphological evolution of a silicate surface under low-energy ion irradiation
Laboratoire de Structure et Propriétés de l'État Solide, UMR 8008, CNRS and Université des Sciences et Technologies de Lille, 59655 Villeneuve d'Ascq, France e-mail: email@example.com
2 Unité de Catalyse et de Chimie du Solide, UMR 8181, CNRS and Université des Sciences et Technologies de Lille, 59655 Villeneuve d'Ascq, France
3 Institut d'Astrophysique Spatiale (IAS), UMR 8617, Université Paris-Sud 11 and CNRS, 91405 Orsay, France
Accepted: 23 January 2008
Aims. Olivine surfaces have been subjected to low-energy ion irradiation with H+, He+ and Ar+ at energies within the keV range in order to simulate the effects of energetic gas-grain interactions within shocked regions of the interstellar medium.
Methods. The induced modifications in the chemical composition and the bonding configuration of the upper and the near surface regions were monitored in situ by X-ray photoelectron spectroscopy (XPS). The associated morphological evolution of the samples was studied by atomic force microscopy (AFM).
Results. Results show that the surface chemistry evolves during irradiation with a noticeable Mg enrichment relative to Si. This evolution is interpreted as coming from magnesium atom diffusion driven by the electric field caused by the positive ion implantation. The iron valence state is also strongly affected by irradiation, with reduction occurring at relatively high fluxes. However, at low fluxes the iron is found to oxidise from Fe2+ to Fe3+ due to a charge transfer between the incident positive ions and the iron in the sample. The atomic force microscopy results show that the surface roughness tends to increase with irradiation and that this roughness influences the surface chemical reactivity of the grains, as shown by the enhanced formation of carbonate on the surfaces when they are exposed to a CO2 atmosphere. The implications for the evolution of interstellar dust include an enhanced dust catalytic activity. These effects would arise from modification under irradiation of the surface reactivity and an increase in the available grain surface area.
Key words: ISM: dust, extinction / ISM: cosmic rays / methods: laboratory
© ESO, 2008
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