Laboratory simulation of heavy-ion cosmic-ray interaction with condensed CO
Centre de Recherche sur les Ions, les Matériaux et la Photonique (CEA/CNRS/ENSICAEN/Université de Caen-Basse Normandie), CIMAP - CIRIL
- Ganil, Boulevard Henri Becquerel, BP 5133, 14070 Caen Cedex 05, France e-mail: firstname.lastname@example.org
2 Physics Department, Pontifícia Universidade Católica, Rua Marquês de S. Vicente 225, 22453-900 Rio de Janeiro, Brazil
3 Grupo de Física e Astronomia - CEFET/Química de Nilópolis, R. Lúcio Tavares 1045, Centro, 26530-060, Nilópolis, Brazil
4 Institut d'Astrophysique Spatiale, Astrochimie Expérimentale, UMR-8617 Université Paris-Sud, bâtiment 121, 91405 Orsay, France
Accepted: 14 January 2010
Context. Within dense interstellar clouds, from their periphery to regions deep inside, ice mantles on dust grains are exposed to cosmic-ray irradiation. Various swift ions contribute from protons to iron in the keV to TeV energy range. Observations show that in some lines of sight condensed CO molecules are an important component of the ice.
Aims. We irradiate CO ices with Ni ions of relatively high energy (50 and 537 MeV) to simulate the effects produced by fast heavy cosmic-ray ions in interstellar grain mantles.
Methods. CO gas is condensed on a CsI substrate at 13 K and irradiated by 50 MeV 58Ni13+ and 537 MeV 64Ni24+ ions up to a final fluence of ≈1 × 1013 cm-2, at a flux of 1 × 109 cm-2 s-1. The sputtering yields, the destruction rate of CO, and the rate of formation of new molecular species are measured in situ by Fourier transform infrared spectroscopy (FTIR).
Results. The measured CO destruction cross-sections and sputtering yields induced by Ni ions are, respectively, (i) for 50 MeV, σd = 1.0 × 10-13 cm2 and Y = 7 × 104 molecules/impact; (ii) for 537 MeV, σd = 3.0 × 10-14 cm2 and Y = 5.85 × 104 molecules/impact. Based on the present and previous results, the desorption rates induced by H, Ni, and Fe ions are estimated for a wide range of energies. The contribution of the heavy ions is found to dominate over that of protons in the interstellar medium.
Key words: astrochemistry / methods: laboratory / circumstellar matter / ISM: clouds / ISM: molecules
© ESO, 2010