Computer Science
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..929d&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Computer Science
Scientific paper
The clathrate structure was discovered in 1965 by Kasper and Cros [1]. It corresponds to a cage of water molecules which traps a gas molecule such as CO2 or CH4. Clathrates are widespread on Earth and are also thought to be present in the Mars polar caps and in the icy crust of the satellites of giant planets. Among these, Titan is of particular interest: it is the biggest satellite of Saturn and the only moon which has an atmosphere, mainly composed of N2 with few percents of methane. The actual presence of methane in Titan's atmosphere, where it is destroyed by photolysis, is still uncertain, but the liberation of methane by dissociation of methane clathrates reservoirs in the crust is a possible scenario [2-3]. Whereas the surface composition of Titan is still poorly known, it can be investigated using the spectroimaging capabilities of the VIMS instrument onboard Cassini. Indeed, VIMS can observe the surface in seven narrow infrared windows between 0.93 and 5 μm. The characterisation of infrared spectral signatures of clathrates provides important references to help in interpreting the remote sensing data. We are currently setting up a laboratory experiment which is aimed at both synthetizing and characterizing ices and clathrates using the complimentary methods of Raman and infrared spectroscopies. We first focus our investigations on CO2 clathrates which are relevant both for Titan and Mars.
Dupire C.
Grasset Olivier
Le Menn Erwan
Le Mouélic Stéphane
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