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Gas hydrates formed in oceans and permafrost occur in vast quantities onEarth representing both a massive potential fuel source and a large threat inclimate forecasts. They have been predicted to be important on other bodies inour solar systems such as Enceladus, a moon of Saturn. CO$_2$-hydrates likelydrive the massive gas-rich water plumes seen and sampled by the spacecraftCassini, and the source of these hydrates is thought to be due to buoyant gashydrate particles. Dispersion forces cause gas hydrates to be coated in a 3-4nm thick film of ice, or to contact water directly, depending on which gas theycontain. These films are shown to significantly alter the properties of the gashydrate clusters, for example, whether they float or sink. It is also expectedto influence gas hydrate growth and gas leakage.

Dispersion forces stabilise ice coatings at certain gas hydrate interfaces which prevent water wetting