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