The cameras of the Viking landers have uncovered several lines of evidence for fine particle mobility on the Martian surface, including particulate drifts, rock-associated raised streaks, and probable ventifacts. Inferred peak wind directions in both Chryse and Utopia are roughly the same and are consistent with peak winds inferred by orbiter photography. A 24¿ systematic offset between the direction of rock-associated streaks in the Viking 1 landing site and Mariner 9 and Viking observations of crater-associated streaks is consistent in both sign and magnitude with a Coriolis acceleration of particles entrained by high-velocity winds in the course of the production of crater-associated streaks. If a significant fraction of the impact energy upon collision goes into deformation, strain, and rupture, there should be a preferential destruction of the most easily saltated grains, which are here called kamikaze particles, and a depletion of 150-μm-diameter grains. Observations of fine particulates dumped on the VL-1 grid indicate that major saltation events occurred between sols 96 and 207 and were caused by winds of >50 m s-1, normalized to the top of the velocity boundary layer. This is the first observation of saltation on another planet and a rough confirmation of the usual Bagnold saltation theory applied to another planet.