The rapid rotation of Mars creates a significant pseudoforce, known as the Coriolis force, that greatly modifies the flight paths and subsequent deposition of distal ejecta (ejecta with launch velocities of 3 km/s and greater). An accurate depiction of the effects of the Coriolis force requires the integration of the Coriolis terms directly into a series of spherical ballistic equations applied within a rotating reference frame. The resulting landing positions of radially ejected particles tend to form distinct wrapping patterns that are focused to specific areas in the hemisphere opposite from the source crater: around the pole for high-latitude craters (45¿ in latitude and above) and in an equatorial band for low-latitude craters (below 45¿ latitude). Consequently, particular locations on the surface receive deposits in stages: direct delivery of ejecta followed by deposits of higher-velocity ejecta. This staged deposition leads to regions of enhanced ejecta accumulations where meters of material collect (millimeters would be predicted in nonrotational radial decay models). Thus high-latitude craters could supply a considerable amount of distal products (tektites and melts) to polar locations, perhaps contributing to the dark circumpolar materials.