 Polewards of 30 degrees of latitude, the form of older impact craters is rounded out ("softened") by acceleration of soil creep by ground ice.The most notable difference between Martian craters and other craters in the Solar System is the presence of lobate (fludized) ejecta blankets.Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is thought to arise when the impacting object melts ice in the subsurface.