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Martian impact craters and emplacement of ejecta by surface flow
Several types of Martian impact craters have been recognized. The most common type, the rampart crater, is distinctively different from lunar and Mercurian craters. It is typically surrounded by
Tectonic Processes on Europa: Tidal Stresses, Mechanical Response, and Visible Features
Abstract Europa's orbital eccentricity, driven by the resonance with Io and Ganymede, results in “diurnal” tides (3.5-day period) and possibly in nonsynchronous rotation. Both diurnal variation and
Magma Generation on Mars: Amounts, Rates, and Comparisons with Earth, Moon, and Venus
Total extrusive and intrusive magma generated on Mars over the last ∼3.8 billion years is estimated at 654 x 106 cubic kilometers, or 0.17 cubic kilometers per year, substantially less than rates for Earth and Venus but much more than for the Moon.
Dust devils on Earth and Mars
Dust devils, particle‐loaded vertical convective vortices found on both Earth and Mars, are characterized by high rotating wind speeds, significant electrostatic fields, and reduced pressure and
Threshold windspeeds for sand on Mars: Wind tunnel simulations
Wind friction threshold speeds (u*t) for particle movement (saltation) were determined in a wind tunnel operating at martian surface pressure with a 95 percent CO2 and 5 percent air atmosphere. The
Fluid lava flows in Gusev crater, Mars
[1] Rocks on the floor of Gusev crater are basaltic in composition, as determined from measurements by the Mars Exploration Rover, Spirit. On the basis of compositional data, models of the basaltic