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Mons Hansteen is a relatively high-albedo, well-known lunar ``red spot'' located on the southern margin of Oceanus Procellarum (2.3°S, 50.2°W). It is an arrowhead-shaped (∼ 25km on a side), two-layer mesa with a small cone-shaped massif on its north edge formed by three morphologically and compositionally distinct geologic units. These units were emplaced in three phases over nearly 200 million years...
Full-resolution (FMIDR) Magellan radar backscatter images have been used to characterize the geology and volcanology of the volcano Maat Mons on Venus. This volcano has often been identified by remote sensing techniques as one of the volcanoes on the planet that could have been recently active, and is the highest volcano on Venus with a relief of ∼9km. The summit of Maat Mons is characterized by a...
We have identified several landforms in the Galaxias Quadrangle of Mars (MTM 35217), 33.0–35.5°N, 216.0–218.0°W which are consistent with this area having been covered by an ancient ice sheet concurrent with volcanic eruptions. Volcanic activity was initiated by the intrusion of several large dikes measuring ∼50–100m wide and protruding up to ∼35m above the present-day surface. These dikes appear...
A distinctive flow deposit southwest of Cerberus Fossae on Mars is analyzed. The flow source is a ∼20m deep, ∼12×1.5km wide depression within a yardang associated with the Medusae Fossae Formation. The flow traveled for ∼40km following topographic lows to leave a deposit on average 3–4km wide. The surface morphology of the deposit suggests that it was produced by the emplacement of a fluid flowing...
We propose a numerical model for the formation of the closely-spaced pits found in the thin, ejecta-related deposits superposed on the floors, interior terrace blocks, and near-rim ejecta blankets of well-preserved martian impact craters. Our model predicts the explosive degassing of water from this pitted material, which is assumed to originally be water-bearing, impact melt-rich breccia at the time...
Recently acquired high-resolution images of martian impact craters provide further evidence for the interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of craters are nearly equally distributed between the two hemispheres, spanning from 53°S to...
Candidate examples of impact melt flows and debris flows have been identified at Tooting crater, an extremely young (<2Myr), 29km diameter impact crater in Amazonis Planitia, Mars. Using HiRISE and CTX images, and stereo-derived digital elevation models derived from these images, we have studied the rim and interior wall of Tooting crater to document the morphology and topography of several flow...
Evidence of volcano–ground ice interactions on Mars can provide important constraints on the timing and distribution of martian volcanic processes and climate characteristics. Northwest of the Elysium Rise is Hrad Vallis, a ∼370 m deep, 800 km long sinuous valley that begins in a source region at 34° N, 218° W. Flanking both sides of the source region is a lobate deposit that extends ∼50 km perpendicular...
Using images from the Mars Orbiter Camera, we have identified several linear ridges located 10-60 km north of the volcano Olympus Mons, Mars, at the edge of the Olympus Mons aureole materials. These ridges appear to be made of unconsolidated material by virtue of the many dust avalanche scars seen on their upper slopes. Based upon their morphology (several ridges have crater-like central depressions)...
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