Mathematics – Logic
Scientific paper
Aug 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mpse.conf...70h&link_type=abstract
International Conference on Mars Polar Science and Exploration, p. 70
Mathematics
Logic
Mars Volcanoes, Mars Surface, Planetary Geology, Geochronology, Mars (Planet), Classifications, Topography, Volcanology, Morphology, Erosion, Ice, Mars Craters
Scientific paper
Most Martian volcanoes have common morphological features indicating mass wasting and erosion compatible with large scale break down of ground ice. While some features suggest the ground ice melted rapidly resulting in catastrophic erosive events, other features indicate a slow melting process (e.g sublimation) resulting in collapse structures. To determine relative volcano age and activity on Mars it is suggested that volcano interactions with an overlying ice sheet may be helpful. Examples of the various morphological features indicating volcano-ice interaction are drawn from the literature: (1) valley formation that probably formed in response to joekulhlaups and subglacial volcanism, (2) isolated thermocarst depressions probably formed by geothermal melting of ground ice, (3) large scale sublimation of distal strata, (4) small fluvial valleys, (5) large scale failure of volcano flanks through aureole development, (6) rimless craters without ash collars, (7) rampart craters on volcanoes, (8) channels, (9) mud flows or lahars. A Viking Orbiter image showing possible thermocarst landscape on the flank of the volcano Hadriaca Patera (Dao Vallis). Although various other explanations can account for some of these features they are all compatible with a ground ice-volcano interaction. These features suggests that to an extent most Martian volcanoes are covered with sheet of ground ice of variable thickness. Over a vast time interval this ground ice layer (or ice sheet) has been failing to a variable extent and in a number of ways depending on different volcano characteristics. As a result it is suggested that Martian volcanoes can be classified or assigned an evolutionary status depending on how widespread their interaction is with the ground ice layer. Thus, for example, within the Tharsis region the volcanoes Olympus Mons and Arsia Mons can be regarded as two evolutionary end points. Volcanism in the former has completely built up through and destroyed the ice sheet over the source area but is at a very early stage in doing so at the latter. This method could provide valuable information on the relative ages of Martian volcanoes where age dating by counting impact craters is probably of but minor value due to lava or sedimentary accumulation and impact crater burial.
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