GEO 330 Lecture Notes - Lecture 7: Thermal Emission Spectrometer, Basaltic Andesite, Tharsis
21 Feb 2018
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Document Summary
Long history of volcanism on mars, concentrated at tharsis and elysium, and near hellas. By end of noachian (~3. 8ga) and tharsis bulge (10km high, 5000km across) was mostly built. Volcanism has continued throughout martian history and is likely still active today. Martian volcanism occurs in different tectonic context than terrestrial volcanism. Heat lost at plate boundaries match with volcano locations. Stable source of magma, sometimes away from plate boundaries. Mars has no plate tectonics (at least not for the last ~4gy), so there are no convergent or divergent margins at which volcanism can occur. Largest volcanoes on mars (mons) resemble terrestrial shield volcanoes like mauna loa, hawaii. Tharsis and elysium shield volcanoes are much larger than terrestrial counterparts. paterae are martian volcanoes that are broad like shields but have low vertical profile. Thermal emission spectrometer (tes) data indicate two major surface types on mars: type 1 = basalt, type 2 = basaltic andesite (bandfield et al. , 2000)
