The Consequences for Volcanic Eruption Styles on Mars of Shallow Interactions Between Magma and Volatiles

Details The Consequences for Volcanic Eruption Styles on Mars of Shallow Interactions Between Magma and Volatiles The Consequences for Volcanic Eruption Styles on Mars of Shallow Interactions Between Magma and Volatiles

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p31b..04w&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #P31B-04

Other

5480 Volcanism (8450), 8414 Eruption Mechanisms, 8424 Hydrothermal Systems (8135), 8450 Planetary Volcanism (5480)

Scientific paper

Recent work has demonstrated that the lateral injection of dikes for distances of many hundreds to a few thousand km has taken place on Mars over much of its history. The depths to dike tops appear to range from a few hundreds of meters to a few km. As a result, shallow sill injection may have been fairly common. If emplaced at opportune depths, sills provide the geometrically most efficient conditions for magma to interact both thermally and mechanically with shallow solid volatiles - ices and clathrates - and with fluids. Dikes present a smaller contact area with shallow volatile layers, though this may not matter if the volatiles are liquid and can migrate efficiently through aquifers. In addition, the dike geometry provides the maximum potential for the accumulation of magmatic volatiles into foam layers or gas pockets at the tops of the dikes. We review these issues and present examples of the various possible consequences, including vigorous explosive eruptions, mildly explosive eruptions, and collapse crater formation due to slow seepage of accumulated magmatic gas. The consequences of both water and carbon dioxide being common sub-surface liquids on Mars are factored into the quantitative discussion of the dispersal of eruption products.

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