Numerical Modeling of Ejecta Dispersal from Transient Volcanic Explosions on Mars
✍ Scribed by Sarah A. Fagents; Lionel Wilson
- Publisher
- Elsevier Science
- Year
- 1996
- Tongue
- English
- Weight
- 429 KB
- Volume
- 123
- Category
- Article
- ISSN
- 0019-1035
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✦ Synopsis
fields. It is anticipated that the martian environment would have caused such features to be greater in size than would be The dynamics of ejecta dispersal in transient volcanic erupthe case in the terrestrial environment. Ash clouds associated tions on Mars are distinct from those on Earth and Venus with discrete explosions are expected to have risen to a maxibecause of the low atmospheric pressure and gravitational acmum of ȁ25 km on Mars, producing deposits having similar celeration. Numerical modeling of the physical mechanisms of widths. Another indication of a volcanic explosion site might such activity, accounting for the different martian environmenbe found in areas of high regolith ice content, such as fretted tal conditions, can help constrain the style of emplacement of terrains, where ice removal and mass-wasting may have modithe eruptive products. The scenario envisaged is one of pressurfied the vent's initial morphology. ized gas, contributed from either a magmatic or meteoric source, The modeling results highlight the implications of the occuraccumulating in the near-surface crust beneath a retaining rence of transient explosive eruptions for the global crustal medium. On failure of the confining material, the gas expands volatile distribution and provide some predictions of the likely rapidly out of the vent, displacing both the ''caprock'' and a manifestation of such activity for testing by upcoming spacemass of atmospheric gas overlying the explosion site, in a discraft missions to Mars.