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 Venu
Modeling the Volcanism on Mars
β Scribed by A. Weizman; D.J. Stevenson; D. Prialnik; M. Podolak
- Publisher
- Elsevier Science
- Year
- 2001
- Tongue
- English
- Weight
- 129 KB
- Volume
- 150
- Category
- Article
- ISSN
- 0019-1035
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β¦ Synopsis
The total amount of melt produced in Mars during its evolution is estimated by means of a parameterized, one-dimensional, analytic mantle convection model that assumes a stagnant lid and whole mantle convection. The fertility of the mantle-defined as the potential to create basalt-and its variation with time are taken into account. The model is composed of core, mantle, and lithosphere, with two boundary layers separating them. The contributions to volcanism by pressure release melting (PRM), and by plumes from the core-mantle boundary layer, are compared and discussed. We show that such models tend to produce considerable melting during the early evolution of the planet, and that the amount of melting depends strongly on the abundances of radioactive elements. Although the model's assumptions may not be valid for the early evolution of the planet, the model is relevant to the later history, which is insensitive to initial conditions. We find that PRM volcanism should have ceased between 1 and 2.5 Byr ago and any recent volcanic activity must have originated in plumes.
π SIMILAR VOLUMES
The Mars Orbiter Laser Altimeter (MOLA) was used to measure the topography of several putative near-polar martian volcanic craterforms. We believe they were formed by effusive lava shield building eruptions and were not hydromagmatic events, as previously suggested. Furthermore, these craterforms ap
Athabasca and Marte Valles lie on the Cerberus plains, between the young, lava-covered plains of Elysium Planitia and Amazonis Planitia. To test pre-MGS (Mars Global Surveyor) suggestions of extremely young volcanic and fluvial activity, we present the first crater counts from MGS imagery, at resolu