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Origin and thermal evolution of Mars

Technical Report ·
OSTI ID:5502640
The thermal evolution of Mars is governed by subsolidus mantle convection beneath a thick lithosphere. Models of the interior evolution are developed by parameterizing mantle convective heat transport in terms of mantle viscosity, the superadiabatic temperature rise across the mantle, and mantle heat production. Geological, geophysical, and geochemical observations of the compositon and structure of the interior and of the timing of major events in Martian evolution are used to constrain the model computations. Such evolutionary events include global differentiation, atmospheric outgassing, and the formation of the hemispherical dichotomy and Tharsis. Numerical calculations of fully three-dimensional, spherical convection in a shell the size of the Martian mantle are performed to explore plausible patterns of Martian mantel convection and to relate convective features, such as plumes, to surface features, such as Tharsis. The results from the model calculations are presented.
Research Organization:
California Univ., Los Angeles, CA (United States)
OSTI ID:
5502640
Report Number(s):
N-91-23011; NASA-CR--188095; NAS--1.26:188095; CNN: NAG9-39; NAG5-814; NSG-7315; NSG-7297
Country of Publication:
United States
Language:
English

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