Other
Scientific paper
Apr 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt.........6r&link_type=abstract
Thesis (PhD). CORNELL UNIVERSITY, Source DAI-B 60/10, p. 5115, Apr 2000, 197 pages.
Other
Scientific paper
All planetary bodies in our Solar System are complex systems. Some processes operate on more than one world and almost all worlds are the product of the interplay between countless phenomena. This thesis presents three studies of three different, but related, phenomena on three different planetary bodies. All of the studies involve geophysical modeling, and heat flow is an important process in each. The three projects can be summarized as follows: 1. Beta Regio, Venus, consists of a large shield volcano at its center surrounded by several radially oriented rifts. I model the uplift, strain and gravity anomaly due to a mantle upwelling and compare it to those same quantities derived for Beta from Magellan altimetry, gravity, and synthetic aperture radar data. The model results show that the data are consistent with the view that a relatively low density region now exists below Beta and caused the uplift and rifting in the region. 2. Early examinations of Galileo images of Europa revealed features interpreted as the surface manifestations of diapirs. Using a previously developed analytic model of thermally-driven diapirism I estimate the initial radii, depth and formation timescale of the diapirs. The diapirs, originate at a depth of no more than a few tens of kilometers. If the diapirs originate at the base of the ice, this is the thickness of the solid ice layer. Since the H2O layer is substantially thicker than this liquid water recently existed beneath the ice on Europa at this location. 3. With widespread evidence of both water and heat sources, it appears that hydrothermal systems are likely to have existed on Mars. I model hydrothermal systems in two different sizes of fresh impact craters and find that the system forms on the crater floor. In complex craters with a melt sheet, a lake will form, even under current Martian atmospheric conditions. By comparing these hydrothermal systems to those that exist and have been studied extensively on the Earth, I make predictions as to the types of minerals that will be found and the forms of life that could exist in such systems.
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