Thesis (M.Sc.)--York University, 2007. Graduate Programme in Earth and Space Science. / Typescript. Includes bibliographical references (leaves 85-89). Also available on the Internet. MODE OF ACCESS via web browser by entering the following URL: http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&res_dat=xri:pqdiss&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&rft_dat=xri:pqdiss:MR32013

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Thesis (M.S.)--Virginia Polytechnic Institute and State University, 1991. / Vita. Abstract. Includes bibliographical references (leaves 92-93). Also available via the Internet.

Thesis (Ph. D.) -- California Institute of Technology, 2010. / Title from home page (viewed 05/10/10). Advisor and committee chair names found in the thesis' metadata record in the digital repository. Includes bibliographical references.

Inaug.-diss.--Strassburg. / Lebenslauf. "Die vorhandenen physichen beobachtungen des Mars" (p. [10]-32) and "Die verschiedenen nomenclaturen der Marsflecke" (p. [33]-36) include bibliographical references.

Thesis--Université de Paris. / Errata slip tipped in.

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Mars is an ideal planet to study planetary evolution and development, as its crust has been preserved over its history, rather than continuously recycled through subduction, as has happened on Earth. In order to attain a more coherent understanding of martian evolution, we focused on the thermal and petrologic history of the martian lithosphere. We developed a model that calculates the thermal state and melt composition of Mars over time. This model provides insight into the planet's history and enables us to describe how the density and seismic properties have evolved over time. We calculated the temperature profile through the lithosphere and then fit an equation to pre-existing experimental data in order to produce a model to predict the composition of melt produced as a function of pressure and temperature. From the melt model, we see a trend from ultramafic to mafic composition over time. We calculated the density and seismic properties of the lithosphere and found that they increase over time, but decrease with depth, which is consistent with the recent observations of NASA's InSight mission. / Master of Science / Mars is an excellent location to study how planets change over time because its crust has remained intact, rather than being destroyed as segments of the crust move and push against each other, which happens on Earth. In order to understand how Mars has evolved over time, we built a model to show how the top part of the planet has changed over time. The model works by calculating the temperature of the rocks. We calculated these temperatures in the present day and at four, three, two, and one billion years ago. We took the temperatures and used them to calculate the elements that are present in the rocks. Knowing the chemistry of the crust made it possible for us to calculate the minerals present in the crust and upper mantle, which we used to calculate the density of the outer layers of Mars and the speed at which earthquake waves would travel through the layers. We found that the density and earthquake wave speeds decrease over the depth of the top part of the planet. Although usually an object that is denser at the top than bottom will flip over, we believe this will not happen on Mars because the rocks are thick enough to prevent them from flipping.

This dissertation examines several questions in Martian surface processes relating to water or ice using a combination of geomorphology and modeling. I first examine sublimation of ice from new small mid-latitude craters with freshly exposed ice imaged by the High Resolution Imaging Science Experiment (HiRISE) camera. I discuss the theory of sublimation by free convection and describe a model that improves on the standard version used in the Mars literature. This model shows some differences from experimental data, but this appears to be because experimental conditions do not accurately capture the sublimation regime appropriate to the Martian surface. I use this sublimation model in concert with a thermal model and calculate sublimation rates at the sites of freshly exposed ice. Calculated sublimated thicknesses of one or more millimeters during the period when HiRISE images show ice imply that this ice is relatively pure, not pore-filling. The ice table thus revealed appears consistent with a model of the Martian subsurface in which relatively clean ice overlies pore-filling ice.Pingos are hills with cores of ice formed by freezing of liquid water under pressure. Possible pingos on Mars have been much discussed because they would have significant implications for Martian hydrological processes. I surveyed HiRISE images across a broad portion of the Martian surface searching for fractured mounds. Such features are candidate pingos, since pingos often develop surface fractures as they grow. A small number of Martian landforms, not previously identified, are morphologically consistent with pingos; however, landforms that appear related to these do show morphological differences from pingos. Other origins are possible, particularly since it is difficult to produce the requisite hydrologic conditions for pingo formation. Previously proposed pingos on Mars lack surface fracturing and are unlikely to be pingos.

Thesis (Ph.D.)--Universität Berlin, 2005. / Includes bibliographical references.