Blaney, Diana L.2009-07-152009-07-151990http://hdl.handle.net/10125/9836Typescript.Thesis (Ph. D.)--University of Hawaii at Manoa, 1990.Includes bibliographical references.Microfiche.xiii, 161 leaves, bound ill. 29 cmEarth-based telescopic data provides information on the mineralogy of the Martian surface. Data was collected during the 1986 and 1988 Earth-Mars oppositions between 3 µm and 5 µm to study carbonates. sulfates. and hydrates. The 1986 data was at 3% spectral resolution with a spatial spot diameter of 2000 km and covered a wavelength region between 2.5 µm and 4.2 µm. The 3 µm bound water band was clearly observed and an upper limit of 3 - 5 wt% carbonate was established for the regions measured based on comparisons with laboratory mixtures of carbonates and Mauna Kea palagonite, a Martian soil analog. The 1988 data had 1/3% spectral resolution between 3.2 µm and 5.1 µm with a 900 km spatial resolution. These data indicate that their is substantial variation (20 %) in the depth of the 3 µm bound water band which is not correlated with atmospheric absorptions. Faint(<1%) atmospheric absorptions caused by isotopically heavy CO2 were detected at 3.6 um and 3.81 µm. An upper limit of 1 - 3 wt% carbonate was made for these regions. The implications of low carbonate abundance for climate change and weathering is explored and several models suggested. An absorption at 4.5 µm was also detected. This absorption is consistent with sulfates in mineral structure that preserves tetrahedral symmetry.en-USAll UHM dissertations and theses are protected by copyright. They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission from the copyright owner.CarbonatesSulfatesHydratesMars (Planet)Thesis