Mathematics – Logic
Scientific paper
Jun 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt........18m&link_type=abstract
Thesis (PHD). CORNELL UNIVERSITY , Source DAI-B 58/12, p. 6624, Jun 1998, 224 pages.
Mathematics
Logic
2
Mars, Remote Sensing, Surface Mineralogy
Scientific paper
Using the SpectroCam-10 instrument on the Hale 200'' telecope at Palomar observatory, I have obtained an extensive set of images and spectra of Mars in the 7.5-13-μm region over the course of three successive oppositions. The data have been used to study two basic classes of scientific problems relating to the surface of Mars: the determination of the present-day thermophysical properties of the surface, and the search for spectral emissivity variations indicative of surface mineralogical composition. The results of these analyses are summarized as follows: (1) A time-sequence of thermal emission images taken over the course of one martian day shows that the present-day thermal inertia of the Cerberus region of Mars has changed since the late 1970's. Visible and near-infrared wavelength observations suggest that this change is the result of dust deposition. Modeling of the Palomar thermal IR data shows that the change in thermal inertia may be accounted for with a 2-4 mm mantle of dust, which implies a deposition rate consistent with the highest rates determined using other techniques. A deposition rate of 400 μm yr-1 is probably representative of the highest rates occurring on a regional scale on Mars today. (2) A broad spectral feature at 9.2 μm has been identified in the Acidalia region of Mars. The persistence of this feature over time indicates that it is caused by spectral emissivity variations in surface materials, and not by atmospheric dust absorption. The spectral feature is interpreted to be indicative of a silicate mineralogy on the surface. Its spectral shape is consistent with the laboratory-measured emissivity spectrum of a glassy basalt sample. (3) A global spectral map shows that Acidalia. is not the only region on the planet that displays thermal IR spectral features. Other areas of the planet, concentrated in the northern latitudes, display spectral features similar to Acidalia. There are also regions that display spectral features distinctly different from Acidalia, indicating that the surface of Mars is not mineralogically homogeneous. Areas showing spectral features are spatially well correlated with predictions of a rock abundance model that is based on thermophysical properties.
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