Mathematics – Logic
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p23c0072l&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #P23C-0072
Mathematics
Logic
5410 Composition (1060, 3672), 5464 Remote Sensing, 5470 Surface Materials And Properties, 5480 Volcanism (6063, 8148, 8450)
Scientific paper
No firm constraints on the composition of Tharsis volcanism exist because a thick dust blanket over much of the region has hindered spectroscopic measurements. The morphology of Tharsis volcanoes is similar to basaltic shield volcanoes on Earth, but estimates of flow rheology permit a wide range of magma compositions. Here, we use THermal EMission Imaging System (THEMIS) and Thermal Emission Spectrometer (TES) data from the Mars Odyssey and Mars Global Surveyor missions, respectively, to characterize the composition of a distal portion of the Arsia Mons flow field (35° S, 138° W). These are the first recognized Tharsis lavas that extend from underneath the regional dust cover. Geologic mapping using THEMIS visible as well as daytime and nighttime thermal infrared (TIR) imagery has allowed recognition of at least four distinct flow units within this part of the flow field. Embayment and superposition relations, together with preserved flow structures and local relative crater densities, help constrain the relative timing of each flow unit. The flows have albedos ranging from 0.11-0.18 and the spectrally derived dust cover indices range from 0.968-0.975, which confirms reasonably low dust cover required for spectral determinations with TES. Preliminary linear spectral deconvolutions of TES spectra are consistent with basaltic compositions for each flow. Comparison of the Arsia flow spectra to one another indicates that, with decreasing relative age, there is a decrease in the spectral contrast. In addition, with increasing relative age, the spectral shapes evolve toward a surface type 1 spectral shape, which may have implications for the interpretation of this surface type. Further analyses of flow compositions, including petrologic modeling of the major oxides, may provide insight into the recent magmatic evolution of the Arsia Mons volcano. Although Tharsis has been hypothesized as a source for young Martian meteorites, comparisons of the Arsia flow spectra to Shergottite and Nakhlite spectra reveal no clear correlations.
Lang Nicholas P.
McSween Harry Y.
Tornabene Livio L.
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