Mathematics – Logic
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p13d1553k&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #P13D-1553
Mathematics
Logic
5410 Composition (1060, 3672), 5464 Remote Sensing, 5470 Surface Materials And Properties, 6225 Mars
Scientific paper
Global modeling of thermal and VIS/NIR spectra of the Martian highlands reveal that many materials contain 10 - 20% olivine that spans a relatively large range of Mg/Fe contents (forsterite numbers 100 - 35). We examine the olivine-bearing locales in Terra Tyrrhena using TES-derived mineralogies, spectral variation maps made from THEMIS IR images, THEMIS and MOC visible images, MOLA topographic profiles, and geologic maps. Basaltic materials containing up to 20% forsteritic olivine (>Fo85) are exposed in knobs and craters near the Hellas rim (71E, 24S); the stratigraphic layer is >550 meters thick and may represent very thick, olivine- bearing flows or the base of an exhumed pluton. Mg-rich (Fo70) olivine is ubiquitous throughout Terra Tyrrhena, but locally high abundances occur in crater ejecta and alluvial fans that spill into craters. This suggests that Mg-rich olivine is a common component of the Martian crust that is in situ primarily in the subsurface, and this composition of olivine is commonly brought to the surface by exhumation via craters. Olivine-bearing materials with intermediate compositions (Fo50) are distributed within flat-lying intercrater flows that embay eroded ridges and knobs. The flows appear younger relative to the Noachian terrain, though they have also been subsequently eroded. Intermediate compositions predominantly occur closer to Syrtis Major, but also appear in small locations near the Hellas rim. Fe-rich olivine (
Hamilton Victoria E.
Koeppen William C.
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