HR: 08:30h
AN: P21A-03    [PDF]
TI: THEMIS Visible and Infrared Investigation of Martian Meteorite-like Compositions on Mars
AU: * Hamilton, V E
EM: hamilton@higp.hawaii.edu
AF: Hawaii Institute of Geophysics and Planetology, University of Hawai'i 2525 Correa Road, Honolulu, HI 96822 United States
AU: Christensen, P R
EM: phil.christensen@asu.edu
AF: Department of Geological Sciences, Arizona State University Box 876305, Tempe, AZ 85287-6305 United States
AB: Early results from the Mars Odyssey THEMIS have revealed, in high (20 to 100 km/pixel) spatial detail, the distribution of orthopyroxene- and olivine-bearing meteorite-like materials identified in MGS TES data [Hamilton and Christensen, 2003; Hamilton et al., 2003]. The presence of significant quantities of these mafic minerals is important not only to understanding the igneous history of Mars, and the possible origins of the Martian meteorites, but also to understanding the weathering regime(s) to which they have been subjected since they were exposed. These sites now have nearly complete THEMIS coverage (day and night) by the infrared subsystem, and greater than 50 percent coverage by the visible subsystem. We will present updated descriptions of the distribution, visible and infrared spectral characteristics, and thermophysical characteristics of these sites as observed by THEMIS, and discuss how these properties provide information on the history of these materials. Additionally, we will discuss how we have used THEMIS data to confirm TES-based identifications of meteorite-like lithologies in spatially small sites. [1] Hamilton, V. E. and P. R. Christensen, LPSC XXXIV, abstract 1982, 2003. [2] Hamilton, V. E., P. R. Christensen, H. Y. McSween Jr., J. L. Bandfield, Meteor. Planet. Sci., in press, 2003.
DE: 3662 Meteorites
DE: 3672 Planetary mineralogy and petrology (5410)
DE: 5410 Composition
DE: 5415 Erosion and weathering
DE: 5464 Remote sensing
SC: Planetary Sciences [P]
MN: 2003 Fall Meeting