Morphology and Composition of the Surface of Mars: Mars Odyssey THEMIS Results

Author:

Christensen Philip R.12345,Bandfield Joshua L.12345,Bell III James F.12345,Gorelick Noel12345,Hamilton Victoria E.12345,Ivanov Anton12345,Jakosky Bruce M.12345,Kieffer Hugh H.12345,Lane Melissa D.12345,Malin Michael C.12345,McConnochie Timothy12345,McEwen Alfred S.12345,McSween Harry Y.12345,Mehall Greg L.12345,Moersch Jeffery E.12345,Nealson Kenneth H.12345,Rice James W.12345,Richardson Mark I.12345,Ruff Steven W.12345,Smith Michael D.12345,Titus Timothy N.12345,Wyatt Michael B.12345

Affiliation:

1. Department of Geological Sciences, Arizona State University, Tempe, AZ 85287–6305, USA.

2. Department of Astronomy, Cornell University, Ithaca, NY 14853–6801, USA.

3. Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA.

4. Jet Propulsion Laboratory, Pasadena, CA 91109–8099, USA.

5. LASP, University of Colorado, Boulder, CO 80309, USA.

Abstract

The Thermal Emission Imaging System (THEMIS) on Mars Odyssey has produced infrared to visible wavelength images of the martian surface that show lithologically distinct layers with variable thickness, implying temporal changes in the processes or environments during or after their formation. Kilometer-scale exposures of bedrockare observed; elsewhere airfall dust completely mantles the surface over thousands of square kilometers. Mars has compositional variations at 100-meter scales, for example, an exposure of olivine-rich basalt in the walls of Ganges Chasma. Thermally distinct ejecta facies occur around some craters with variations associated with crater age. Polar observations have identified temporal patches of water frost in the north polar cap. No thermal signatures associated with endogenic heat sources have been identified.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference33 articles.

1. Space Science Reviews

2. Sedimentary Rocks of Early Mars

3. Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission

4. All infrared images presented here were acquired using Band 9 centered at 12.6 μm and are 32 km wide unless otherwise noted.

5. Soil and Surface Temperatures at the Viking Landing Sites

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