Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results.
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 bedrock are 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.
Christensen
Philip R
PR
Department of Geological Sciences, Arizona State University, Tempe, AZ 85287-6305, USA. phil.christensen@asu.edu
Bandfield
Joshua L
JL
Bell
James F
JF
Gorelick
Noel
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Hamilton
Victoria E
VE
Ivanov
Anton
A
Jakosky
Bruce M
BM
Kieffer
Hugh H
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Lane
Melissa D
MD
Malin
Michael C
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McConnochie
Timothy
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McEwen
Alfred S
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McSween
Harry Y
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Mehall
Greg L
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Moersch
Jeffery E
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Nealson
Kenneth H
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Rice
James W
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Richardson
Mark I
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Ruff
Steven W
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Smith
Michael D
MD
Titus
Timothy N
TN
Wyatt
Michael B
MB
D002245:Carbon Dioxide; D005118:Extraterrestrial Environment; D019015:Geologic Sediments; D055593:Geological Phenomena; D005844:Geology; D018535:Mars; D012621:Seasons; D013696:Temperature; D014867:Water
D014867:Water; D002245:Carbon Dioxide