Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results
Science
By: P. R. Christensen, J. L. Bandfield, J.F. Bell III, N. Gorelick, V.E. Hamilton, A. Ivanov, B. M. Jakosky, H. H. Kieffer, M. D. Lane, M. C. Malin, T. McConnochie, A. S. McEwen, H.Y. McSween Jr., G.L. Mehall, J.E. Moersch, K.H. Nealson, J. W. Rice Jr., M.I. Richardson, S. W. Ruff, M. D. Smith, T.N. Titus, and M.B. Wyatt
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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 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.
| Publication type | Article |
|---|---|
| Publication Subtype | Journal Article |
| Title | Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results |
| Series title | Science |
| DOI | 10.1126/science.1080885 |
| Volume | 300 |
| Issue | 5628 |
| Year Published | 2003 |
| Language | English |
| Larger Work Type | Article |
| Larger Work Subtype | Journal Article |
| Larger Work Title | Science |
| First page | 2056 |
| Last page | 2061 |
| Google Analytic Metrics | Metrics page |