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21 - Martian surface properties from joint analysis of orbital, Earth-based, and surface observations

from Part IV - Physical Properties of Surface Materials

Published online by Cambridge University Press:  10 December 2009

By
M. P. Golombek ,
A. F. C. Haldemann ,
R. A. Simpson ,
R. L. Fergason ,
N. E. Putzig ,
R. E. Arvidson ,
J. F. Bell III  and
M. T. Mellon
Edited by
Jim Bell
M. P. Golombek
Affiliation:
JPL MS 183-501 4800 Oak Grove Drive Pasadena, CA 91109, USA
A. F. C. Haldemann
Affiliation:
JPL 4800 Oak Grove Drive Pasadena, CA 91109, USA
R. A. Simpson
Affiliation:
Stanford University, David Packard #332 350 Serra Mall Stanford, CA 94305-9515, USA
R. L. Fergason
Affiliation:
School of Earth & Space Exploration Arizona State University, PO Box 876305 Tempe, AZ 85287-6305, USA
N. E. Putzig
Affiliation:
Laboratory for Atmospheric & Space Physics, University of Colorado, Campus Box 392 Boulder, CO 80309, USA
R. E. Arvidson
Affiliation:
Earth & Planetary Science, Washington University, St Louis, MO 63130, USA
J. F. Bell III
Affiliation:
Cornell University, Department of Astronomy, 402 Space Sciences Building, Ithaca, NY 14853-6801, USA
M. T. Mellon
Affiliation:
Laboratory for Atmospheric & Space Physics, University of Colorado – Boulder Boulder, CO 80309-0392, USA
Jim Bell
Affiliation:
Cornell University, New York
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Summary

ABSTRACT

Surface characteristics at the five sites where spacecraft have successfully landed on Mars can be related favorably to their signatures in remotely sensed data from orbit and from the Earth. Comparisons of the rock abundance, types and coverage of soils (and their physical properties), thermal inertia, albedo, and topographic slope all agree with orbital remote-sensing estimates and show that the materials at the landing sites can be used as “ground truth” for the materials that make up most of the equatorial and mid-latitude regions of Mars. The five landing sites sample two of the three dominant global thermal inertia and albedo units that cover ∼ 80% of the surface of Mars. The Viking Landers 1 and 2, Spirit, and Mars Pathfinder landing sites are representative of the moderate-to-high thermal inertia and intermediate-to-high albedo unit that is dominated by crusty, cloddy, and blocky soils (duricrust) with various abundances of rocks and bright dust. The Opportunity landing site is representative of the moderate-to-high thermal inertia and low-albedo surface unit that is relatively dust-free and composed of dark eolian sand and/or increased abundance of rocks. Interpretation of radar data confirms the presence of load bearing, relatively dense surfaces controlled by the soil type at the landing sites, regional rock populations from diffuse scattering similar to those observed directly at the sites, and root-mean-squared (RMS) slopes that compare favorably with 100 m scale topographic slopes extrapolated from altimetry profiles and meter scale slopes from high-resolution stereo images.

Type
Chapter
Information
The Martian Surface
Composition, Mineralogy and Physical Properties
 , pp. 468 - 498
Publisher: Cambridge University Press
Print publication year: 2008

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