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19 - Physical properties of the Martian surface from spectrophotometric observations

from Part IV - Physical Properties of Surface Materials

Published online by Cambridge University Press:  10 December 2009

By
J. R. Johnson ,
J. F. Bell III ,
P. Geissler ,
W. M. Grundy ,
E. A. Guinness ,
P. C. Pinet  and
J. Soderblom
Edited by
Jim Bell
J. R. Johnson
Affiliation:
US Geological Survey Astrogeology Team 2255 N. Gemini Drive Flagstaff, AZ 86001-1698, USA
J. F. Bell III
Affiliation:
Cornell University, Department of Astronomy, 402 Space Sciences Building, Ithaca, NY 14853-6801, USA
P. Geissler
Affiliation:
US Geological Survey 2255 N. Gemini Drive Flagstaff, AZ 86001, USA
W. M. Grundy
Affiliation:
Lowell Observatory 1400 W. Mars Hill Road Flagstaff, AZ 86001, USA
E. A. Guinness
Affiliation:
Washington University, Campus Box 1169 St Louis, MO 63130, USA
P. C. Pinet
Affiliation:
UMR 5562/CNRS Observatoire Midi-Pyrenees 14 Avenue Edouard Belin Toulouse, 31400, France
J. Soderblom
Affiliation:
Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd. Tucson, AZ 85721, USA
Jim Bell
Affiliation:
Cornell University, New York
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Summary

ABSTRACT

The reflection of visible and near-infrared light from Mars can vary significantly depending on the directional scattering characteristics of surface materials. Observations acquired under a range of illumination and viewing angles can be input to radiative transfer models to constrain the albedo, surface roughness, grain size, and/or porosity of these materials. This chapter reviews multiangular measurements of Mars obtained by Earth-based telescopes (including the Hubble Space Telescope), orbiters (Mariner, Viking, Mars Express), landers (Viking, Mars Pathfinder), and rovers (Mars Exploration Rovers), and how the photometric analyses of these datasets have been used to understand the surface properties of local and regional geologic units and terrain types. Although acquisition of data covering sufficient incidence, emission, or phase angles to fully constrain all parameters within photometric models is challenging, a common theme among these studies is the dominantly backscattering nature of the Martian surface, the magnitude of which is often related to the presence of high-albedo aeolian dust. The local and regional photometric variability observed in these data encourages further refinement of radiative transfer methods and atmospheric correction algorithms to provide additional tools with which to categorize and map distinct photometric units on Mars, particularly to provide support for ongoing and upcoming orbital and landed missions.

Type
Chapter
Information
The Martian Surface
Composition, Mineralogy and Physical Properties
 , pp. 428 - 450
Publisher: Cambridge University Press
Print publication year: 2008

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  • Physical properties of the Martian surface from spectrophotometric observations
    • By J. R. Johnson, US Geological Survey Astrogeology Team 2255 N. Gemini Drive Flagstaff, AZ 86001-1698, USA, J. F. Bell III, Cornell University, Department of Astronomy, 402 Space Sciences Building, Ithaca, NY 14853-6801, USA, P. Geissler, US Geological Survey 2255 N. Gemini Drive Flagstaff, AZ 86001, USA, W. M. Grundy, Lowell Observatory 1400 W. Mars Hill Road Flagstaff, AZ 86001, USA, E. A. Guinness, Washington University, Campus Box 1169 St Louis, MO 63130, USA, P. C. Pinet, UMR 5562/CNRS Observatoire Midi-Pyrenees 14 Avenue Edouard Belin Toulouse, 31400, France, J. Soderblom, Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd. Tucson, AZ 85721, USA
  • Edited by Jim Bell, Cornell University, New York
  • Book: The Martian Surface
  • Online publication: 10 December 2009
  • Chapter DOI: https://doi.org/10.1017/CBO9780511536076.020
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  • Physical properties of the Martian surface from spectrophotometric observations
    • By J. R. Johnson, US Geological Survey Astrogeology Team 2255 N. Gemini Drive Flagstaff, AZ 86001-1698, USA, J. F. Bell III, Cornell University, Department of Astronomy, 402 Space Sciences Building, Ithaca, NY 14853-6801, USA, P. Geissler, US Geological Survey 2255 N. Gemini Drive Flagstaff, AZ 86001, USA, W. M. Grundy, Lowell Observatory 1400 W. Mars Hill Road Flagstaff, AZ 86001, USA, E. A. Guinness, Washington University, Campus Box 1169 St Louis, MO 63130, USA, P. C. Pinet, UMR 5562/CNRS Observatoire Midi-Pyrenees 14 Avenue Edouard Belin Toulouse, 31400, France, J. Soderblom, Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd. Tucson, AZ 85721, USA
  • Edited by Jim Bell, Cornell University, New York
  • Book: The Martian Surface
  • Online publication: 10 December 2009
  • Chapter DOI: https://doi.org/10.1017/CBO9780511536076.020
Available formats
×

Save book to Google Drive

To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Google Drive.

  • Physical properties of the Martian surface from spectrophotometric observations
    • By J. R. Johnson, US Geological Survey Astrogeology Team 2255 N. Gemini Drive Flagstaff, AZ 86001-1698, USA, J. F. Bell III, Cornell University, Department of Astronomy, 402 Space Sciences Building, Ithaca, NY 14853-6801, USA, P. Geissler, US Geological Survey 2255 N. Gemini Drive Flagstaff, AZ 86001, USA, W. M. Grundy, Lowell Observatory 1400 W. Mars Hill Road Flagstaff, AZ 86001, USA, E. A. Guinness, Washington University, Campus Box 1169 St Louis, MO 63130, USA, P. C. Pinet, UMR 5562/CNRS Observatoire Midi-Pyrenees 14 Avenue Edouard Belin Toulouse, 31400, France, J. Soderblom, Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd. Tucson, AZ 85721, USA
  • Edited by Jim Bell, Cornell University, New York
  • Book: The Martian Surface
  • Online publication: 10 December 2009
  • Chapter DOI: https://doi.org/10.1017/CBO9780511536076.020
Available formats
×