Concentration of H, Si, Cl, K, Fe, and Th in the low‐ and mid‐latitude regions of Mars

DOI Web Site Web Site 被引用文献10件
  • W. V. Boynton
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • G. J. Taylor
    Institute of Geophysics and Planetology University of Hawaii at Manoa Honolulu Hawaii USA
  • L. G. Evans
    Science Programs Computer Sciences Corporation Lanham Maryland USA
  • R. C. Reedy
    Institute of Meteoritics University of New Mexico Albuquerque New Mexico USA
  • R. Starr
    Department of Physics Catholic University of America Washington D. C. USA
  • D. M. Janes
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • K. E. Kerry
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • D. M. Drake
    TechSource Santa Fe New Mexico USA
  • K. J. Kim
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • R. M. S. Williams
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • M. K. Crombie
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • J. M. Dohm
    Department of Hydrology and Water Resources University of Arizona Tucson Arizona USA
  • V. Baker
    Department of Hydrology and Water Resources University of Arizona Tucson Arizona USA
  • A. E. Metzger
    Jet Propulsion Laboratory California Institute of Technology Pasadena California USA
  • S. Karunatillake
    Center for Radiophysics and Space Research Cornell University Ithaca New York USA
  • J. M. Keller
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • H. E. Newsom
    Institute of Meteoritics University of New Mexico Albuquerque New Mexico USA
  • J. R. Arnold
    Department of Chemistry University of California, San Diego La Jolla California USA
  • J. Brückner
    Max‐Planck‐Institut für Chemie Mainz Germany
  • P. A. J. Englert
    Institute of Geophysics and Planetology University of Hawaii at Manoa Honolulu Hawaii USA
  • O. Gasnault
    Centre d'Etude Spatiale des Rayonnements CNRS/UPS Toulouse France
  • A. L. Sprague
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA
  • I. Mitrofanov
    Space Research Institute (IKI) Moscow Russia
  • S. W. Squyres
    Center for Radiophysics and Space Research Cornell University Ithaca New York USA
  • J. I. Trombka
    NASA Goddard Space Flight Center Greenbelt Maryland USA
  • L. d'Uston
    Centre d'Etude Spatiale des Rayonnements CNRS/UPS Toulouse France
  • H. Wänke
    Max‐Planck‐Institut für Chemie Mainz Germany
  • D. K. Hamara
    Lunar and Planetary Laboratory University of Arizona Tucson Arizona USA

書誌事項

公開日
2007-12
権利情報
  • http://onlinelibrary.wiley.com/termsAndConditions#vor
DOI
  • 10.1029/2007je002887
公開者
American Geophysical Union (AGU)

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説明

<jats:p>We report maps of the concentrations of H, Si, Cl, K, Fe, and Th as determined by the Gamma Ray Spectrometer (GRS) on board the 2001 Mars Odyssey Mission for ±∼45° latitudes. The procedures by which the spectra are processed to yield quantitative concentrations are described in detail. The concentrations of elements determined over the locations of the various Mars landers generally agree well with the lander values except for Fe, although the mean of the GRS Fe data agrees well with that of Martian meteorites. The water‐equivalent concentration of hydrogen by mass varies from about 1.5% to 7.5% (by mass) with the most enriched areas being near Apollinaris Patera and Arabia Terra. Cl shows a distribution similar to H over the surface except that the Cl content over Medusae Fossae is much greater than elsewhere. The map of Fe shows enrichment in the northern lowlands versus the southern highlands. Silicon shows only very modest variation over the surface with mass fractions ranging from 19% to 22% over most of the planet, though a significant depletion in Si is noted in a region west of Tharsis Montes and Olympus Mons where the Si content is as low as 18%. K and Th show a very similar pattern with depletions associated with young volcanic deposits and enrichments associated with the TES Surface Type‐2 material. It is noted that there appears to be no evidence of significant globally distributed thick dust deposits of uniform composition.</jats:p>

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