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22 - Implications of observed primary lithologies

from Part V - Synthesis

Published online by Cambridge University Press:  10 December 2009

By
G. J. Taylor ,
S. M. McLennan ,
H. Y. McSween Jr. ,
M. B. Wyatt  and
R. C. F. Lentz
Edited by
Jim Bell
G. J. Taylor
Affiliation:
Hawaii Institute of Geophysics & Planetology, 1680 East-West Road, Post 504 Honolulu, HI 96822, USA
S. M. McLennan
Affiliation:
Department of Geosciences, SUNY Stony Brook Stony Brook, NY 11794-2100, USA
H. Y. McSween Jr.
Affiliation:
Department of Earth & Planetary, Science University of Tennessee, Knoxville, TN 37996-1410, USA
M. B. Wyatt
Affiliation:
Brown University, Department of Geological, Science 324 Brook Street Providence, RI 02912-1846, USA
R. C. F. Lentz
Affiliation:
University of Hawai'i at Manoa Hawai'i, Institute of Geophysics and Planetology 1680 East-West Road, POST 602 Honolulu, HI 96822, USA
Jim Bell
Affiliation:
Cornell University, New York
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Summary

ABSTRACT

Data from Martian meteorites, orbital remote-sensing instruments, and in situ measurements at robotic landing sites reveal that Mars has a heterogeneous surface composition. We use these data to infer the compositional and mineralogical nature of Martian igneous rocks. Basaltic rocks dominate, but highly mafic magmas also formed, producing cumulate rocks inside lava flows. Cumulate rocks also formed in intrusions. Evolved, silicic rocks occur, but are not abundant. The diversity of igneous rocks indicates several distinctive source regions in the Martian mantle. These sources probably formed early in Martian history as the result of crystallization in a magma ocean followed by overturn of an unstable cumulate pile. Shergottites alone represent at least two distinct mantle sources (assuming no crustal assimilation), with mixing between them, but could represent several distinct sources on the basis of initial Sr-isotopic compositions. The nakhlites may represent a somewhat complementary source, but there is clearly an additional source with subchondritic Ba/La. Surface Types 1 and 2 are probably composed of multiple types of igneous rock, possibly mixed with altered materials, and on average are different in trace element (K, Th) and Fe abundances. They may be derived from distinct mantle source regions. The crust appears to have been constructed by basaltic magmatism, some associated with primary differentiation (probably a magma ocean), the rest formed by partial melting during mantle overturn and other dynamic processes.

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Information
The Martian Surface
Composition, Mineralogy and Physical Properties
 , pp. 501 - 518
Publisher: Cambridge University Press
Print publication year: 2008

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  • Implications of observed primary lithologies
    • By G. J. Taylor, Hawaii Institute of Geophysics & Planetology, 1680 East-West Road, Post 504 Honolulu, HI 96822, USA, S. M. McLennan, Department of Geosciences, SUNY Stony Brook Stony Brook, NY 11794-2100, USA, H. Y. McSween, Jr., Department of Earth & Planetary, Science University of Tennessee, Knoxville, TN 37996-1410, USA, M. B. Wyatt, Brown University, Department of Geological, Science 324 Brook Street Providence, RI 02912-1846, USA, R. C. F. Lentz, University of Hawai'i at Manoa Hawai'i, Institute of Geophysics and Planetology 1680 East-West Road, POST 602 Honolulu, HI 96822, 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/CBO9780511536076.023
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  • Implications of observed primary lithologies
    • By G. J. Taylor, Hawaii Institute of Geophysics & Planetology, 1680 East-West Road, Post 504 Honolulu, HI 96822, USA, S. M. McLennan, Department of Geosciences, SUNY Stony Brook Stony Brook, NY 11794-2100, USA, H. Y. McSween, Jr., Department of Earth & Planetary, Science University of Tennessee, Knoxville, TN 37996-1410, USA, M. B. Wyatt, Brown University, Department of Geological, Science 324 Brook Street Providence, RI 02912-1846, USA, R. C. F. Lentz, University of Hawai'i at Manoa Hawai'i, Institute of Geophysics and Planetology 1680 East-West Road, POST 602 Honolulu, HI 96822, 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/CBO9780511536076.023
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.

  • Implications of observed primary lithologies
    • By G. J. Taylor, Hawaii Institute of Geophysics & Planetology, 1680 East-West Road, Post 504 Honolulu, HI 96822, USA, S. M. McLennan, Department of Geosciences, SUNY Stony Brook Stony Brook, NY 11794-2100, USA, H. Y. McSween, Jr., Department of Earth & Planetary, Science University of Tennessee, Knoxville, TN 37996-1410, USA, M. B. Wyatt, Brown University, Department of Geological, Science 324 Brook Street Providence, RI 02912-1846, USA, R. C. F. Lentz, University of Hawai'i at Manoa Hawai'i, Institute of Geophysics and Planetology 1680 East-West Road, POST 602 Honolulu, HI 96822, 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/CBO9780511536076.023
Available formats
×