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Thick shell tectonics on one-plate planets - Applications to MarsUsing the zero frequency equations of a self-gravitating elastic spherical shell overlying a strengthless fluid, a theory for stress distribution in thick lithospheric shells on one-plate planets is developed. For both the compensated and flexural modes, stress distributions in lithospheres are reviewed. For compensated modes, surface stresses depend only on surface topography, whereas for flexural modes it is shown that, for long wavelengths, stress trajectories are mainly dependent on the lithospheric lateral density distribution and not on elastic properties. Computational analyses are performed for Mars, and it is found that isostatically compensated models correctly predict the graben structure in the immediate Tharsis region and a flexural loading model is satisfactory in explaining the graben in the regions surrounding Tharsis. A three-stage model for the evolution of Tharsis is hypothesized: isostasy with north-south graben formation on Tharsis, followed by flexural loading and radial graben formation on the perimeter of Tharsis, followed by a last stage of loading with little or no regional deformation.
Document ID
19830034334
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Banerdt, W. B.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA, United States)
Saunders, R. S.
(California Institute of Technology, Jet Propulsion Laboratory, Pasadena CA, United States)
Phillips, R. J.
(Lunar and Planetary Institute, Houston; Southern Methodist University Dallas, TX, United States)
Sleep, N. H.
(Stanford University Stanford, CA, United States)
Date Acquired
August 11, 2013
Publication Date
November 30, 1982
Subject Category
Lunar And Planetary Exploration
Accession Number
83A15552
Funding Number(s)
CONTRACT_GRANT: NAS6-3389
CONTRACT_GRANT: NAS7-100
Distribution Limits
Public
Copyright
Other

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