New constraints on the thermal and volatile evolution of Mars

Guest, A.; Smrekar, S. E.

doi:10.1016/j.pepi.2007.06.010

Cited by 16 publications

(15 citation statements)

References 40 publications

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“…Therefore, although a dry mantle rheology cannot be ruled out, a wet mantle rheology is clearly preferred. These results are similar to those presented by Guest and Smrekar (2007) and Grott and Breuer (2008a), who also concluded that the low elastic thickness values in the Noachian are best compatible with wet crustal and mantle rheologies.…”

Section: Accepted M Manuscriptsupporting

confidence: 91%

“…Furthermore, the low elastic thickness values observed during the early Martian evolution are best compatible with a wet mantle rheology (Guest and Smrekar, 2007;Grott and Breuer, 2008a). However, to investigate the whole range of possible evolution scenarios, we will study wet as well as dry mantle rheologies.…”

Section: Parametersmentioning

confidence: 99%

“…In our models, this increase is caused by the loss of the incompetent lower crustal layer (Guest and Smrekar, 2007;Grott and Breuer, 2008a), but a transition from a wet to a dry crustal rheology has also been considered (Guest and Smrekar, 2007).…”

Section: Accepted M Manuscriptmentioning

confidence: 99%

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Implications of large elastic thicknesses for the composition and current thermal state of Mars

Grott

Breuer

2009

Icarus

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To cite this version:M. Grott, D. Breuer. Implications of large elastic thicknesses for the composition and current thermal state of Mars. Icarus, Elsevier, 2009, 201 (2) This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. A C C E P T E D M A N U S C R I P T ACCEPTED MANUSCRIPT A C C E P T E D M A N U S C R I P T ACCEPTED MANUSCRIPT AbstractThe Martian elastic lithosphere thickness T e has recently been constrained by modeling the geodynamical response to loading at the Martian polar caps and T e was found to exceed 300 km at the north pole today. Geological evidence suggests that Mars has been volcanically active in the recent past and we have reinvestigated the Martian thermal evolution, identifying models which are consistent with T e > 300 km and the observed recent magmatic activity. We find that although models satisfying both constraints can be constructed, special assumptions regarding the concentration and distribution of radioactive elements, the style of mantle convection and/or the mantle's volatile content need to be made. If a dry mantle rheology is assumed, strong plumes caused by, e.g., a strongly pressure dependent mantle viscosity or endothermic phase transitions near the core-mantle boundary are required to allow for decompression melting in the heads of mantle plumes. For a wet mantle, large mantle water contents of the order of 1000 ppm are required to allow for partial mantle melting. Also, for a moderate crustal enrichment of heat producing, elements the planet's bulk composition needs to be 25% and 50% sub-chondritic for dry and wet mantle rheologies, respectively. Even then, models resulting in a globally averaged elastic thicknesses of T e > 300 km are difficult to reconcile with most elastic thickness estimates available for the Hesperian and Amazonian periods. It therefore seems likely that large elastic thicknesses in excess of 300 km are not representative for the bulk of the planet and that T e possibly shows a large degree of spatial heterogeneity.

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Section: Accepted M Manuscriptsupporting

confidence: 91%

Section: Parametersmentioning

confidence: 99%

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Implications of large elastic thicknesses for the composition and current thermal state of Mars

Grott

Breuer

2009

Icarus

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“…A wet lithospheric mantle rheology is consistent with the results based on comparative analyses between the evolution of effective elastic thickness through time and the thermal history models for Mars (Guest and Smrekar, 2007;Grott and Breuer, 2007). As the thickness of the crust in this region is ∼ 0-5 km thicker than the average planetary value , our results suggest an average thickness of ∼ 40-75 km for the Martian crust, which is consistent with the range of 38-62 km obtained by Wieczorek and Zuber (2004) from geophysical and geochemical arguments.…”

Section: Conclusion: Putting It All Togethersupporting

confidence: 81%

“…The use of a "standard" wet diabase for the Martian crust is consistent with extensive evidence for water-related geological activity during the Late Noachian and Early Hesperian (e.g., Head et al, 2001). Otherwise, a dry crustal rheology is hardly consistent with the comparison among the evolution of effective elastic thickness of the lithosphere and the thermal history models for Mars (Guest and Smrekar, 2007;Grott and Breuer, 2007).…”

Section: Heat Flow From the Depth Of Amenthes Rupes-related Thrust Faultmentioning

confidence: 80%

Ancient heat flow, crustal thickness, and lithospheric mantle rheology in the Amenthes region, Mars

Ruíz

Fernández

Gómez-Ortíz

et al. 2008

Earth and Planetary Science Letters

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Electrical Conductivity of Minerals and Rocks

Karato

Wang

2013

Physics and Chemistry of the Deep Earth

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Electrical conductivity of most minerals is sensitive to hydrogen (water) content, temperature, major element chemistry and oxygen fugacity. The influence of these parameters on electrical conductivity of major minerals has been characterized for most of the lower crust, upper mantle and transition zone minerals. When the results of properly executed experimental studies are selected, the main features of electrical conductivity in minerals can be interpreted by the physical models of impurity-assisted conduction involving ferric iron and hydrogen-related defects. Systematic trends in hydrogen-related conductivity are found among different types of hydrogen-bearing minerals that are likely caused by the difference in the mobility of hydrogen. A comparison of experimental results with geophysically inferred conductivity shows: (1) Electrical conductivity of the continental lower crust can be explained by a combination of high temperature, high (ferric) iron content presumably associated with dehydration.(2) Electrical conductivity of the asthenosphere can be explained by a modest amount of water (~10 -2 wt% in most regions, less than 10 -3 wt% in the central/western Pacific). ( 3) Electrical conductivity of the transition zone requires a higher water content (~10 -1 wt% in most regions, ~10 -3 wt% in the southern European transition zone, ~1 wt% in the East Asian transition zone). The majority of observations including those on the lower crust and the asthenosphere can be interpreted without partial melting or any fluids. However, experimental studies on electrical conductivity of lower mantle minerals are incomplete and it is not known if hydrogen enhances the conductivity of lower mantle minerals or not. Some discussions are also presented on the electrical conductivity in other planetary bodies including the Moon and Mars.

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New constraints on the thermal and volatile evolution of Mars

Cited by 16 publications

References 40 publications

Implications of large elastic thicknesses for the composition and current thermal state of Mars

Implications of large elastic thicknesses for the composition and current thermal state of Mars

Ancient heat flow, crustal thickness, and lithospheric mantle rheology in the Amenthes region, Mars

Electrical Conductivity of Minerals and Rocks

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