Elastic dislocation modeling of wrinkle ridges on Mars

Watters, T. R.

doi:10.1016/j.icarus.2004.05.024

Cited by 63 publications

(82 citation statements)

References 72 publications

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“…The morphology of wrinkle ridges is likely related to the presence of layering and to the mechanical contact between layers (Watters, 1991(Watters, , 2004. In a multi-layered medium, if inter-layer contacts are weak, an upward propagating thrust fault will induce near-surface folding that can produce a wrinkle ridge.…”

Section: Basin-interior Smooth Plainsmentioning

confidence: 99%

“…The portion of the basin interior imaged by Mariner 10 is dominated by smooth plains, which display wrinkle ridges and troughs interpreted to record multiple episodes of deformation (Strom et al, 1975;Melosh and McKinnon, 1988;Watters et al, 2005). Wrinkle ridges are common tectonic landforms typically found in plains material on the Moon and terrestrial planets (Strom, 1972;Bryan, 1973;Watters, 1988) and are interpreted to result from a combination of folding and thrust faulting (Plescia and Golombek, 1986;Watters, 1988;Schultz, 2000;Golombek et al, 2001;Watters, 2004). Within Caloris, wrinkle ridges fall within roughly arcuate regions near the basin margin and have orientations that are both concentric and radial to the basin Earth and Planetary Science Letters 285 (2009) Contents lists available at ScienceDirect…”

Section: Introductionmentioning

confidence: 99%

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Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Watters

Murchie

Robinson

et al. 2009

Earth and Planetary Science Letters

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Section: Basin-interior Smooth Plainsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Watters

Murchie

Robinson

et al. 2009

Earth and Planetary Science Letters

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“…The interior plains exhibit wrinkle ridges and younger, cross-cutting extensional troughs (10)(11)(12). Wrinkle ridges, thought to have formed by a combination of thrust faulting and folding (13)(14)(15), occur near the eastern basin margin and are both concentric and radial to the basin, a pattern common in mare basalt-filled lunar basins. The troughs are graben formed by extensional stresses and have linear and sinuous segments that form giant polygons (10,11,15).…”

mentioning

confidence: 99%

“…Wrinkle ridges, thought to have formed by a combination of thrust faulting and folding (13)(14)(15), occur near the eastern basin margin and are both concentric and radial to the basin, a pattern common in mare basalt-filled lunar basins. The troughs are graben formed by extensional stresses and have linear and sinuous segments that form giant polygons (10,11,15). Before MESSENGER, it was not known if or how far the wrinkle ridges and graben extended westward into the then-unimaged portion of the basin, or how consistent their spatial and age relations were across the basin.…”

mentioning

confidence: 99%

Geology of the Caloris Basin, Mercury: A View from MESSENGER

Murchie

Watters

Robinson

et al. 2008

Science

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The Caloris basin, the youngest known large impact basin on Mercury, is revealed in MESSENGER images to be modified by volcanism and deformation in a manner distinct from that of lunar impact basins. The morphology and spatial distribution of basin materials themselves closely match lunar counterparts. Evidence for a volcanic origin of the basin's interior plains includes embayed craters on the basin floor and diffuse deposits surrounding rimless depressions interpreted to be of pyroclastic origin. Unlike lunar maria, the volcanic plains in Caloris are higher in albedo than surrounding basin materials and lack spectral evidence for ferrous iron-bearing silicates. Tectonic landforms, contractional wrinkle ridges and extensional troughs, have distributions and age relations different from their counterparts in and around lunar basins, indicating a different stress history.

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“…These two morphologic elements can occur independently of one another, and for wrinkle ridges in the imaged hemisphere of Mercury, this is the rule rather than the exception (see . Although the consensus is that wrinkle ridges are the result of a combination of folding and thrust faulting, the number and the geometry of the faults involved are not obvious (see Schultz 2000;Gold et al 2001;Watters 2004). Mercury's known wrinkle ridges are predominantly found in the floor material of the Caloris basin and in the smooth plains surrounding the basin.…”

Section: Geological Processes On Mercury: Tectonismmentioning

confidence: 99%

The Geology of Mercury: The View Prior to the MESSENGER Mission

Head¹,

Chapman²,

Domingue³

et al. 2007

The Messenger Mission to Mercury

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Mariner 10 and Earth-based observations have revealed Mercury, the innermost of the terrestrial planetary bodies, to be an exciting laboratory for the study of Solar System geological processes. Mercury is characterized by a lunar-like surface, a global magnetic field, and an interior dominated by an iron core having a radius at least three-quarters of the radius of the planet. The 45% of the surface imaged by Mariner 10 reveals some distinctive differences from the Moon, however, with major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. Our current image coverage of Mercury is comparable to that of telescopic photographs of the Earth's Moon prior to the launch of Sputnik in 1957. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor (∼1 km), and as with many lunar telescopic photographs, much of the available surface of Mercury is distorted by foreshortening due to viewing geometry, or poorly suited for geological analysis and impact-crater counting for age determinations because of high-Sun illumination conditions. Currently available topographic information is also very limited. Nonetheless, Mercury is a geological laboratory that represents (1) a planet where the presence of a huge iron core may be due to impact stripping of the crust and upper mantle, or alternatively, where formation of a huge core may have resulted in a residual mantle and crust of potentially unusual composition and structure; (2) a planet with an internal chemical and mechanical structure that provides new insights into planetary thermal history and the relative roles of conduction and convection in planetary heat loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the global tectonic system; (4) a planet where volcanic resurfacing may not have played a significant role in planetary history and internally generated volcanic resurfacing may have ceased at ∼3.8 Ga; (5) a planet where impact craters can be used to disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry; (6) an environment where global impact crater counts can test fundamental concepts of the distribution of impactor populations in space and time; (7) an extreme environment in which highly radar-reflective polar deposits, much more extensive than those on the Moon, can be better understood; (8) an extreme environment in which the basic processes of space weathering can be further deduced; and (9) a potential end-member in terrestrial planetary body geological evolution in which the relationships of internal and surface evolution can be clearly assessed from both a tectonic and volcanic point of view. In the half-century since the launch of Sputnik, more than 30 spacecraft have been sent to the Moon, yet only now is a second spacecraft en route to Mercury. The MESSENGER mission will address key questions ...

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Elastic dislocation modeling of wrinkle ridges on Mars

Cited by 63 publications

References 72 publications

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Geology of the Caloris Basin, Mercury: A View from MESSENGER

The Geology of Mercury: The View Prior to the MESSENGER Mission

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