The Canyonlands model for planetary grabens: revised physical basis and implications

Small-scale lunar graben: Distribution, dimensions, and formation processes

“…In this model, fault initiation occurs at the surface and is likely influenced by local inhomogeneities, stress concentrations, or planes of weakness. Graben width is largely dependent on the initiation depth of the normal fault (Melosh and Williams, 1989) and is influenced by the flexural rigidity of the material it forms in, which depends on layer thickness and material properties (e.g., the elastic ''stiffness'' or Young's modulus) (Buck, 1988;Schultz-Ela and Walsh, 2002;Schultz et al, 2007). The width of a symmetric graben (bounded by antithetic normal faults dipping at $60°) can approximate layer thickness if the bounding faults converge at the base of the layer (Golombek, 1979).…”

“…The width of a symmetric graben (bounded by antithetic normal faults dipping at $60°) can approximate layer thickness if the bounding faults converge at the base of the layer (Golombek, 1979). However, since faults likely nucleate at the surface and propagate downward, instead of originating at some discontinuity at depth and propagating toward the surface, graben tend to be asymmetric (Schultz et al, 2007). Thus, the widths of Fig.…”

Interpretation and analysis of planetary structures

“…One bounding or border fault (in this case, the northwestern one) is much more pronounced than the other one, and the graben floor is clearly tilted, although the regional topography does not display any tilting. This geometry is typical for terrestrial grabens such as the Canyonlands graben system (e.g., Trudgill and Cartwright, 1994;Moore and Schultz, 1999;Schultz et al, 2007).…”

Volcanism and tectonism across the inner solar system: an overview

“…Extensional features include normal faults, halfgraben, graben and rift-like structures such as Acheron Fossae (Kronberg et al 2007) (Figs 8 & 9g). As for other terrestrial worlds, most graben likely represent an hourglass-shaped subsurface pattern (Schultz et al 2007). And as for Mercury and the Moon, wrinkle ridges (Figs 7f & 9h) are very common landforms on the Martian surface once more interpreted as arcuate, asymmetric ridges that have formed above an underlying, low-angle thrust fault.…”

“…Plescia & Saunders 1982;Schultz et al 2007), reverse (e.g. Schultz & Tanaka 1994) and strike-slip senses of movement (Andrews-Hanna et al 2008;Yin 2012) (Fig.…”