Morphometric analysis of a Hesperian aged Martian lobate scarp using high-resolution data

Ruj, Trishit; Komatsu, G.; Pondrelli, M.; Pietro, Ilaria Di; Pozzobon, Riccardo

doi:10.1016/j.jsg.2018.04.018

Cited by 10 publications

(7 citation statements)

References 62 publications

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“…Assuming planar fault geometries dipping at 30°, the average D max /L ratio determined for these 49 thrust faults is 6.1 × 10 −3 . This value is comparable to other global ratios found for thrust faults on Mars, ranging from 4.5 × 10 −3 to 6.2 × 10 -3 (Ruj et al, 2018;Schultz et al, 2006;Watters & Robinson, 1999;Watters et al, 1998Watters et al, , 2000. Results from our investigation show significantly different D max /L ratios (Figure 6) for the northern lowlands (n = 24; D max /L = 2.9 × 10 −3 ) and the southern highlands (n = 25; D max /L = 9.2 × 10 −3 ).…”

Section: Displacement-length Scaling Ratiossupporting

confidence: 88%

“…Decreasing the fault dip angle to 25° increases the mean D max /L to 6.2 × 10 −3 , and increasing the assumed dip angle to 35° decreases the ratio to 4.6 × 10 −3 . These values are within the range published for other Martian thrust faults of 4.5 × 10 −3 to 6.2 × 10 -3 (Ruj et al, 2018;Schultz et al, 2006;Watters & Robinson, 1999;Watters et al, 1998Watters et al, , 2000. Lengths of measured faults are similar between the structures in the northern and southern hemispheres, with median lengths of 211.5 and 141.0 km, respectively.…”

Section: Displacement-length Scalingsupporting

confidence: 84%

“…Displacement-length ratios of Earth-based thrust faults are typically 1.0-8.0 × 10 −2 (Davis et al, 2005;Manighetti et al, 2009Manighetti et al, , 2015Watters et al, 2000). The D max /L for thrust faults on Mars have been reported as 4.5-6.2 × 10 -3 (Ruj et al, 2018;Schultz et al, 2006;Watters, 2003;Watters & Robinson, 1999;Watters et al, 1998Watters et al, , 2000. Thrust faults on Mercury exhibit D max /L ratios of 6.0-9.0 × 10 −3 (Byrne et al, 2014;Watters, 2021).…”

Section: Displacement-length Scalingmentioning

confidence: 99%

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A Morphometric Investigation of Large‐Scale Crustal Shortening on Mars

et al. 2022

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Mars' surface exhibits abundant topographic expressions of large thrust fault‐related folds that have been attributed to global planetary contraction. Morphometric analyses of such structures provide insight into their growth history. With global THEMIS imagery and HRSC–MOLA topographic data, 49 thrusts with lengths between 35 and 544 km were mapped across Mars' surface. Assuming planar fault geometries with dips of 30°, the average maximum displacement‐length ratio (Dmax/L) of these structures is 6.1 × 10−3 ± 1.4 × 10−3, with smaller ratios observed for faults within the northern lowlands (2.9 × 10−3 ± 0.9 × 10−3) compared to the southern highlands (9.2 × 10−3 ± 1.9 × 10−3). However, these differences may be accounted for if mechanical layering in the northern lowland crust promotes either a shallowing of the fault dip angle relative to the southern highlands or the development of ramp‐flat geometries such that the topographic scarp height may under‐estimate the total fault displacement or a combination of these two scenarios together. Alternatively, these Dmax/L patterns may reflect hemispheric differences in the brittle‐ductile transition (BDT) depth; however, the observed pattern is stratigraphically inconsistent with the Martian crustal dichotomy, whereby the northern lowlands have thinner (or denser) crust and therefore presumably a deeper BDT than the southern highlands. Fault displacement‐length profiles are commonly asymmetric, with multiple local minima observed along their lengths. Spectral analysis of these profiles, using Fourier‐ and S‐Transforms, indicates power at a range of spatial frequencies, reflecting complex growth and linkage histories, with peak spectral frequency, or number of segments, being negatively correlated with the Dmax/L ratios.

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Section: Displacement-length Scaling Ratiossupporting

confidence: 88%

Section: Displacement-length Scalingsupporting

confidence: 84%

Section: Displacement-length Scalingmentioning

confidence: 99%

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A Morphometric Investigation of Large‐Scale Crustal Shortening on Mars

et al. 2022

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“…Mosaiced CTX images superimposed with MOLA-HRSC DEM/DTM images can be utilized, enabling separation, model drawing, and understanding 3D aspects for making elevation profiles and cross-section profiles particularly to measure topographic relief and mark the geomorphic units in the study area. The mosaiced CTX images can also be used in morphometric analysis [14] of Martian drainage basins, particularly in identification, characterization, and classification of landforms to know their origin, i.e., fluvial, volcanic, or structural…”

Section: Discussion and Applicationsmentioning

confidence: 99%

A New Method of Mosaicking Context Camera (CTX) Images for the Geomorphological Study of Martian Landscape

Chavan¹,

Sarkar²,

Thakkar³

et al. 2021

OJG

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Various spacecraft and satellites from the world's best space agencies are exploring Mars since 1970, constantly with great ability to capture the maximum amount of dataset for a better understanding of the red planet. In this paper, we propose a new method for making a mosaic of Mars Reconnaissance Orbiter (MRO) spacecraft payload Context Camera (CTX) images. In this procedure, we used ERDAS Imagine for image rectification and mosaicking as a tool for image processing, which is a new and unique method of generating a mosaic of thousands of CTX images to visualize the large-scale areas. The output product will be applicable for mapping of Martian geomorphological features, 2D mapping of the linear feature with high resolution, crater counting, and morphometric analysis to a certain extent.

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“…A trailing syncline and a frontal syncline are usually present on each side of the anticline (e.g., Grott et al, ; Herrero‐Gil et al, , ; Schultz, ; Schultz & Watters, ). The large thrust faults underlying lobate scarps have been studied and modeled by several authors on different terrestrial bodies like Mars (e.g., Egea‐González et al, ; Grott et al, ; Herrero‐Gil et al, , ; Klimczak et al, ; Mueller et al, ; Ruiz et al, ; Ruj et al, ; Schultz & Watters, ), Mercury (e.g., Crane & Klimczak, ; Egea‐González et al, ; Galluzzi et al, , ; Giacomini et al, ; Semenzato et al, ; Watters et al, ), the Moon (e.g., Byrne et al, ; Williams et al, ), Ceres (Ruiz et al, ), and asteroid 433 Eros (Watters et al, ). These works usually include the study of the timing of faulting and the analysis of the structural parameters that define the fault morphology and kinematics (depth of faulting, dip angle and fault slip), with the final aim of advancing on the knowledge of the tectonic and thermal evolution of these terrestrial bodies.…”

Section: Introductionmentioning

confidence: 99%

Lithospheric Contraction on Mars: A 3D Model of the Amenthes Thrust Fault System

2020

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Amenthes Rupes is the topographic expression of a main fault belonging to a thrust fault system located parallel to the martian dichotomy boundary. A 3D forward model has been applied to the Amenthes thrust fault system, constraining fault geometries at depth, variations of slip along strike, and structural parameters controlling the formation of fault propagation folds. Our results provide a complex 3D view of the tectonic framework of the area, with implications for tectonic evolution, regional shortening distribution, and the main mechanical discontinuities in the lithosphere. The modeled fault surfaces show planar morphologies combined with listric geometries at depth. The obtained depths of faulting for the major faults of this fault system suggest a depth of the brittle‐ductile transition (at the time of formation) of 20–24 km, somewhat shallower than previous estimates for this area. A possible mechanical discontinuity located at 10.5–13 km deep can be deduced from the faulting depths of the secondary faults. The listric geometries at depth imply that slip is transmitted from the decollement, which, together with the inclusion in the model of secondary and subsidiary faults, allow us to estimate the horizontal shortening recorded in this area ranging from 2–3 km up to ~5.5 km in the southeastern part of the fault system. This range increases the previous shortening estimates in this area between ~60% and ~200%. Consequently, global shortening estimates based on global fault maps are biased by the detail of mapping, and shortening would substantially increase if secondary faults were included.

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Morphometric analysis of a Hesperian aged Martian lobate scarp using high-resolution data

Cited by 10 publications

References 62 publications

A Morphometric Investigation of Large‐Scale Crustal Shortening on Mars

A Morphometric Investigation of Large‐Scale Crustal Shortening on Mars

A New Method of Mosaicking Context Camera (CTX) Images for the Geomorphological Study of Martian Landscape

Lithospheric Contraction on Mars: A 3D Model of the Amenthes Thrust Fault System

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