Ring faults and ring dikes around the Orientale basin on the Moon

Andrews-Hanna, J. C.; Head, J. W.; Johnson, Brandon C.; Keane, J. T.; Kiefer, W. S.; McGovern, P. J.; Neumann, Gregory A.; Wieczorek, M. A.; Zuber, M. T.

doi:10.1016/j.icarus.2017.12.012

Cited by 34 publications

(52 citation statements)

References 74 publications

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“…Both of these characteristics are consistent with normal faults cutting through the crust‐mantle interface (Andrews‐Hanna et al, ; Zuber et al, ). The topography of Orientale's innermost ring, the Inner Rook located at R ≈ 230 km, indicates that it is related to the peak rings of smaller basins (Andrews‐Hanna et al, ; Nahm et al, ).…”

Section: Introductionsupporting

confidence: 66%

“…Johnson et al () found that the Outer Rook and Cordillera, the outer rings of Orientale, are large normal faults that form during crater collapse. These faults offset the crust‐mantle interface and locally thin the crust consistent with constraints from GRAIL gravity (Andrews‐Hanna et al, ; Zuber et al, ). In the simulations of Johnson et al () faults formed as the result of inward flow of warm and weak mantle material during collapse of the transient cavity.…”

Section: Introductionsupporting

confidence: 62%

“…Orientale has three well‐defined topographic rings. Orientale's outer two rings, the Outer Rook and Cordillera, located at R ≈ 310 and 460 km (Andrews‐Hanna et al, ), respectively, appear to be large fault scarps (Nahm et al, ). High‐resolution gravity data from Gravity Recovery and Interior Laboratory reveal that the Outer Rook and Cordillera have locally thinned the crust and offset the crust‐mantle interface (Andrews‐Hanna et al, ; Zuber et al, ).…”

Section: Introductionmentioning

confidence: 99%

“…Orientale's outer two rings, the Outer Rook and Cordillera, located at R ≈ 310 and 460 km (Andrews‐Hanna et al, ), respectively, appear to be large fault scarps (Nahm et al, ). High‐resolution gravity data from Gravity Recovery and Interior Laboratory reveal that the Outer Rook and Cordillera have locally thinned the crust and offset the crust‐mantle interface (Andrews‐Hanna et al, ; Zuber et al, ). Both of these characteristics are consistent with normal faults cutting through the crust‐mantle interface (Andrews‐Hanna et al, ; Zuber et al, ).…”

Section: Introductionmentioning

confidence: 99%

“…High‐resolution gravity data from Gravity Recovery and Interior Laboratory reveal that the Outer Rook and Cordillera have locally thinned the crust and offset the crust‐mantle interface (Andrews‐Hanna et al, ; Zuber et al, ). Both of these characteristics are consistent with normal faults cutting through the crust‐mantle interface (Andrews‐Hanna et al, ; Zuber et al, ). The topography of Orientale's innermost ring, the Inner Rook located at R ≈ 230 km, indicates that it is related to the peak rings of smaller basins (Andrews‐Hanna et al, ; Nahm et al, ).…”

Section: Introductionmentioning

confidence: 99%

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Controls on the Formation of Lunar Multiring Basins

et al. 2018

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Multiring basins dominate the crustal structure, tectonics, and stratigraphy of the Moon.Understanding how these basins form is crucial for understanding the evolution of ancient planetary crusts. To understand how preimpact thermal structure and crustal thickness affect the formation of multiring basins, we simulate the formation of lunar basins and their rings under a range of target and impactor conditions. We find that ring locations, spacing, and offsets are sensitive to lunar thermal gradient (strength of the lithosphere), temperature of the deep lunar mantle (strength of the asthenosphere), and preimpact crustal thickness. We also explore the effect of impactor size on the formation of basin rings and reproduce the observed transition from peak-ring basins to multiring basins and reproduced many observed aspects of ring spacing and location. Our results are in broad agreement with the ring tectonic theory for the formation of basin rings and also suggest that ring tectonic theory applies to the rim scarp of smaller peak-ring basins.Plain Language Summary The largest impact craters on the Moon are multiring basins that exhibit three or more topographic rings. Great volumes of material were ejected and redistributed during the formation of these 1,000-km-scale basins. Formation of these basins is the predominant process driving change of the lunar crust, the outermost layer of the Moon. Why large basins have multiple topographic rings and what they might tell us about the Moon remain poorly understood. Here we simulate the formation of these basins and their rings during an asteroid impact. We explore how thickness of the lunar crust, size of the impacting body, and interior temperature of the Moon affect the formation of basins and their rings. With well-persevered multiring basins and an abundance of high-quality gravity and topography data, the Moon is an ideal location to explore the formation of multiring basins. A better understanding of the formation of these basins will help us understand how similar basins may have affected the crusts of the Earth, Mars, Mercury, and Venus.Other than the 2,000-km-scale elliptical South Pole-Aitken basin Key Points:• We simulate the formation of multiring basins exploring the effect of impactor size, target thermal structure, and crustal thickness • Our simulations reproduce observed trends in ring spacing including the transition from peak-ring to multiring structures • Our results show that basin ring formation is quite sensitive to target thermal structure in general agreement with ring tectonic theory

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Section: Introductionsupporting

confidence: 66%