Model Estimates of Non-Hydrostatic Stresses in the Martian Crust and Mantle: 1—Two-Level Model

Гудкова, Т. В.; Batov, A. V.; Жарков, В. Н.

doi:10.1134/s003809461706003x

Cited by 18 publications

(4 citation statements)

References 48 publications

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“…With respect to point 2, Searls and Phillips (2007) used finite element modeling to demonstrate that global tectonic compression is necessary to create the radial and concentric faults observed around Utopia Planitia. Similar results were obtained by Gudkova et al (2017). Lastly, concerning point 3, for the Utopia Planitia region, the average material density is ~2700 kg m -3 (Searls and Phillips, 2007), the gravitational acceleration on Mars is 3.711 m s -2 , and the land surface has a slope of 0.1°…”

Section: Implications For Planetary Geologysupporting

confidence: 72%

Sheeting joints and polygonal patterns in the Navajo Sandstone, southern Utah: Controlled by rock fabric, tectonic joints, buckling, and gullying

Loope

Burberry

2018

Geosphere

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Sheeting joints are ubiquitous in outcrops of the Navajo Sandstone on the west-central Colorado Plateau, USA. As in granitic terrains, these are opening-mode fractures and form parallel to land surfaces. In our study areas in south-central Utah, liquefaction during Jurassic seismic events destroyed stratification in large volumes of eolian sediment, and first-order sheeting joints are now preferentially forming in these structureless (isotropic) sandstones. Vertical cross-joints abut the land-surface-parallel sheeting joints, segmenting broad (tens of meters) rock sheets into equant, polygonal slabs ~5 m wide and 0.25 m thick. On steeper slopes, exposed polygonal slabs have domed surfaces; eroded slabs reveal an onion-like internal structure formed by 5-m-wide, second-order sheeting joints that terminate against the crossjoints, and may themselves be broken into polygons. In many structureless sandstone bodies, however, the lateral extent of first-order sheeting joints is severely limited by pre-existing, vertical tectonic joints. In this scenario, non-conjoined sheeting joints form extensive agglomerations of laterally contiguous, polygonal domes 3-6 m wide, exposing exhumed sheeting joints. These laterally confined sheeting joints are, in turn, segmented by short vertical cross-joints into numerous small (~0.5 m) polygonal rock masses. We hypothesize that the sheeting joints in the Navajo Sandstone form via contemporaneous, land-surface-parallel compressive stresses, and that vertical cross-joints that delineate polygonal masses (both large and small) form during compression-driven buckling of thin, convex-up rock slabs. Abrasion of friable sandstone during runoff events widens vertical tectonic joints into gullies, enhancing land-surface convexity. Polygonal rock slabs described here provide a potential model for interpretation of similar-appearing patterns developed on the surface of Mars.

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Section: Implications For Planetary Geologysupporting

confidence: 72%

Sheeting joints and polygonal patterns in the Navajo Sandstone, southern Utah: Controlled by rock fabric, tectonic joints, buckling, and gullying

Loope

Burberry

2018

Geosphere

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“…VM is amongst the largest canyons in the solar system (Coles et al, 2019). Together with the Tharsis province, it has been proposed as one of the most seismically active regions on Mars, supported by both surface faulting observations (Golombek et al, 1992) and joint inversion of gravity and topography data (Gudkova et al, 2017). Furthermore, in an analysis of boulder falls in VM, Senthil Kumar et al (2019) suggest that the region must have been seismically active in its recent past.…”

Section: Distant Events Clustermentioning

confidence: 93%

Mapping the Seismicity of Mars With InSight

Ceylan,

Giardini,

Clinton

et al. 2023

JGR Planets

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The InSight seismometers have recorded more than 1300 events. Ninety‐eight of these, named the low‐frequency family, show energy predominantly below 1 Hz down to ∼0.1 Hz. The Marsquake Service identified seismic phases and computed distances for 42 of these marsquakes, 24 of which have backazimuths. Hence, the locations of the majority of low‐frequency family events remain undetermined. Here, we use an envelope shape similarity approach to determine event classes and distances, and introduce an alternative method to estimate the backazimuth. In our analysis, we use the highest quality marsquakes with known distances as templates, including the largest event S1222a, and assign new distances to similar group of events for which distance estimates were not previously available. We find the Tharsis region to be more active than initially perceived on the basis of 5 newly located events near Valles Marineris and Olympus Mons. We relocate two marsquakes with little or no S‐wave energy in the NE of the Elysium Bulge. The event epicenters in Cerberus Fossae follow a north‐south trend due to uncertainties in location, while the fault system is in the NW‐SE direction; therefore, these events are re‐projected along the observed fault system based on our interpretations. The marsquakes in our interpreted catalog are predominantly observed in the northern hemisphere of Mars above the equatorial dichotomy boundary.

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“…12 do not include the contribution of stresses produced by lithospheric flexure due to loading. Tensile-compressive stresses as well as shear stresses distribution in the martian lithosphere correlate with surface structures and can affect the seismic moment distribution in particular in areas such as Tharsis, Hellas Planitia, Argyre Planitia, Acidalia Planitia, Arcadia Planitia, and Valles Marineris (Gudkova et al, 2017;Batov et al, 2018). In addition, although the seismicity distribution Fig.…”

Section: Isothermmentioning

confidence: 99%

Interior Dynamics and Thermal Evolution of Mars -- a Geodynamic Perspective

Plesa¹,

Wieczorek²,

Knapmeyer³

et al. 2022

Preprint

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Over the past decades, global geodynamical models have been used to investigate the thermal evolution of terrestrial planets. With the increase of computational power and improvement of numerical techniques, these models have become more complex, and simulations are now able to use a high resolution 3D spherical shell geometry and to account for strongly varying viscosity, as appropriate for mantle materials. In this study we review global 3D geodynamic models that have been used to study the thermal evolution and interior dynamics of Mars. We discuss how these models can be combined with local and global observations to constrain the planet's thermal history. In particular, we use the recent InSight estimates of the crustal thickness, upper mantle structure, and core size to show how these constraints can be combined with 3D geodynamic models to improve our understanding of the interior dynamics, present-day thermal state and temperature variations in the interior of Mars. Our results show that the crustal thickness variations control the surface heat flow and the elastic thickness pattern, as well as the location of melting zones in the present-day martian mantle. The lithospheric temperature and the seismic velocities pattern in the shallow mantle reflect the crustal thickness pattern. The large size of the martian core leads to a smaller scale convection pattern in the mantle than previously suggested. Strong mantle plumes that produce melt up to recent times become focused in Tharsis and Elysium, while weaker plumes are distributed throughout the mantle. The thickness of the seismogenic layer, where seismic events can occur, can be used to discriminate between geodynamic models, if the source depth and location of seismic events is known. Furthermore model predictions of present-day martian seismicity can be compared to the values measured by InSight. Future models need to consider recent estimates from the presentday elastic lithosphere thickness at the north pole of Mars, the effects of lateral variations of seismic velocities on waves propagation through the mantle and lithosphere, and to test the spatial distribution of seismicity by comparing model predictions to observations.

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Model Estimates of Non-Hydrostatic Stresses in the Martian Crust and Mantle: 1—Two-Level Model

Cited by 18 publications

References 48 publications

Sheeting joints and polygonal patterns in the Navajo Sandstone, southern Utah: Controlled by rock fabric, tectonic joints, buckling, and gullying

Sheeting joints and polygonal patterns in the Navajo Sandstone, southern Utah: Controlled by rock fabric, tectonic joints, buckling, and gullying

Mapping the Seismicity of Mars With InSight

Interior Dynamics and Thermal Evolution of Mars -- a Geodynamic Perspective

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