Drop Height and Volume Control the Mobility of Long‐Runout Landslides on the Earth and Mars

Johnson, Brandon C.; Campbell, Charles S.

doi:10.1002/2017gl076113

Cited by 38 publications

(42 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Runs with no reported particle size assume D = 1 m. Each point represents the result of a landslide simulation. The results for Earth and Mars surface gravity were reported previously byJohnson et al (2016) andJohnson and Campbell (2017). Note g Earth = 9.8 m/s 2 , g Mars = 3.7 m/s 2 , and g Ceres = 0.27 m/s 2 .…”

supporting

confidence: 79%

Landslide Morphology and Mobility on Ceres Controlled by Topography

Johnson

Sori

2020

JGR Planets

Self Cite

View full text Add to dashboard Cite

Ceres is a dwarf planet, is the largest body in the asteroid belt, and was one of the targets of the NASA's Dawn mission (Russell et al., 2016). There is abundant evidence that Ceres is a relatively water rich body. The relatively low bulk density of Ceres (2,162 kg/m 3) is indicative of a water content of about 25% (Thomas et al., 2005). At the surface, ice is unstable at most locations and will quickly sublimate (Hayne & Aharonson, 2015; Landis et al., 2017), but has been detected in permanently shadowed regions at the poles (Platz et al., 2017) and at fresh exposures in Oxo crater (Combe et al., 2016). Hazes produced by sublimation have been proposed to be detected (Nathues et al., 2015). In the very shallow subsurface (tens of centimeters), observations by Dawn's Gamma Ray and Neutron Detector (GRaND) suggest there is abundant ice and hydrated minerals that follows the expected latitudinal pattern predicted by thermal models of ice stability (Prettyman et al., 2017); that is, shallower ice at high latitudes. Despite the evidence of abundant water on Ceres, constraints on ice content and how it varies with location and depth beyond the upper meter that is sensitive to GRaND's nuclear spectroscopy are limited. The outer crust of Ceres is thought to be a complex mixture of ice, phyllosilicates, hydrated salts, and/or clathrates. Initial two-layer models of a partially differentiated Ceres constrained by Dawn gravity indicate that Ceres has a 70-190 km thick outer crust with a density of 1,680-1,950 kg/m 3 , substantially denser than the 930 kg/m 3 value expected for pure ice (Park et al., 2016). Subsequent analysis, performed as more geophysical observations were taken, refine these numbers to best fit values of 41 km for crustal thickness and 1,287 kg/m 3 for crustal density (Ermakov et al., 2017), and most recently to 41 km and 1,233 kg/m 3

show abstract

supporting

confidence: 79%

Landslide Morphology and Mobility on Ceres Controlled by Topography

Johnson

Sori

2020

JGR Planets

Self Cite

View full text Add to dashboard Cite

show abstract

“…20 • (Farin et al, 2014;Borykov et al, 2019), whereas it has no influence for more gentle slopes. This dependency of landslide propagation on slope, and indirectly on volume (and friction), initially identified in lab- oratory experiments (Farin et al, 2014) could be adequately documented by natural examples thanks to some very large Martian landslides (Johnson and Campbell, 2017;Borykov et al, 2019), much larger than any terrestrial landslide, which help populate the landslide dataset for voluminous landslides that propagate on nearly flat surfaces. Similar to landslides, DSGSD occurs on mountain slopes that are much smaller on Earth than on Mars, and at the first order, their origin may be similar.…”

Section: Scaling Of Processes Involved In Deep-seated Gravitational Smentioning

confidence: 73%

“…Although similar at first order, landslide propagation is not controlled by the same parameters because the landslide slope is different. It was shown that landslide volume is one of the factors that control landslide propagation (McEwen, 1989;Lucas et al, 2014;Johnson and Campbell, 2017) when the slope angle of the propagation plane is steeper than ca. 20 • (Farin et al, 2014;Borykov et al, 2019), whereas it has no influence for more gentle slopes.…”

Section: Scaling Of Processes Involved In Deep-seated Gravitational Smentioning

confidence: 99%

Deep-seated gravitational slope deformation scaling on Mars and Earth: same fate for different initial conditions and structural evolutions

et al. 2019

View full text Add to dashboard Cite

Abstract. Some of the most spectacular instances of deep-seated gravitational slope deformation (DSGSD) are found on Mars in the Valles Marineris region. They provide an excellent opportunity to study DSGSD phenomenology using a scaling approach. The topography of selected DSGSD scarps in Valles Marineris and in the Tatra Mountains is investigated after their likely similar postglacial origin is established. The deformed Martian ridges are larger than the deformed terrestrial ridges by 1 to 2 orders of magnitude with, however, a similar height-to-width ratio of ∼0.24. The measured horizontal spreading perpendicular to the ridges is proportionally 1.8 to 2.6 times larger for the Valles Marineris ridges than the Tatra Mountains and vertically 2.9 to 5.1 times larger, suggesting that starting from two different initial conditions, with steeper slopes in Valles Marineris, the final ridge geometry is now similar. Because DSGSD is expected to now be inactive in both regions, their comparison suggests that whatever the initial ridge morphology, DSGSD proceeds until a mature profile is attained. Fault displacements are therefore much larger on Mars. The large offsets imply reactivation of the DSGSD fault scarps in Valles Marineris, whereas single seismic events would be enough to generate DSGSD fault scarps in the Tatra Mountains. The required longer activity of the Martian faults may be correlated with a long succession of climate cycles generated by the unstable Martian obliquity.

show abstract

“…Accordingly, our research team proposed that thermal pressurization induced by frictional heating may be a key factor in the frictional weakening of the avalanche basal facies samples, which provides insight into rock avalanche hypermobility mechanisms. This discovery brings to mind another rock avalanche feature revealed by field data statistics: the reduction of Fahrböschung with increasing rock avalanche volume, that is, rock avalanche volume effect (Johnson & Campbell, ; Legros, ; Lucas et al, ; Pudasaini & Miller, ).…”

Section: Introductionmentioning

confidence: 98%

Normal Stress‐Dependent Frictional Weakening of Large Rock Avalanche Basal Facies: Implications for the Rock Avalanche Volume Effect

2018

View full text Add to dashboard Cite

To explore the mechanism behind the volume effect of rock avalanches observed in field data, a series of rotary shear tests were conducted at a shearing velocity of 0.87 m/s and varying normal stress levels (from 0.29 to 1.85 MPa) on soil collected from the basal facies of the Yigong rock avalanche in Tibet, China. This experimental study reveals that (1) as normal stress increases, the steady state apparent friction coefficient (μss) of the soil decreases, indicating a normal stress‐dependent feature of μss; (2) the higher the normal stress, the lower the decay rate of μss; (3) water vaporization induced by frictional heating is commonly observed in the tests accompanied by large decreases in μss, and excess pore pressure is generated in the shearing zones of the samples due to vapor accumulation; and (4) with increases in normal stress and decreases in soil permeability, an increasing feature of excess pore pressure is reached. Based on the experimental results, we propose that the coupled effects of water vaporization induced by frictional heating in avalanche basal facies and depth‐dependent permeability of avalanche basal facies should be contributed to the volume effect of rock avalanches.

show abstract

Drop Height and Volume Control the Mobility of Long‐Runout Landslides on the Earth and Mars

Cited by 38 publications

References 37 publications

Landslide Morphology and Mobility on Ceres Controlled by Topography

Landslide Morphology and Mobility on Ceres Controlled by Topography

Deep-seated gravitational slope deformation scaling on Mars and Earth: same fate for different initial conditions and structural evolutions

Normal Stress‐Dependent Frictional Weakening of Large Rock Avalanche Basal Facies: Implications for the Rock Avalanche Volume Effect

Contact Info

Product

Resources

About