Effects of dispersed particulates on the rheology of water ice at planetary conditions

Durham, W. B.; Kirby, Stephen H.; Stern, Laura A.

doi:10.1029/92je02326

Cited by 153 publications

(187 citation statements)

References 28 publications

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“…0.80 samples, a measured amount of liquid water and sand were loosely mixed (think sand castles), then molded and frozen. After fabrication, samples were sealed in indium tubes of 0.5-mm wall thickness, loaded into our high-pressure cryogenic creep apparatus [Durham et al, 1992], pressurized with N 2 gas as the confining medium, and deformed axially in compression at constant differential stress (creep).…”

Section: Rheology Of Icy Sand Packs At Planetary Conditionsmentioning

confidence: 99%

“…[5] We previously conducted measurements of the rheological properties of ice-rich mixtures ranging from 42% to 100% ice by volume [Durham et al, 1992]. Recent studies have explored the brittle-to-ductile transition of sand-rich mixtures, with application to very near-surface planetary features [Mangold et al, 2002;Yasui and Arakawa, 2008].…”

Section: Introductionmentioning

confidence: 99%

“…Non-mobile samples: as measured; mobile samples: extrapolated based on estimated transient strain + 10 6 Á _ e ss at std conds (details in Table S1). tude [Durham et al, 1992], at f > 0.58 viscosity increases by at least another two orders of magnitude over a fairly small interval of f (dot-dashed lines in Figure 2 inset).…”

mentioning

confidence: 99%

“…Whereas viscosity in the interval 0 f 0.58 (dashed line in Figure 2 inset) is linear in log space and gradual, spanning approximately two orders of magni- , n = 4, Q = 61 kJ/mol, R = 8.31 J/mol Á K [Durham et al, 1992]. Non-mobile samples: as measured; mobile samples: extrapolated based on estimated transient strain + 10 6 Á _ e ss at std conds (details in Table S1).…”

mentioning

confidence: 99%

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Mobility of icy sand packs, with application to Martian permafrost

Durham¹,

Pathare²,

Stern³

et al. 2009

Geophysical Research Letters

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The physical state of water on Mars has fundamental ramifications for both climatology and astrobiology. The widespread presence of “softened” Martian landforms (such as impact craters) can be attributed to viscous creep of subsurface ground ice. We present laboratory experiments designed to determine the minimum amount of ice necessary to mobilize topography within Martian permafrost. Our results show that the jammed‐to‐mobile transition of icy sand packs neither occurs at fixed ice content nor is dependent on temperature or stress, but instead correlates strongly with the maximum dry packing density of the sand component. Viscosity also changes rapidly near the mobility transition. The results suggest a potentially lower minimum volatile inventory for the impact‐pulverized megaregolith of Mars. Furthermore, the long‐term preservation of partially relaxed craters implies that the ice content of Martian permafrost has remained close to that at the mobility transition throughout Martian history.

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Section: Rheology Of Icy Sand Packs At Planetary Conditionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Mobility of icy sand packs, with application to Martian permafrost

Durham¹,

Pathare²,

Stern³

et al. 2009

Geophysical Research Letters

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“…All else being equal, the thickness of the granular material is somewhat proportional to the overlain ice thickness. Like most current ice dynamic models, our modelling framework supports Glen [34], Goldsby and Kohlstedt [35], and Durham's [36] flow laws. Ice sheet mass balance is simply the difference between whatever goes in and whatever comes out.…”

Section: Ice Dynamics Modelmentioning

confidence: 99%

A new ice sheet model validated by remote sensing of the Greenland ice sheet

Ren

Karoly

et al. 2010

Open Geosciences

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Accurate prediction of future sea level rise requires models that accurately reproduce and explain the recent observed dramatic ice sheet behaviours. This study presents a new multi-phase, multiple-rheology, scalable and extensible geofluid model of the Greenland ice sheet that shows the credential of successfully reproducing the mass loss rate derived from the Gravity Recovery and Climate Experiment (GRACE), and the microwave remote sensed surface melt area over the past decade. Model simulated early 21st century surface ice flow compares satisfactorily with InSAR measurements. Accurate simulation of the three metrics simultaneously cannot be explained by fortunate model tuning and give us confidence in using this modelling system for projection of the future fate of Greenland Ice Sheet (GrIS). Based on this fully adaptable three dimensional, thermo-mechanically coupled prognostic ice model, we examined the flow sensitivity to granular basal sliding, and further identified that this leads to a positive feedback contributing to enhanced mass loss in a future warming climate. The rheological properties of ice depend sensitively on its temperature, thus we further verified modelâ€Źs temperature solver against in situ observations. Driven by the NCEP/NCAR reanalysis atmospheric parameters, the ice model simulated GrIS mass loss rate compares favourably with that derived from the GRACE measurements, or about -147 km 3 /yr over the 2002-2008 period. Increase of the summer maximum melt area extent (SME) is indicative of expansion of the ablation zone. The modeled SME from year 1979 to 2006 compares well with the cross-polarized gradient ratio method (XPGR) observed melt area in terms of annual variabilities. A high correlation of 0.88 is found between the two time series. In the 30-year model simulation series, the surface melt exhibited large inter-annual and decadal variability, years 2002, 2005 and 2007 being three significant recent melt episodes.

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Compositional diapirism as the origin of the low‐albedo terrain and vaporization at midlatitude on Ceres

Dake

Kurita

2014

JGR Planets

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Recent observations of Ceres, made using the Heterodyne Instrument for the Far Infrared on board the European Space Agency's Herschel Space Observatory, have shown that water vapor is emanated from the low‐albedo midlatitude regions. Based on the supposition that some dark spots on Europa may be caused by diapirism, we explored whether Ceres' environment also can induce compositional diapirism, and whether an upwelling diapir could explain the origin and distribution of the dark spots and vaporization of Ceres. If the density of the rock that constitutes Ceres is around 2700 kg m−3, the undifferentiated crust is stable over geological time periods at less than 180 K. At a surface temperature of 170 K, a diapir can reach the surface if the crust is a few tens of kilometers thick. Alternatively, if the surface temperature is 150 K, a large contrast in viscosity would prevent diapirs from reaching the surface. The relatively moderate surface temperature in the midlatitude regions of Ceres may be the reason for the formation of dark terrains occurring only in such areas. Our finite difference calculations do not show that diapirism melts the surface ice because the temperature gradient changes very little. However, if the observed vapor emission is caused by the sublimation of fresh ice, compositional diapirism could be the mechanism that transports the fresh ice to the surface. In addition to other mechanisms such as cryovolcanism, diapirism is a valid hypothesis for explaining the dark terrain and vapor emissions of Ceres.

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Effects of dispersed particulates on the rheology of water ice at planetary conditions

Cited by 153 publications

References 28 publications

Mobility of icy sand packs, with application to Martian permafrost

Mobility of icy sand packs, with application to Martian permafrost

A new ice sheet model validated by remote sensing of the Greenland ice sheet

Compositional diapirism as the origin of the low‐albedo terrain and vaporization at midlatitude on Ceres

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