The fracture of water ice Ih: A short overview

Schulson, E. M.

doi:10.1111/j.1945-5100.2006.tb00432.x

Cited by 28 publications

(19 citation statements)

References 70 publications

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“…Similar enhancements in stress were identified in models of Charon that included low viscosity underlying ice layers [ Rhoden et al ., ]. These stresses are an order of magnitude larger than those associated with fracture formation on Europa [ Kattenhorn and Hurford , ] and approach or exceed the failure strength of water ice in laboratory tests [ Schulson , ; Collins et al ., ]. Based on these values, we would expect Mimas' surface to be globally fractured in the presence of a subsurface ocean.…”

Section: Resultsmentioning

confidence: 99%

“…Yin and Pappalardo, 2015). For initial estimates of tidal stresses on Enceladus, the Love number, h 2 , which controls the tidal stress magnitude, was selected to fit proposed models [e.g., Hurford et al, 2007;Nimmo et al, 2007]. In contrast, Behounkova et al [2015] calculated tidal stresses for a variety of plausible interiors of Enceladus using a viscoelastic model, similar to the approach we have applied here to Mimas.…”

Section: 1002/2016je005097mentioning

confidence: 99%

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The implications of tides on the Mimas ocean hypothesis

et al. 2017

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We investigate whether a present‐day global ocean within Mimas is compatible with the lack of tectonic activity on its surface by computing tidal stresses for ocean‐bearing interior structure models derived from observed librations. We find that, for the suite of compatible rheological models, peak surface tidal stresses caused by Mimas' high eccentricity would range from a factor of 2 smaller to an order of magnitude larger than those on tidally active Europa. Thermal stresses from a freezing ocean, or a past higher eccentricity, would enhance present‐day tidal stresses, exceeding the magnitudes associated with Europa's ubiquitous tidally driven fractures and, in some cases, the failure strength of ice in laboratory studies. Therefore, in order for Mimas to have an ocean, its ice shell cannot fail at the stress values implied for Europa. Furthermore, if Mimas' ocean is freezing out, the ice shell must also be able to withstand thermal stresses that could be an order of magnitude higher than the failure strength of laboratory ice samples. In light of these challenges, we consider an ocean‐free Mimas to be the most straightforward model, best supported by our tidal stress analysis.

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Section: Resultsmentioning

confidence: 99%

Section: 1002/2016je005097mentioning

confidence: 99%

The implications of tides on the Mimas ocean hypothesis

et al. 2017

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“…Alternatively, buoyancy from gas exsolution may allow water to rise further into the ice shell [Crawford and Stevenson, 1988] and these gases would separate from the water once the sill is emplaced. Freezing of isolated water bodies [Fagents, 2003], including water generated in or above diapirs [Sotin et al, 2002;Pappalardo and Barr, 2004;Schmidt et al, 2011], should be able to produce overpressures up to values comparable to the tensile strength of ice, about 1 − 3 × 10 6 Pa [Schulson, 2006], and hence large enough to make the hypothesized sills. However, the water reservoir must also be large enough to supply enough water while maintaining a high pressure.…”

Section: Discussionmentioning

confidence: 99%

Domes, pits, and small chaos on Europa produced by water sills

2014

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Key Points:• The spreading of water sills is limited by ice fracturing • Deep sills can thicken significantly in contrast to shallow sills • Pits, domes, and small chaos morphology can result from subsequent sill evolution Abstract Pits, domes, and small chaos on Europa's surface are quasi-circular features a few to a few tens of kilometers in diameter. We examine if injection of water sills into Europa's ice shell and their subsequent evolution can induce successive surface deformations similar to the morphologies of these features. We study the dynamics of water spreading within the elastic part of the ice shell and show that the mechanical properties of ice exert a strong control on the lateral extent of the sill. At shallow depths, water makes room for itself by lifting the overlying ice layer and water weight promotes lateral spreading of the sill. In contrast, a deep sill bends the underlying elastic layer and its weight does not affect its spreading. In that case, the sill lateral extent is limited by the fracture toughness of ice and the sill can thicken substantially. After emplacement, cooling of the sill warms the surrounding ice and thins the overlying elastic ice layer. As a result, preexisting stresses in the elastic part of the ice shell increase locally to the point that they may disrupt the ice above the sill (small chaos). Disruption of the surface also allows for partial isostatic compensation of water weight, leading to a topographic depression at the surface (pit), of the order of ∼10 2 m. Complete water solidification finally causes expansion of the initial sill volume and results in an uplifted topography (dome) of ∼10 2 m.

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“…However, in the case of the low‐viscosity layer extending to the surface (run 2) the stresses generated are relatively low (<0.1 MPa). The tensile strength of crack‐free ice of 1‐mm sized grains is in the order of 1.5 MPa (Schulson, ); thus, a low‐viscosity surface layer is probably not able to generate the observed concentric fractures.…”

Section: Formation Scenarios For Rim Fracturesmentioning

confidence: 99%

Ceres Crater Degradation Inferred From Concentric Fracturing

et al. 2019

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The dwarf planet Ceres exhibits a collection of craters that possess concentric fractures beyond the crater rim. These fractures typically range from a few hundred meters to a few kilometers in length and are less than 300 m wide. They occur preferentially on elevated regions around the crater and are located less than a crater radius beyond the rim. In total there are 17 craters exhibiting concentric fracturing beyond the rim. They are located in the midlatitudes. The craters' diameters range between 20 and 270 km. We investigate the concentric fractures of three craters (Azacca, Ikapati, and Occator) in detail and suggest that the formation of such concentric fractures can be explained by a shallow (<10‐km) low‐viscosity (~1020‐Pa·s) subsurface layer extending underneath the crater and its surroundings. Finite element modeling of such a scenario applied to a typical concentrically fractured crater of 50‐km diameter implies that the depth of the low‐viscosity layer is comparable to the crater depth and the layer does not extend to the surface. Given that not every crater of comparable size on Ceres exhibits concentric fractures, it is also suggested that these conditions are only met locally and may be related to the surface temperature. Correlations of concentrically fractured craters with other volatile related features, such as pitted terrains and floor fracturing, suggest that the low‐viscosity subsurface layer may be enriched in ice.

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The fracture of water ice Ih: A short overview

Cited by 28 publications

References 70 publications

The implications of tides on the Mimas ocean hypothesis

The implications of tides on the Mimas ocean hypothesis

Domes, pits, and small chaos on Europa produced by water sills

Ceres Crater Degradation Inferred From Concentric Fracturing

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