Measurements of target compressive and tensile strength for application to impact cratering on ice‐silicate mixtures

Hiraoka, K.; Arakawa, Masahiko; Setoh, M.; Nakamura, Akiko

doi:10.1029/2007je002926

Cited by 16 publications

(14 citation statements)

References 19 publications

(39 reference statements)

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“…To measure tensile strength we used the Brazilian splitting tension test [ Fairhurst , 1964; ISRM , 1978], in which test cylinders are loaded in compression along an axial line, and fail in tension due to elastic strain perpendicular to the loading axis (Figure 2b). Although the Brazilian test is an indirect ‘index’ test, it is commonly used in testing rock [ Berenbaum and Brodie , 1959; Goodman , 1989] due to the ease of use, and has been employed previously on ice [ Mellor and Hawkes , 1971; Frederking and Timco , 1980; Hiraoka et al , 2008]. Sample cylinders were cut to 40–50 mm lengths, placed in the test fixture, and loaded at a constant displacement rate as in the fracture toughness tests.…”

Section: Methodsmentioning

confidence: 99%

“…Ice tensile strength decreases approximately exponentially with increasing porosity [ Schulson and Duval , 2009], and may be particularly important when pores are filled with fluids that lower crack tip resistance to propagation. Solid silicate impurities have been shown to increase tensile strength and resistance to impact wear [ Lange and Aherns , 1983; Arakawa and Tomizuka , 2004; Hiraoka et al , 2008] and ductile flow at low strain rates [ Goughnour and Andersland , 1968; Durham et al , 1992], although direct measurements of the effect of non‐silicate impurities on tensile strength at sub‐ballistic impact strain rates are lacking.…”

Section: Introductionmentioning

confidence: 99%

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Influence of temperature, composition, and grain size on the tensile failure of water ice: Implications for erosion on Titan

Litwin¹,

Zygielbaum²,

Polito³

et al. 2012

J. Geophys. Res.

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[1] Ice resistance to tensile fracture influences surface morphodynamics on outer planetary satellites such as Titan, yet measurements of tensile strength and fracture toughness of polycrystalline water ice at temperatures below terrestrial conditions (<220 K) have not been previously reported. We investigated these parameters from 260 K to 110 K using a walk-in freezer, and chilling by dry ice and liquid nitrogen. We also investigated the influence of solid impurity concentration and the spread in crystal grain size distribution. Although fracture toughness showed no sensitivity to temperature, we find that tensile strength increases with decreasing temperature at 7 kPa KÀ1 for all ice types tested. For pure water ice, samples made from uniform-sized seed crystals were stronger than mixed-grain-size ice, suggesting that strength is limited by the coarse tail of the size distribution. Samples tested submerged in liquid ethanol were 0.45 MPa weaker than in air; increasing porosity reduced tensile strength. Tensile strength increased linearly with concentration of urea, basalt and ammonium sulfate. These results suggest that on Titan and other icy satellites, the tensile strength of fine-grained polycrystalline water ice containing solid impurities may be several times greater than the 1 MPa value commonly used in modeling. For low strain rate processes where fracture propagation rather than fracture initiation limits strength, a temperature invariant fracture toughness of 0.15 MPa m 1/2 is appropriate. Understanding ice diagenesis on Titan, and the resulting composition, grain size distribution, and porosity, is needed to accurately model surface processes that are limited by ice resistance to fracture.

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Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Influence of temperature, composition, and grain size on the tensile failure of water ice: Implications for erosion on Titan

Litwin¹,

Zygielbaum²,

Polito³

et al. 2012

J. Geophys. Res.

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“…The tensile strength of a mixture depends on various factors, including porosity, fraction of impurity, composition of impurity, temperature, and grain size (e.g., Arakawa and Tomizuka, 2004;Hiraoka et al, 2008;Litwin et al, 2012). Although the results of this study suggested that the degree of collisional destruction of the targets would depend on tensile strength rather than compressive strength, the tensile strength of the targets were not directly measured in this study.…”

Section: Discussionmentioning

confidence: 77%

Collisional disruption of highly porous targets in the strength regime: Effects of mixture

Murakami

Nakamura

Yokoyama

et al. 2020

Planetary and Space Science

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Highly porous small bodies are thought to have been ubiquitous in the early solar system. Therefore, it is essential to understand the collision process of highly porous objects when considering the collisional evolution of primitive small bodies in the solar system. To date, impact disruption experiments have been conducted using high-porosity targets made of ice, pumice, gypsum, and glass, and numerical simulations of impact fracture of porous bodies have also been conducted. However, a variety of internal structures of high-porosity bodies are possible. Therefore, laboratory experiments and numerical simulations in the wide parameter space are necessary.In this study, high-porosity targets of sintered hollow glass beads and targets made by mixing perlite with hollow beads were used in a collision disruption experiment to investigate the effects of the mixture on collisional destruction of high-porosity bodies.Among the targets prepared under the same sintering conditions, it was found that the targets with more impurities tend to have lower compressive strength and lower resistance against impact disruption. Further, destruction of the mixture targets required more impact energy density than would have been expected from compressive strength. It is likely that the perlite grains in the target matrix inhibit crack growth through the glass framework. The mass fraction of the largest fragment collapsed to a single function of a scaling parameter of energy density in the strength regime ( ) when assuming ratios of tensile strength to compressive strength based on a relationship obtained for ice-silicate mixtures. However, the dependence on is much larger than that shown for porous targets with different internal microstructures from the targets in this study. The depth of the deep cavity specific to the high-porosity target was well represented by a dimensionless parameter using the compressive strength of both the pure glass and mixture targets. The empirical relationship of cavity depth was shown to hold for various targets used in previous studies irrespective of the internal microstructure of the targets.

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“…the values of Hiraoka et al, 2006. The targets were made in spheres using thin walled rubber balloons sitting in hemispherical moulds.…”

Section: Laboratory Experiments For Icy Bodiesmentioning

confidence: 99%

Impact cratering and break up of the small bodies of the Solar System

Leliwa-Kopystyński

Burchell

Lowen

2008

Icarus

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We consider the largest impact craters observed on small satellites and asteroids and the impact disruption of such bodies. Observational data are considered from 21 impact-like structures on 13 satellites and 8 asteroids (target body radii in the range 0.7 -265 km). If the radius of the target body is R and the diameter of the largest crater observed on this body D, the ratio D/R is then the main observational parameter of interest. This is found on the observed bodies and

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Measurements of target compressive and tensile strength for application to impact cratering on ice‐silicate mixtures

Cited by 16 publications

References 19 publications

Influence of temperature, composition, and grain size on the tensile failure of water ice: Implications for erosion on Titan

Influence of temperature, composition, and grain size on the tensile failure of water ice: Implications for erosion on Titan

Collisional disruption of highly porous targets in the strength regime: Effects of mixture

Impact cratering and break up of the small bodies of the Solar System

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