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Planetary Impact Processes in Porous Materials

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Shock Phenomena in Granular and Porous Materials

Part of the book series: Shock Wave and High Pressure Phenomena ((SHOCKWAVE))

Abstract

Porous materials abound in the Solar System. Primordial solids accreted gently from dust into fragile, high-porosity aggregates; many asteroids have been disrupted and reaccreted as loosely bound porous rubble piles; and the crusts of airless, unprotected planetary surfaces are heavily fractured from prolonged bombardment of asteroids and comets. High porosity attenuates shock propagation and localizes shock heating, which has several important implications for the evolution of planetary surfaces. The high porosity of early solids implies that shock heating from collisions may have been sufficient to lithify the compacted material, mobilize fluids, cause crystallographic transformation and even generate significant volumes of melt. Internal porosity in asteroids increases their resistance to collisional disruption and reduces momentum transfer efficiency by virtue of enhanced shock attenuation and reduced particle velocity. This enhances accretional efficiency and lengthens the collisional lifespan of asteroids, but at the same time makes them harder to deflect by kinetic impact. Porosity in the crusts and soils of planetary surfaces has a similar effect on the impact process, reducing the speed and mass of ejecta as well as the ultimate size of the crater. Constraining the influence of subsurface porosity variations on impact crater size is a crucial step in using crater populations to estimate impactor flux, date planetary surfaces and infer subsurface properties.

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Notes

  1. 1.

    A fifth process, spallation, can be important, but is not relevant to the present discussion. Spallation occurs when the compressive shock reflects from the target surface in tension. If the tensile stress exceeds the strength of the target material, thin plate-shaped fragments are ejected from the periphery of the crater [14,15,16].

  2. 2.

    The crush strength is not as well defined as, say, the tensile strength of a brittle material. In actuality porous geological materials crush over a wide range of pressure, with more void space being eliminated as pressure increases. This has been described using the so-called P-α model [27] or a modified version referred to as the 𝜖-α model [28]. We refer to a single crush strength measure here as a way to simply characterize the material’s resistance to compaction. The specific values of crush strength cited refer to the stress that compresses the material 50% of the way to zero porosity [18].

  3. 3.

    The original definition of π 2 included a multiplicative factor of 3.22, which is not used here.

  4. 4.

    This is strictly true only when the target strength does not itself depend on size or timescales.

  5. 5.

    See discussion of mesoscale modeling in chapter by Vogler and Fredenburg.

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Authors and Affiliations

  1. Imperial College London, London, UK

    Gareth S. Collins

  2. University of Washington, Seattle, WA, USA

    Kevin R. Housen

  3. Center for Space and Habitability, Physics Institute, University of Bern, Bern, Switzerland

    Martin Jutzi

  4. Graduate School of Science, Kobe University, Kobe, Japan

    Akiko M. Nakamura

Authors
  1. Gareth S. Collins
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  2. Kevin R. Housen
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  3. Martin Jutzi
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  4. Akiko M. Nakamura
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Correspondence to Gareth S. Collins .

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Editors and Affiliations

  1. Sandia National Laboratories, Livermore, CA, USA

    Tracy J. Vogler

  2. Los Alamos National Laboratory, Los Alamos, NM, USA

    D. Anthony Fredenburg

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Collins, G.S., Housen, K.R., Jutzi, M., Nakamura, A.M. (2019). Planetary Impact Processes in Porous Materials. In: Vogler, T., Fredenburg, D. (eds) Shock Phenomena in Granular and Porous Materials. Shock Wave and High Pressure Phenomena. Springer, Cham. https://doi.org/10.1007/978-3-030-23002-9_4

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