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Grains and Dust Dynamics

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Physics of Soft Impact and Cratering

Part of the book series: Lecture Notes in Physics ((LNP,volume 910))

Abstract

We have studied impact drag force and impact cratering mechanics thus far in this book. As a target material, dense granular beds have been principally considered. Soft impact with a loose granular target causes many intriguing phenomena, as described in the previous chapters. In this chapter, we will focus on other types of soft impact phenomena that are also related to planetary science. First, the impact of dust aggregates in a protoplanetary disk will be discussed. Dust grains coagulate to become fluffy dust aggregates. The physical properties of the aggregates are key quantities to understanding the history of planetesimal formation. Next, we will return to the discussion of dense macroscopic grains called regolith that cover the surface of various astronomical objects. Some interesting physical properties relating to the impact of dust aggregates and regolith migration will be briefly discussed in this chapter.

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Notes

  1. 1.

    The scale height H scale is computed from the balance between the vertical force F z in Eq. (7.5) and the pressure gradient force as \(\varOmega _{K}^{2}z + (1/\rho _{t})dp/dz = 0\). Assuming the isothermal condition p = ρ t C s 2, the vertical density profile is computed as \(\rho _{t} \sim \exp [-(z/H_{\mathrm{scale}})^{2}]\).

  2. 2.

    \(\alpha _{\nu } = 10^{-3}\) is used to calculate the collision velocity.

  3. 3.

    Since the handling of tiny grains under a microgravity environment demands sophisticated experimental techniques, only this group has been able to perform this type of experiment.

  4. 4.

    The word monomer represents individual submicron-sized particle that compose the dust aggregate.

  5. 5.

    If two monomer sizes are different (D 1 and D 2), D i corresponds to the reduced diameter \(D_{i} = D_{1}D_{2}/(D_{1} + D_{2})\).

  6. 6.

    Note that this factor \(\mathcal{Q}\) and the quality factor Q are different.

  7. 7.

    This situation is the same as that in the case of thermal conduction in rocks.

  8. 8.

    The mean collisional lifetime T life is determined by the average period of the large impact which results in the catastrophic disruption of the body. This upper limit of the impact energy relates to the constraint (ii). Additionally, the convective velocity by the largest impact cannot exceed the escape velocity. Thus, the constraint (i) is automatically fulfilled. For the convective roll size, we temporarily assume the small roll size (\(\simeq 100D_{g}\)) on the basis of preliminary experimental observation.

  9. 9.

    To obtain this relation, we assume that the initial vertical velocity is proportional to the friction velocity.

  10. 10.

    To make the two-dimensionally spreading washboard road pattern, an extensively wide wheel is necessary. It is difficult to imagine such a situation.

  11. 11.

    To model the large-scale dune migration in a laboratory, water flow was used in the experiment. This is a type of similar modeling for geological-scale phenomena (Sect. 2.8).

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Authors and Affiliations

  1. Department of Earth and Environmental Sciences, Nagoya University, Nagoya, Japan

    Hiroaki Katsuragi

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  1. Hiroaki Katsuragi
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Katsuragi, H. (2016). Grains and Dust Dynamics. In: Physics of Soft Impact and Cratering. Lecture Notes in Physics, vol 910. Springer, Tokyo. https://doi.org/10.1007/978-4-431-55648-0_7

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