The Scaling of Impact Processes in Planetary Sciences

Holsapple, K.

doi:10.1146/annurev.earth.21.1.333

Cited by 178 publications

(413 citation statements)

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“…The density ratio for this work (ρ/δ ∼ 1.3) is larger than those for the previous experiments: ρ/δ ∼ 0.65 (Schmidt and Housen, 1987), 0.49 (Mizutani et al, 1983), and 0.31 to 0.74 (Hartmann, 1985). However, ν is typically 1/3 and µ is about ∼ 0.4 (Holsapple, 1993), that is, the exponent is γ ∼ 0.056. In this case, the differences in (ρ/δ) γ between this work and the previous experiments are ∼ 4% (Schmidt and Housen, 1987), ∼ 6% (Mizutani et al, 1983), and 3-8% (Hartmann, 1985).…”

Section: Discussionmentioning

confidence: 99%

“…The power-law exponent for the Π R -Π 2 relation decreases from TA to TC. The value of is related to the coupling parameter that links the early and late stages in impact cratering (Holsapple, 1993). It is therefore proposed that this coupling parameter also depends on target material properties.…”

Section: Relation Between Depth and Diameter Of Cratermentioning

confidence: 99%

“…Pi-group scaling has been used as a scaling relation for impact crater sizes (e.g., Holsapple, 1993). In this analysis, two dimensionless parameters are used:…”

Section: Introductionmentioning

confidence: 99%

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Transient crater growth in granular targets: An experimental study of low velocity impacts into glass sphere targets

Yamamoto

Wada

Okabe

et al. 2006

Icarus

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We experimentally studied the formation and collapse processes of transient craters. Polycarbonate projectiles with mass of 0.49 g were impacted into the soda-lime glass sphere target (mean diameters of glass spheres are ∼ 36, 72, and 220µm, respectively) using a single-stage light-gas gun. Impact velocity ranged from 11 to 329 m s −1 . We found that the transient crater collapses even at laboratory scales. The shape (diameter and depth) of the transient crater differs from that of the final crater. The depth-rim diameter ratios of the final and transient craters are 0.11-0.14 and 0.26-0.27, respectively. The rim diameter of both the transient and final crater depends on target material properties; however, the ratio of final to transient crater diameter does not. This suggests that target material properties affect the formation process of transient craters even in the gravity regime, and must be taken into account when scaling experimental results to planetary scales. By observing impacts into glass sphere targets, we show that although the early stage of the excavation flow does not depend on the target material properties, the radial expansion of the cavity after the end of vertical expansion does. This suggests that the effect of target material properties is specifically important in the later part of the crater excavation and collapse.

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Section: Discussionmentioning

confidence: 99%

Section: Relation Between Depth and Diameter Of Cratermentioning

confidence: 99%

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Transient crater growth in granular targets: An experimental study of low velocity impacts into glass sphere targets

Yamamoto

Wada

Okabe

et al. 2006

Icarus

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“…However, the average interval between two impacts is 140 My for a 100 m radius meteoroid (Marchi et al 2005) so that, when the inner core is large, the Slichter mode of Mercury could be more frequently excited. Holsapple (1993) has developed scaling laws describing the properties of a crater impact from the radius and velocity of the impactor. When the gravity dominates the strength of the materials in the formation of the crater, the rim radius of a simple bowl-shaped crater is given by (Holsapple 1993)…”

Section: Slichter Modes Detectionmentioning

confidence: 99%

Period of the Slichter mode of Mercury and its possible observation

Coyette

Hoolst

Déhant

2012

A&A

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Aims. We study the period of the Slichter mode (vibrational mode of the inner core of a planet) of Mercury in relation to its interior structure and assess the possibility to observe this mode with the probes MESSENGER and BepiColombo. Methods. The methodology of Grinfeld & Wisdom (2005, Phys. Earth Planet. Int., 151, 77) for the determination of the period of the polar Slichter modes of a planetary interior consisting of three homogeneous layers is generalized to models with an arbitrary but finite number of layers. Slichter modes periods are calculated for a large set of interior structure models of Mercury. We study the possible excitation of Slichter modes by a colllision with a meteoroid and estimate the minimal size of the meteoroid that could lead to a detection of these modes by BepiColombo. Results. The Slichter mode period obtained is on the order of several hours. Observation of the Slichter mode of Mercury allows constraining the inner core. An impact by a meteoroid with a radius of at least 100 m could excite the Slichter mode to a level observable by BepiColombo (assuming that the Slichter mode is the only excited mode), but since the estimated damping time of the Slichter mode is well below the average time between impacts of at least that size such an impact must have occured recently (less than 0.5 My ago).

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“…Consider the destruction of a grain of mass by the collision m \ 4no d s3/3 with a grain of mass m@. The mass *m lost from the target grain m by cratering with the collisional velocity u is (Holsapple 1993…”

Section: Collisional Destruction Of Grainsmentioning

confidence: 99%

Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks

Takeuchi

Artymowicz

2001

ApJ

206

239

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We analyze the dynamics of gas-dust coupling in the presence of stellar radiation pressure in circumstellar disks, which are in a transitional stage between the gas-dominated, optically thick, primordial nebulae, and the dust-dominated, optically thin Vega-type disks. Dust grains undergo radial migration, either leaving the disk owing to a strong radiation pressure or seeking a stable equilibrium orbit in corotation with gas. In our models of A-type stars surrounded by a total gas mass from a fraction to dozens of Earth masses, the outward migration speed of dust is comparable with the gas sound speed. Equilibrium orbits are circular, with exception of those signiÐcantly a †ected by radiation pressure, which can be strongly elliptic with apocenters extending beyond the bulk of the gas disk. The migration of dust gives rise to radial fractionation of dust and creates a variety of possible observed disk morphologies, which we compute by considering the equilibrium between the dust production and the dust-dust collisions removing particles from their equilibrium orbits. Large grains (typically km) are distributed Z200 throughout most of the gas disk. Smaller grains (in the range of 10È200 km) concentrate in a prominent ring structure in the outer region of the gas disk (presumably at radius D100 AU), where gas density is rapidly declining with radius. The width and density, as well as density contrast of the dust ring with respect to the inner dust disk, depend on the distribution of gas and the mechanical strength of the particles. Our results open the prospect for deducing the distribution of gas in circumstellar disks by observing their dust. We have qualitatively compared our models with two observed transitional disks around HR 4796A and HD 141569A. Dust migration can result in observation of a ring or a bimodal radial dust distribution, possibly very similar to the ones produced by gap-opening planets embedded in the disk, or shepherding it from inside or outside. We conclude that a convincing planet detection via dust imaging should include speciÐc nonaxisymmetric structure (spiral waves, streamers, resonant arcs) following from the dynamical simulations of perturbed disks.

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The Scaling of Impact Processes in Planetary Sciences

Cited by 178 publications

References 0 publications

Transient crater growth in granular targets: An experimental study of low velocity impacts into glass sphere targets

Transient crater growth in granular targets: An experimental study of low velocity impacts into glass sphere targets

Period of the Slichter mode of Mercury and its possible observation

Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks

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