Impacts into Ice–Silicate Mixtures: Ejecta Mass and Size Distributions

Koschny, D.

doi:10.1006/icar.2001.6708

Cited by 76 publications

(68 citation statements)

References 21 publications

(15 reference statements)

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“…Here we investigated how those distributions as well as the material ejection angles vary with different projectile incidence angles. Our results agree with the results derived from impacts into other materials made by other authors [1,2,3,4].…”

Section: Introductionsupporting

confidence: 93%

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Research on Europa's Dust Cloud at The Open University's HVI Laboratory

Miljković

Mason

Zarnecki

2009

Trans. JSASS Space Tech. Japan

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Space in the vicinity of Europa is populated by dust originating from its surface. Fragments of the surface are ejected due to meteoroid hypervelocity impacts (but also they may originate from the sub-surface such as was found on Enceladus). It is assumed that orbit-based detection and analysis of material ejected from the Europan surface may provide an alternative method for sampling Europan material without landing on the surface. Relative impact speeds from these dust sources onto an in-orbit detector would, typically, be about 2 kms -1 . This impact speed is generally too low for complete vapourisation of the impactor/target and the ejecta material could be captured in-situ for further analysis. Our current work is aimed at the development of a new hybrid dust detector for any Europa orbiter as well as an understanding of Europa's dust cloud by mimicing micrometeoroid impact into simulated European regolith/ice. In this paper we present our latest research as well as the facility we have developed as a new laboratory in the field of HVI physics.

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Section: Introductionsupporting

confidence: 93%

“…1 In Table 1, our results are compared with other authors that performed similar studies on different target materials with different projectiles. [12], [2] for impacts into water, ice and ice-silica mixtures, indicating that gypsum is a good analogue for an icy/regolith planetary surface. …”

Section: Experimental Methods and Resultsmentioning

confidence: 99%

Research on Europa's Dust Cloud at The Open University's HVI Laboratory

Miljković

Mason

Zarnecki

2009

Trans. JSASS Space Tech. Japan

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“…Koschny and Grün (2001) performed impact experiments in mixtures of compact ice and silicate particles and showed that this relationship remains valid for inhomogeneous targets. It therefore seems appropriate to our study.…”

Section: Size-velocity Relationshipmentioning

confidence: 89%

Properties of the dust cloud caused by the Deep Impact experiment

Jordá

Lamy

Faury

et al. 2007

Icarus

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We present an analysis of the observations of the Deep Impact event performed by the OSIRIS narrow angle camera aboard the Rosetta spacecraft over two weeks, in an effort to characterize the cometary dust grains ejected from the nucleus of Comet 9P/Tempel 1. We adopt a Monte Carlo approach to generate calibrated synthetic images, and a linear combination of them is fitted to the calibrated images so as to determine the physical parameters of the dust cloud. Our model considers spherical olivine particles with a density of 3780 kg m −3 . It incorporates constraints on the direction of the cone of emission coming from additional images obtained at Pic du Midi observatory, and constraints on the dust terminal velocities coming from the physics of the impact. We find that the slope of the differential dust size distribution of grains with radii <20 µm (β > 0.008) is 3.1 ± 0.3, a value typical of cometary dust tails. This shows that there is no evidence in our data for an enhancement in sub-micron particles in the ejecta compared to the typical dust distribution of active comets. We estimate the mass of particles with radii <1.4 µm (β > 0.14) to be 1.5 ± 0.2 × 10 5 kg. These particles represent more than 80% of the cross-section of the observed dust cloud. The mass carried by larger particles depends whether the gas significantly increases the kinetic energy of the grains in the inner coma; it lies in the range 1-14 × 10 6 kg for particles with radii <100 µm (β > 0.002). We obtain the distribution of terminal velocities reached by the dust after the dust-gas interaction which is very well constrained between 10 and 600 m s −1 . It is characterized by Gaussian with a maximum at about 190 m s −1 and a width at half maximum of 150 m s −1 .

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“…In this paper, we concentrate on the crater parameters (crater morphology, volume, and yield); the measured ejecta parameters is described in a companion paper (Koschny and Grün 2001). The aim of this work is to find empirical formulae to describe the crater parameters as a function of the projectile and target properties.…”

Section: Introductionmentioning

confidence: 99%