Impacts into Ice–Silicate Mixtures: Crater Morphologies, Volumes, Depth-to-Diameter Ratios, and Yield

Koschny, D.; Grün, E.

doi:10.1006/icar.2001.6707

Cited by 77 publications

(67 citation statements)

References 24 publications

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“…This is in agreement with earlier measurements (e.g. Onose (2007); Koschny and Grün (2001) and Evans et al (1994)). The larger and slower fragments are usually ejected in a nearly vertical direction (e.g.…”

Section: Spatial Distribution Of Solid Ejecta Fragments In Gypsum Andsupporting

confidence: 94%

“…The larger and slower fragments are usually ejected in a nearly vertical direction (e.g. Onose (2007); Koschny and Grün (2001); Polanskey and Ahrens (1990)), hence those fragments were less likely to hit the Al foil, but they also may be too slow to make an imprint in the foil. Unlike gypsum, the spatial distribution of ejected fragments from ice could not be fully determined due 8 to the weak imprint and low fragment impact count on the foils.…”

Section: Spatial Distribution Of Solid Ejecta Fragments In Gypsum Andmentioning

confidence: 99%

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Ejecta fragmentation in impacts into gypsum and water ice

Miljković

Mason

Zarnecki

2011

Icarus

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Please cite this article as: Miljković, K., Mason, N.J., Zarnecki, J.C., Ejecta fragmentation in impacts into gypsum and water ice, Icarus (2011Icarus ( ), doi: 10.1016Icarus ( /j.icarus.2011 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. Ejecta fragmentation in impacts into AbstractUsing the light gas gun at the Open University's hypervelocity impact facility, a series of impact experiments exploring impacts into water ice and gypsum have been performed. Fragmentation of solid ejecta was recorded using two different methods, analysed and compared with the total ejecta. Preliminary results show that the size distribution of the ejecta fragments from water ice is very similar to those from gypsum. These results also represent a step towards a better understanding of ejecta fragmentation in geological materials, including icy surfaces in the Solar system.

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Section: Spatial Distribution Of Solid Ejecta Fragments In Gypsum Andsupporting

confidence: 94%

Section: Spatial Distribution Of Solid Ejecta Fragments In Gypsum Andmentioning

confidence: 99%

Ejecta fragmentation in impacts into gypsum and water ice

Miljković

Mason

Zarnecki

2011

Icarus

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“…Gault 1973;Koschny & Grün 2001). Historically, the simplified M cra = αE col relation has been derived by Marcus (1969) who extrapolated experimental results, obtained mainly by Gault et al (1962) on small projectiles, to the much larger sizes considered in his study (see p. 77 of Marcus 1969).…”

Section: B2 Catastrophic Fragmentationmentioning

confidence: 88%

“…See text for details. and the Koschny & Grün (2001) formula for crater-excavated masses M cra for ices and silicates (Appendix B). In order to explore how our results depend on the collision prescription, we have performed the following two additional runs:…”

Section: Collision Outcome Prescriptionmentioning

confidence: 99%

“…-one "hard" material run, assuming the Benz & Asphaug (1999) and Koschny & Grün (2001) prescriptions for compact silicates hold for the entire disc (i.e. numerically setting a sub = ∞ AU); -one "weak" material run, where we assume the Q * prescription of Krivov et al (2006), and a value of M cra five times higher than in the nominal case.…”

Section: Collision Outcome Prescriptionmentioning

confidence: 99%

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Collisional processes and size distribution in spatially extended debris discs

Thébault

Augereau

2007

A&A

158

250

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Context. New generations of instruments provide, or are about to provide, pan-chromatic images of debris discs and photometric measurements, that require new generations of models, in particular to account for their collisional activity. Aims. We present a new multi-annulus code for the study of collisionally evolving extended debris discs. We first aim to confirm and extend our preliminary result obtained for a single-annulus system, namely that the size distribution in realistic debris discs always departs from the theoretical collisional "equilibrium" dN ∝ R −3.5 dR power law, especially in the crucial size range of observable particles (R < ∼ 1 cm), where it displays a characteristic wavy pattern. We also study how debris discs density distributions, scattered light luminosity profiles, and Spectral Energy Distributions (SEDs) are affected by the coupled effect of collisions and radial mixing due to radiation pressure affected small grains. Methods. The size distribution evolution is modeled over 10 orders of magnitude, going from µm-sized grains to 50 km-sized bodies. The model takes into account the crucial influence of radiation pressure-affected small grains. We consider the collisional evolution of a fiducial, idealized a = 120 AU radius disc with an initial surface density Σ(a) ∝ a α . Several key parameters are explored: surface density profile, system's dynamical excitation, total dust mass, collision outcome prescriptions. Results. We show that the system's radial extension plays a crucial role and that the waviness of the size distribution is amplified by inter-annuli interactions: in most regions the collisional and size evolution of the dust is imposed by small particles on eccentric or unbound orbits produced further inside the disc. Moreover, the spatial distribution of all grains < ∼ 1 cm departs significantly from the initial profile in Σ(a) ∝ a α , while the bigger objects, containing most of the system's mass, still follow the initial distribution. This has consequences on the scattered-light radial profiles which get significantly flatter. We propose an empirical law to trace back the distribution of large unseen parent bodies from the observed profiles. We also show that the the waviness of the size distribution has a clear observable signature in the far-infrared and at (sub-)millimeter wavelengths. This suggests a test of our collision model, which requires observations with future facilities such as Herschel, SOFIA, SCUBA-2 and ALMA. Finally, we provide empirical formulae for the collisional size distribution and collision timescale which can be used for future debris disc modeling.

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Constraining the Ratio of Micrometeoroids From Short‐ and Long‐Period Comets at 1 AU From LADEE Observations of the Lunar Dust Cloud

Janches

Sarantos

Horányi

et al. 2018

Geophysical Research Letters

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We interpret recent observations of the secondary dust ejecta cloud around the Moon from the Lunar Dust Experiment (LDEX) on board the NASA Lunar Atmosphere and Dust Environment Explorer (LADEE) spacecraft with help from dynamical models of meteoroids. Results suggest that in order to match the spatial structure of observed ejecta profiles, the flux of meteoroids on the Moon must be primarily provided by short‐period comets with an excess ratio of at least 1.3:1 compared to long‐period comets. This ratio increases significantly if the dependence of the ejecta yield on impactor velocity is stronger than generally believed. The model accounts for the orbital geometry of LADEE and shows no indication of a large asymmetry in the meteoroid flux impacting from the Helion and Anti‐Helion directions.

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Impacts into Ice–Silicate Mixtures: Crater Morphologies, Volumes, Depth-to-Diameter Ratios, and Yield

Cited by 77 publications

References 24 publications

Ejecta fragmentation in impacts into gypsum and water ice

Ejecta fragmentation in impacts into gypsum and water ice

Collisional processes and size distribution in spatially extended debris discs

Constraining the Ratio of Micrometeoroids From Short‐ and Long‐Period Comets at 1 AU From LADEE Observations of the Lunar Dust Cloud

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