Ejecta from experimental impact craters: Particle size distribution and fragmentation energy

Buhl, Elmar; Sommer, Frank; Poelchau, M. H.; Dresen, Georg; Kenkmann, T.

doi:10.1016/j.icarus.2014.04.039

Cited by 46 publications

(51 citation statements)

References 43 publications

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“…This alone indicates that the initial mass distribution of the ejecta particles is, to a good approximation, independent of their initial speed and angular distributions (Methods subsection 'Dust ejecta clouds'), and that the number of ejecta particles generated on the surface per unit time with mass greater than m follows a power law: N 1 (.m) / m 2a . The LDEX measurements indicate a < 0.9, surprisingly close to the value a G 5 0.8 suggested by the Galileo mission at the icy moons of Jupiter 12 and to laboratory experimental results of ejecta production from impacts 13 . The derived ejecta size distribution also represents the size distribution of the smallest lunar fines (very small particles) on the surface because most ejecta particles return to the Moon and comprise the regolith itself, unless these small particles efficiently conglomerate on the lunar surface into larger particles.…”

supporting

confidence: 85%

A permanent, asymmetric dust cloud around the Moon

Horányi

Szalay

Kempf

et al. 2015

Nature

202

151

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Interplanetary dust particles hit the surfaces of airless bodies in the Solar System, generating charged and neutral gas clouds, as well as secondary ejecta dust particles. Gravitationally bound ejecta clouds that form dust exospheres were recognized by in situ dust instruments around the icy moons of Jupiter and Saturn, but have hitherto not been observed near bodies with refractory regolith surfaces. High-altitude Apollo 15 and 17 observations of a 'horizon glow' indicated a putative population of high-density small dust particles near the lunar terminators, although later orbital observations yielded upper limits on the abundance of such particles that were a factor of about 10(4) lower than that necessary to produce the Apollo results. Here we report observations of a permanent, asymmetric dust cloud around the Moon, caused by impacts of high-speed cometary dust particles on eccentric orbits, as opposed to particles of asteroidal origin following near-circular paths striking the Moon at lower speeds. The density of the lunar ejecta cloud increases during the annual meteor showers, especially the Geminids, because the lunar surface is exposed to the same stream of interplanetary dust particles. We expect all airless planetary objects to be immersed in similar tenuous clouds of dust.

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supporting

confidence: 85%

A permanent, asymmetric dust cloud around the Moon

Horányi

Szalay

Kempf

et al. 2015

Nature

202

151

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“…Small craters excavate smaller volumes of material that is finer-grained on average than larger craters (e.g. : Gault et al, 1963;O'Keefe and Ahrens, 1985;Melosh, 1989;Buhl et al, 2014). Fine-grained rocks are more easily eroded or buried than coarser-grained rocks, so the coarser ejecta at larger pits should be preferentially preserved and less buried.…”

Section: Discussionmentioning

confidence: 99%

“…The average grain size for ejecta decreases with radial distance from the crater, such that the largest clasts or blocks are proximal to the crater rim (e.g. : Gault et al, 1963;O'Keefe and Ahrens, 1985;Melosh, 1989;Buhl et al, 2014). Conversely, drainage and collapse features such as sinkholes, which are typical of karst landscapes, and lava tube skylights form by gravitational collapse and do not create raised rims nor emplace material atop their rims (e.g., Okubo and Martel, 1998;Salvati and Sasowsky, 2002;Cushing et al, 2007;Robinson et al, 2012).…”

Section: Introductionmentioning

confidence: 99%

Evidence for an explosive origin of central pit craters on Mars

Williams

Bell

Christensen

et al. 2015

Icarus

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“…Comparative analysis of craters of various sizes documented that the extent of subsurface damage is very similar in size, volume, and geometry when normalized to the projectile size (Buhl et al. ). The D ‐value (2.42) measured in a shock recovery experiment (experiment 2‐1; Table ) was much higher than in the cratering experiments (Buhl et al.…”

Section: Damage Gradientsmentioning

confidence: 99%

Experimental impact cratering: A summary of the major results of the MEMIN research unit

Kenkmann

Deutsch

Thoma

et al. 2018

Meteorit & Planetary Scien

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This paper reviews major findings of the Multidisciplinary Experimental and Modeling Impact Crater Research Network (MEMIN). MEMIN is a consortium, funded from 2009 till 2017 by the German Research Foundation, and is aimed at investigating impact cratering processes by experimental and modeling approaches. The vision of this network has been to comprehensively quantify impact processes by conducting a strictly controlled experimental campaign at the laboratory scale, together with a multidisciplinary analytical approach. Central to MEMIN has been the use of powerful two‐stage light‐gas accelerators capable of producing impact craters in the decimeter size range in solid rocks that allowed detailed spatial analyses of petrophysical, structural, and geochemical changes in target rocks and ejecta. In addition, explosive setups, membrane‐driven diamond anvil cells, as well as laser irradiation and split Hopkinson pressure bar technologies have been used to study the response of minerals and rocks to shock and dynamic loading as well as high‐temperature conditions. We used Seeberger sandstone, Taunus quartzite, Carrara marble, and Weibern tuff as major target rock types. In concert with the experiments we conducted mesoscale numerical simulations of shock wave propagation in heterogeneous rocks resolving the complex response of grains and pores to compressive, shear, and tensile loading and macroscale modeling of crater formation and fracturing. Major results comprise (1) projectile–target interaction, (2) various aspects of shock metamorphism with special focus on low shock pressures and effects of target porosity and water saturation, (3) crater morphologies and cratering efficiencies in various nonporous and porous lithologies, (4) in situ target damage, (5) ejecta dynamics, and (6) geophysical survey of experimental craters.

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Ejecta from experimental impact craters: Particle size distribution and fragmentation energy

Cited by 46 publications

References 43 publications

A permanent, asymmetric dust cloud around the Moon

A permanent, asymmetric dust cloud around the Moon

Evidence for an explosive origin of central pit craters on Mars

Experimental impact cratering: A summary of the major results of the MEMIN research unit

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