Hydrocode modelling of hypervelocity impacts on ice

Fendyke, Stephen M.; Price, M. C.; Burchell, M. J.

doi:10.1016/j.asr.2013.04.010

Cited by 8 publications

(7 citation statements)

References 33 publications

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“…Some workers have shown that transient crater scaling between impactor size and crater size in cold water ice scales like rock in the gravity regime (Chapman & McKinnon, 1986;McKinnon & Parmentier, 1986;Turtle & Pierazzo, 2001). Yet other models and impact experiments suggest that impactor size to crater size scaling may be different in water ice, with differences made more intense as material properties such as porosity evolve with time (Bierhaus & Schenk, 2010;Fendyke et al, 2013;Kurosawa & Takada, 2019;Michikami et al, 2017;Prieur et al, 2017;Yasui et al, 2017). As ice, regolith, and rocks are bombarded, broken, and mixed, the porosity, yield strength, and density of the target evolve with time in poorly constrained ways.…”

Section: Gardening Ice and Regolith On The Moon And Mercurymentioning

confidence: 99%

Impact Gardening as a Constraint on the Age, Source, and Evolution of Ice on Mercury and the Moon

et al. 2020

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We update an analytic impact gardening model (Costello et al., 2018, https://doi.org/10.1016/j.icarus.2018.05.023) to calculate the depth gardened by impactors on the Moon and Mercury and assess the implications of our results for the age, extent, and source of water ice deposits on both planetary bodies. We show that if the water presently on the Moon has a primordial origin, it may have been 4–15 m thick. If ice deposits are buried, they may be as shallow as 3 cm or as deep as 10 m and provide a gradient of probability for ice gardened into a column. Our calculations for gardening on Mercury show that thermal lag deposits will be reworked into the background over 200 Myr, and, thus, the most recent large‐scale deposition of ice on Mercury must have occurred no more than 200 Myr ago. We also find that gardening mixes incremental layers of ice with underlying regolith and prevents the growth of pure ice deposits by continuous supply. We conclude that ice deposits on the Moon and Mercury are likely the result of sudden and voluminous deposition.

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Section: Gardening Ice and Regolith On The Moon And Mercurymentioning

confidence: 99%

Impact Gardening as a Constraint on the Age, Source, and Evolution of Ice on Mercury and the Moon

et al. 2020

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“…This is the classic crater shape observed in thick brittle targets such as ice (e.g., Fendyke et al. ) or glass (e.g., Burchell and Grey ). An interesting feature is the regularity of the radial fractures.…”

Section: Resultsmentioning

confidence: 73%

“…However, Fendyke et al. () showed that it is possible to simulate laboratory‐scale hypervelocity impacts into thick water ice targets and Bray et al. () showed that layered targets can also be simulated.…”

Section: Introductionmentioning

confidence: 99%

Hypervelocity impacts into ice‐topped layered targets: Investigating the effects of ice crust thickness and subsurface density on crater morphology

Harriss

Burchell

2017

Meteorit & Planetary Scien

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Abstract-Many bodies in the outer solar system are theorized to have an ice shell with a different subsurface material below, be it chondritic, regolith, or a subsurface ocean. This layering can have a significant influence on the morphology of impact craters. Accordingly, we have undertaken laboratory hypervelocity impact experiments on a range of multilayered targets, with interiors of water, sand, and basalt. Impact experiments were undertaken using impact speeds in the range of 0.8-5.3 km s À1, a 1.5 mm Al ball bearing projectile, and an impact incidence of 45°. The surface ice crust had a thickness between 5 and 50 mm, i.e., some 3-30 times the projectile diameter. The thickness of the ice crust as well as the nature of the subsurface layer (liquid, well consolidated, etc.) have a marked effect on the morphology of the resulting impact crater, with thicker ice producing a larger crater diameter (at a given impact velocity), and the crater diameter scaling with impact speed to the power 0.72 for semi-infinite ice, but with 0.37 for thin ice. The density of the subsurface material changes the structure of the crater, with flat crater floors if there is a dense, well-consolidated subsurface layer (basalt) or steep, narrow craters if there is a less cohesive subsurface (sand). The associated faulting in the ice surface is also dependent on ice thickness and the substrate material. We find that the ice layer (in impacts at 5 km s À1 ) is effectively semi-infinite if its thickness is more than 15.5 times the projectile diameter. Below this, the crater diameter is reduced by 4% for each reduction in ice layer thickness equal to the impactor diameter. Crater depth is also affected. In the ice thickness region, 7-15.5 times the projectile diameter, the crater shape in the ice is modified even when the subsurface layer is not penetrated. For ice thicknesses, <7 times the projectile diameter, the ice layer is breached, but the nature of the resulting crater depends heavily on the subsurface material. If the subsurface is noncohesive (loose) material, a crater forms in it. If it is dense, well-consolidated basalt, no crater forms in the exposed subsurface layer.

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“…Standard AUTODYN library materials were used to simulate copper (Steinberg, 1991 for EoS data using a strength model from Steinberg et al, 1980). Ice was simulated using the 5-phase EoS detailed in Senft and Stewart (2008), using an easy to implement strength model validated against experimental data described in Fendyke et al (2013). Peak pressures were determined by placing tracers (referred to as 'gauges' in AUTODYN) within the projectile.…”

Section: Resultsmentioning

confidence: 99%

Survivability of copper projectiles during hypervelocity impacts in porous ice: A laboratory investigation of the survivability of projectiles impacting comets or other bodies

McDermott

Price

Cole

et al. 2016

Icarus

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a b s t r a c tDuring hypervelocity impact (>a few km s À1 ) the resulting cratering and/or disruption of the target body often outweighs interest on the outcome of the projectile material, with the majority of projectiles assumed to be vaporised. However, on Earth, fragments, often metallic, have been recovered from impact sites, meaning that metallic projectile fragments may survive a hypervelocity impact and still exist within the wall, floor and/or ejecta of the impact crater post-impact. The discovery of the remnant impactor composition within the craters of asteroids, planets and comets could provide further information regarding the impact history of a body. Accordingly, we study in the laboratory the survivability of 1 and 2 mm diameter copper projectiles fired onto ice at speeds between 1.00 and 7.05 km s À1 . The projectile was recovered intact at speeds up to 1.50 km s À1 , with no ductile deformation, but some surface pitting was observed. At 2.39 km s À1 , the projectile showed increasing ductile deformation and broke into two parts. Above velocities of 2.60 km s À1 increasing numbers of projectile fragments were identified post impact, with the mean size of the fragments decreasing with increasing impact velocity. The decrease in size also corresponds with an increase in the number of projectile fragments recovered, as with increasing shock pressure the projectile material is more intensely disrupted, producing smaller and more numerous fragments. The damage to the projectile is divided into four classes with increasing speed and shock pressure: (1) minimal damage, (2) ductile deformation, start of break up, (3) increasing fragmentation, and (4) complete fragmentation. The implications of such behaviour is considered for specific examples of impacts of metallic impactors onto Solar System bodies, including LCROSS impacting the Moon, iron meteorites onto Mars and NASA's ''Deep Impact" mission where a spacecraft impacted a comet.

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Hydrocode modelling of hypervelocity impacts on ice

Cited by 8 publications

References 33 publications

Impact Gardening as a Constraint on the Age, Source, and Evolution of Ice on Mercury and the Moon

Impact Gardening as a Constraint on the Age, Source, and Evolution of Ice on Mercury and the Moon

Hypervelocity impacts into ice‐topped layered targets: Investigating the effects of ice crust thickness and subsurface density on crater morphology

Survivability of copper projectiles during hypervelocity impacts in porous ice: A laboratory investigation of the survivability of projectiles impacting comets or other bodies

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