The role of asteroid strength, porosity and internal friction in impact momentum transfer

Raducan, Sabina D.; Davison, T. M.; Luther, R.; Collins, G. S.

doi:10.1016/j.icarus.2019.03.040

Cited by 65 publications

(157 citation statements)

References 51 publications

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“…Craters and ejecta distributions produced by impacts simulated with iSALE have been validated previously against laboratory impact experiments (Wünnemann et al, 2016;Luther et al, 2018;Raducan et al, 2019). iSALE has also been benchmarked against other hydrocodes (Pierazzo et al, 2008), with crater size typically agreeing to within 10%.…”

Section: Numerical Modelmentioning

confidence: 99%

“…It can be converted to an approximate pressure at the onset of crushing by multiplying by the bulk modulus. As in previous work (Raducan et al, 2019), e0 was set proportional to the ratio of the cohesion of the damaged material Y d0 and the bulk modulus. For simplicity and numerical stability, we set the χ parameter (the elastic wave speed ratio of porous and non-porous material) to 1, implying that the elastic wave speed in the porous material was equal to that in the nonporous component.…”

Section: Homogeneous Porous Half-spacementioning

confidence: 99%

“…During the excavation stage of crater formation, a large amount of material is ejected ballistically out of the crater as ejecta (Oberbeck, 1975;Housen et al, 1983). Previous laboratory (Housen and Holsapple, 2011) and numerical studies (Jutzi and Michel, 2014;Luther et al, 2018;Raducan et al, 2019) of impact events into homogeneous targets have shown that the speed and mass of ejecta depends sensitively on target material properties, such as cohesive strength, porosity and the coefficient of internal friction. However, most bodies in the Solar System are not homogeneous, as shown by past missions to asteroids, such as the NEAR-Shoemaker (Veverka et al, 2001), the OSIRIS-REx (Lauretta et al, 2019;Walsh et al, 2012) or the Hayabusa missions (Yano et al, 2006;Watanabe et al, 2019), as well as Earth-based thermal infrared observations (Delbo et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

“…In our previous work, Raducan et al (2019), we presented numerical simulations of strength-dominated impacts on a homogeneous, small-asteroid surface. We quantified the influence of target cohesion, porosity and internal friction coefficient on the mass-velocity ejecta distribution produced by an example artificial impact and used the DART mission (Michel et al, 2016;Cheng et al, 2016) as a motivating case study.…”

Section: Introductionmentioning

confidence: 99%

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The effects of asteroid layering on ejecta mass-velocity distribution and implications for impact momentum transfer

Raducan

Davison

Collins

2020

Planetary and Space Science

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Most bodies in the Solar System do not have a homogeneous structure. Understanding the outcome of an impact into regolith layers of different properties is especially important for NASA's Double Asteroid Redirection Test (DART) and ESA's Hera missions. Here we used the iSALE shock physics code to simulate the DART impact into three different target scenarios in the strength regime: a homogeneous porous half-space; layered targets with a porous weak layer overlying a stronger bedrock; and targets with exponentially decreasing porosity with depth. For each scenario we determined the sensitivity of crater morphology, ejecta mass-velocity distribution and momentum transferred from the impact for deflection, β −1, to target properties and structure. We found that for the homogeneous porous half-space, cohesion and porosity play a significant role and the DART impact is expected to produce a β − 1 between 1 and 3. In the two-layer target scenario, the

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Section: Numerical Modelmentioning

confidence: 99%

Section: Homogeneous Porous Half-spacementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The effects of asteroid layering on ejecta mass-velocity distribution and implications for impact momentum transfer

Raducan

Davison

Collins

2020

Planetary and Space Science

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“…iSALE includes a strength model suitable for impacts into geologic targets (Collins et al, 2004) and a porosity compaction model: the ϵ − α model (Collins et al, 2011; Wünnemann et al, 2006). iSALE has been extensively validated against laboratory impact experiments (Raducan et al, 2019; Wünnemann et al, 2016), as well as benchmarked against other hydrocodes (Davison et al, 2011; Pierazzo et al, 2008) for simulating crater size and morphology.…”

Section: Numerical Modelmentioning

confidence: 99%

Morphological Diversity of Impact Craters on Asteroid (16) Psyche: Insight From Numerical Models

2020

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The asteroid (16) Psyche, target of NASA's “Psyche” mission, is thought to be one of the most massive exposed iron cores in the solar system. Earth‐based observations suggest that Psyche has a metal‐rich surface; however, its internal structure cannot be determined from ground‐based observations. Here we simulate impacts into a variety of possible target structures on Psyche and show the possible diversity in crater morphologies that the “Psyche” mission could encounter. If Psyche's interior is homogeneous, then the mission will find simple bowl‐shaped craters, with a depth‐diameter ratio diagnostic of rock or iron. Craters will be much deeper than those on other visited asteroids and possess much more spectacular rims if the surface is dominated by metallic iron. On the other hand, if Psyche has a layered structure, the spacecraft could find craters with more complex morphologies, such as concentric or flat‐floored craters. Furthermore, if ferrovolcanism occurred on Psyche, then the morphology of craters less than 2 km in diameter could be even more exotic. Based on three to four proposed large craters on Psyche's surface, model size‐frequency distributions suggest that if Psyche is indeed an exposed iron core, then the spacecraft will encounter a very old and evolved surface, that would be 4.5 Gyr old. For a rocky surface, then Psyche could be at least 3 Gyr old.

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Deflection driven evolution of asteroid impact risk under large uncertainties

et al. 2020

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The role of asteroid strength, porosity and internal friction in impact momentum transfer

Cited by 65 publications

References 51 publications

The effects of asteroid layering on ejecta mass-velocity distribution and implications for impact momentum transfer

The effects of asteroid layering on ejecta mass-velocity distribution and implications for impact momentum transfer

Morphological Diversity of Impact Craters on Asteroid (16) Psyche: Insight From Numerical Models

Deflection driven evolution of asteroid impact risk under large uncertainties

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