A crater and its ejecta: An interpretation of Deep Impact

Holsapple, K. A.; Housen, K. R.

doi:10.1016/j.icarus.2006.08.029

Cited by 234 publications

(304 citation statements)

References 21 publications

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“…The estimate of the projectile size needed to form a crater of 170 m has been performed considering two scaling laws, namely for porous material and cohesive soils (Holsapple & Housen 2007). The material strength has been set to 2 × 10 4 and 10 7 dyne/cm 2 .…”

Section: How Frequent Are the Impacts?mentioning

confidence: 99%

The activity of main belt comets

Capria

Marchi

Sanctis

et al. 2012

A&A

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Context. Main belt comets represent a recently discovered class of objects. They are quite intriguing because, while having a Tisserand invariant value higher than 3, are showing cometary activity. Aims. We study the activity of the main belt comets making the assumption that they are icy-bodies and that the activity has been triggered by an impact. We try to determine the characteristics of this activity. We also try to determine if the nowadays impact rate in the main asteroid belt is compatible with the hypothesis of an activity triggered by a recent impact. Methods. Due to the fact that the main belt comets can be considered as a kind of comets, we apply a thermal evolution model developed for icy bodies in order to simulate their activity. We also apply a model to derive the impact rate, with respect to the size of the impactor, in the main belt. Results. We demonstrate that a stable activity can result from a recent impact, able to expose ice-rich layers, and that the impact rate in the main belt is compatible with this explanation.

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Section: How Frequent Are the Impacts?mentioning

confidence: 99%

The activity of main belt comets

Capria

Marchi

Sanctis

et al. 2012

A&A

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“…These derived scaling laws allow us to relate the effects of different sizes, velocities, and superficial gravity and then obtain the size of a crater produced by a collision with a Solar System body. Holsapple & Housen (2007) present the updated scaling laws for cratering in a recent work dedicated to interpreting the observations of the Deep Impact event. These cratering laws are used here to calculate the size of the craters on Phoebe.…”

Section: Craters On Phoebe By Sdosmentioning

confidence: 99%

“…These cratering laws are used here to calculate the size of the craters on Phoebe. Thus, the diameter D of a crater produced by an impactor of diameter d can be obtained from the general equation (Holsapple & Housen 2007)…”

Section: Craters On Phoebe By Sdosmentioning

confidence: 99%

“…Since Phoebe is a small satellite with a relatively low gravity, the strength regime can be important for the smaller craters. As Phoebe's density (1.63 g cm −3 ) is similar to sand and lower compacting material is found on its surface, we adopt K 1 = 1.03, μ = 0.41, and ν = 0.4, which correspond to either sand or cohesive soil in Holsapple & Housen (2007). This value of μ corresponds to materials with a porosity of ∼30−35% (Holsapple & Schmidt 1987), which is compatible with the ranges of Phoebe's predicted porosity.…”

Section: Craters On Phoebe By Sdosmentioning

confidence: 99%

“…We note that D l depends strongly on the assumed value of strength, which is actually unknown. Then considering other values of the strength for less cohesive soils such as terrestrial dry desert alluvium of Y = 65 kpa (Holsapple & Housen 2007) and surface lunar regolith Y = 10 kpa (Holsapple 2011) 1 , D l could take the values 1.5 km and 233 mts, respectively. In the following, we will assume that D l = 4.2 km but it must be taken into account that D l can be as small as 233 mts.…”

Section: Craters On Phoebe By Sdosmentioning

confidence: 99%

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Origin of craters on Phoebe: comparison withCassini’s data

Sisto

Brunini

2011

A&A

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Context. Phoebe is one of the irregular satellites of Saturn. The images taken by the Cassini-Huygens spacecraft have allowed us to analyze its surface and the craters on it. Aims. We study the craters on Phoebe produced by both Centaur objects from the scattered disk (SD) and plutinos that have escaped from the 3:2 mean motion resonance with Neptune and compare our results with the observations by Cassini. Methods. We use previously developed simulations of trans-Neptunian objects and a method that allows us to derive the number of craters and the cratering rate on Phoebe.Results. We determine the number of craters and the largest crater on Phoebe produced by Centaurs in the present configuration of the solar system. We obtain a present normalized rate of encounters of Centaurs with Saturn ofḞ = 7.1 × 10 −11 per year, from which we can infer the current cratering rate on Phoebe for each crater diameter. Conclusions. Our study and comparison with observations suggest that the main crater features on Phoebe are unlikely to have been produced in the present configuration of the solar system but that they must have been created instead when the SD were depleted in the early solar system. If this is indeed what happened and the craters were produced when Phoebe was a satellite of Saturn, then it must have been captured, very early on in the evolution of the solar system.

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Morphology of asteroid (4179) Toutatis as imaged by Chang'E‐2 spacecraft

Zhu

et al. 2014

Geophysical Research Letters

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Close observations by the Chang'E-2 spacecraft reveal that the surface of asteroid (4179) Toutatis is characterized by abundant impact craters with most of them being degraded by surface resetting. The less degraded large crater with a diameter of~800 m at the south pole is estimated to be produced by an impactor with a diameter of~50 m from strength crater scaling relations. From the analysis of large-impact events on highly porous targets, we argue that Toutatis is likely a rubble-pile body and its two lobes are contact binaries. The fact that Toutatis suffered plenty of impacts with seismic shaking resetting the initial surface features but not resulting in catastrophic disruption is probably because of the material's high attenuation of shock wave.

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A crater and its ejecta: An interpretation of Deep Impact

Cited by 234 publications

References 21 publications

The activity of main belt comets

The activity of main belt comets

Origin of craters on Phoebe: comparison withCassini’s data

Morphology of asteroid (4179) Toutatis as imaged by Chang'E‐2 spacecraft

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