Impact-Induced Seismic Activity on Asteroid 433 Eros: A Surface Modification Process

Richardson, James E.; Melosh, H. J.; Greenberg, R.

doi:10.1126/science.1104731

Cited by 145 publications

(158 citation statements)

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“…[24] As we already mentioned, seismic shaking has been recognized as a major mechanism of global resurfacing of asteroids and other small bodies [e.g., Asphaug and Melosh, 1993;Richardson et al, 2004Richardson et al, , 2005Thomas and Robinson, 2005]. While on the Moon the global resurfacing affects kilometer-scale topography, but leaves 10-km scale and larger craters well recognizable, on small bodies the seismic effects can completely reset the observed geological record (see discussion by Asphaug [2008]).…”

Section: Discussionmentioning

confidence: 99%

“…For example, Houston et al [1973] argued that seismic shaking from impacts contributes to regolith gardening on the Moon. Seismic shaking works more effectively on small bodies [e.g., Cintala et al, 1978] and has been recognized as the primary cause of global resurfacing on them [e.g., Asphaug and Melosh, 1993;Richardson et al, 2004Richardson et al, , 2005Thomas and Robinson, 2005;Asphaug, 2008]. Seismic shaking can trigger global downslope mass movement, if the acceleration of the surface due to seismic waves is comparable to or exceeds gravity.…”

Section: Introductionmentioning

confidence: 99%

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New observational evidence of global seismic effects of basin‐forming impacts on the Moon from Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter data

Kreslavsky

Head

2012

J. Geophys. Res.

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[1] New maps of kilometer-scale topographic roughness and concavity of the Moon reveal a very distinctive roughness signature of the proximal ejecta deposits of the Orientale basin (the Hevelius Formation). No other lunar impact basin, even the just-preceding Imbrium basin, is characterized by this type of signature although most have similar types of ejecta units and secondary crater structures. The preservation of this distinctive signature, and its lack in basins formed prior to Orientale, is interpreted to be the result of seismically induced smoothing caused by this latest major basin-forming event. Intense seismic waves accompanying the Orientale basin-forming event preceded the emplacement of its ejecta in time and operated to shake and smooth steep and rough topography associated with earlier basin deposits such as Imbrium. Orientale ejecta emplaced immediately following the passage of the seismic waves formed the distinctive roughness signature that has been preserved for almost 4 billion years.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

New observational evidence of global seismic effects of basin‐forming impacts on the Moon from Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter data

Kreslavsky

Head

2012

J. Geophys. Res.

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“…Seismic shaking -in Itokawa and Eros, seismic shaking remains the main mechanism to explain the presence of smooth terrains in gravitational lows (Richardson et al 2004(Richardson et al , 2005Miyamoto et al 2007). Seismic shaking tends to fluidize the material and to sort grains by size, with the finest grains migrating, by gravity, toward gravitational lows.…”

Section: Smooth Terrainsmentioning

confidence: 99%

Geomorphology of the Imhotep region on comet 67P/Churyumov-Gerasimenko from OSIRIS observations

Auger

Groussin

Jordá

et al. 2015

A&A

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Context. Since August 2014, the OSIRIS Narrow Angle Camera (NAC) onboard the Rosetta spacecraft has acquired high spatial resolution images of the nucleus of comet 67P/Churyumov-Gerasimenko, down to the decimeter scale. This paper focuses on the Imhotep region, located on the largest lobe of the nucleus, near the equator. Aims. We map, inventory, and describe the geomorphology of the Imhotep region. We propose and discuss some processes to explain the formation and ongoing evolution of this region. Methods. We used OSIRIS NAC images, gravitational heights and slopes, and digital terrain models to map and measure the morphologies of Imhotep. Results. The Imhotep region presents a wide variety of terrains and morphologies: smooth and rocky terrains, bright areas, linear features, roundish features, and boulders. Gravity processes such as mass wasting and collapse play a significant role in the geomorphological evolution of this region. Cometary processes initiate erosion and are responsible for the formation of degassing conduits that are revealed by elevated roundish features on the surface. We also propose a scenario for the formation and evolution of the Imhotep region; this implies the presence of large primordial voids inside the nucleus, resulting from its formation process.

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“…Understanding materials physics under impact has motivated extensive research in areas ranging from asteroid strikes [1] and ballistic deposition [2] to mechanochemical synthesis [3], materials failures [4,5], structural modification [6], and phase transformation [7]. Less conventionally, three decades ago, metallic powder particles were first observed to bond to metallic substrates under supersonicimpact conditions at low temperatures [8].…”

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confidence: 99%

Melting Can Hinder Impact-Induced Adhesion

et al. 2017

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Melting has long been used to join metallic materials, from welding to selective laser melting in additive manufacturing. In the same school of thought, localized melting has been generally perceived as an advantage, if not the main mechanism, for the adhesion of metallic microparticles to substrates during a supersonic impact. Here, we conduct the first in situ supersonic impact observations of individual metallic microparticles aimed at the explicit study of melting effects. Counterintuitively, we find that under at least some conditions melting is disadvantageous and hinders impact-induced adhesion. In the parameter space explored, i.e., ∼10 μm particle size and ∼1 km=s particle velocity, we argue that the solidification time is much longer than the residence time of the particle on the substrate, so that resolidification cannot be a significant factor in adhesion. DOI: 10.1103/PhysRevLett.119.175701 Understanding materials physics under impact has motivated extensive research in areas ranging from asteroid strikes [1] and ballistic deposition [2] to mechanochemical synthesis [3], materials failures [4,5], structural modification [6], and phase transformation [7]. Less conventionally, three decades ago, metallic powder particles were first observed to bond to metallic substrates under supersonicimpact conditions at low temperatures [8]. The notion of impact-induced adhesion, thereafter, has been implemented in powder processing through kinetic deposition or cold spray [9,10]. Kinetic deposition has proven successful in making coatings [11][12][13], in reclaiming damaged metallic surfaces [14], and in additively manufacturing bulk metallic materials [15].In this area of impact science, researchers have repeatedly observed a material-dependent critical velocity [16,17] [20] have been put forth to explain the underlying mechanism(s) of impact-induced adhesion, each of which enjoys partial support from observational data. For instance, sharp jumps observed in the temperature and strain in Lagrangian impact simulations have been used to support an argument for adiabatic shear localization [16,21]. Experimental measurements of reduced oxide content in cold spray coatings as compared to initial powder feedstock underpins an argument for oxide layer breakup [22]. Small spherical ejecta found in the coating [20] or intermetallic detected at the interface [23] suggest localized melting or interdiffusion.More consensus, however, has been attained around postmortem observations of material jets around the periphery of adhered particles [16,24,25]. We have recently, for the first time, conducted in situ observations of the impact behavior of individual supersonic metallic microparticles below and above the critical velocity and found that material ejection and jetting are crucial for adhesion [26,27]. We argued that neither shear localization nor melting are needed to account for material ejection. Rather, it can arise from the interaction of the impactinduced pressure wave with the contact periphery of the particle. A...

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Impact-Induced Seismic Activity on Asteroid 433 Eros: A Surface Modification Process

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Cited by 145 publications

References 22 publications

New observational evidence of global seismic effects of basin‐forming impacts on the Moon from Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter data

New observational evidence of global seismic effects of basin‐forming impacts on the Moon from Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter data

Geomorphology of the Imhotep region on comet 67P/Churyumov-Gerasimenko from OSIRIS observations

Melting Can Hinder Impact-Induced Adhesion

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