Ejecta cloud from the AIDA space project kinetic impact on the secondary of a binary asteroid: II. Fates and evolutionary dependencies

Yu, Yang; Michel, Patrick

doi:10.1016/j.icarus.2018.04.017

Cited by 30 publications

(32 citation statements)

References 34 publications

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“…Similarly, there have been studies of the fate of ejecta and debris from man‐made impacts on asteroids. In particular, studies of the expected evolution of the debris cloud after the impact of the DART mission (Schwartz et al, ; Yu et al, ; Yu & Michel, ) and the Hayabusa2 Small Carryon Impactor experiment (Arakawa et al, ; Giancotti et al, ) have been carried out recently. While these asteroids are more similar in size to Bennu, the source of the ejecta is again from a high‐energy impact, which differs from the observed events at Bennu because they predominantly produce high‐velocity ejecta that quickly escape the system.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Evolution of Simulated Particles Ejected From Asteroid Bennu

et al. 2020

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In early 2019, the OSIRIS‐REx spacecraft discovered small particles being ejected from the surface of the near‐Earth asteroid Bennu.sww Although they were seen to be ejected at slow speeds, on the order of tens of cm/s, a number of particles were surprisingly seen to orbit for multiple revolutions and days, which requires a dynamical mechanism to quickly and substantially modify the orbit to prevent re‐impact upon their first periapse passage. This paper demonstrates that, based on simulations constrained by the conditions of the observed events, the combined effects of gravity, solar radiation pressure, and thermal radiation pressure from Bennu can produce many sustained orbits for ejected particles. Furthermore, the simulated populations exhibit two interesting phenomena that could play an important role in the geophysical evolution of bodies such as Bennu. First, small particles (<1 cm radius) are preferentially removed from the system, which could lead to a deficit of such particles on the surface. Second, re‐impacting particles preferentially land near or on the equatorial bulge of Bennu. Over time, this can lead to crater in‐filling and growth of the equatorial radius without requiring landslides.

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Section: Introductionmentioning

confidence: 99%

Dynamical Evolution of Simulated Particles Ejected From Asteroid Bennu

et al. 2020

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“…• The debris that falls on the surface of Didymos, with impact velocities not greater than 10 m/s [18], will not cause large disturbances either though they will cause some secondary ejecta.…”

Section: Implications For Asteroidsmentioning

confidence: 99%

Seismic waves in the asteroid environment

Sánchez

Scheeres

2021

EPJ Web Conf.

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Through numerical simulations, we investigate impact generated seismic wave transmission in granular media under extremely low pressure. This mimics the conditions in the interior of asteroids and other small planetary bodies. We find a dependency not only on the overburden pressure on the medium, but also on the velocity of the impact that generates the wave. This is, at extremely low values of overburden pressure, the wave speed depends no only on the imposed pressure, but also on the increment in pressure created by the passing of the wave. We study crystalline and random packings and find very similar behaviour though with different wave speeds as expected. We then relate our results to different mission-related events on asteroids.

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“…The strength of their surfaces and interiors has been the topic of large research efforts, but they have been focused on the macroscopic strength of the soil disjoint from the global mechanics of the asteroid. The upcoming DART [49] mission is also running into the same question about the strength of asteroid Didymos. Other efforts related to planetary defense and asteroid mining can also be added to the interested parties, but a theoretical explanation to establish how cohesive and gravitational forces interact to support the structural integrity of granular asteroids or how they scale is lacking.…”

Section: Fig 5 Coordination Number Z * and Anisotropy Descriptors (A *mentioning

confidence: 99%

Scaling behavior of cohesive self-gravitating aggregates

2018

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By means of extensive three-dimensional contact dynamics simulations, we analyze the strength properties and microstructure of a granular asteroid, modeled as a self-gravitating cohesive granular aggregate composed of spherical particles, and subjected to diametrical compression tests. We show that, for a broad range of system parameters (shear rate, cohesive forces, asteroid diameter), the behavior can be described by a modified inertial number that incorporates interparticle cohesion and gravitational forces. At low inertial numbers, the behavior is ductile with a well-defined stress peak that scales with internal pressure with a prefactor 0.9. As the inertial number increases, both the prefactor and fluctuations around the mean increase, evidencing a dynamical crisis resulting from the destabilizing effect of particle inertia. From a micromechanical description of the contact and force networks, we propose a model that accounts for solid fraction, local stress, particle connectivity, and granular texture. In the limit of small inertial numbers, we find a very good agreement of the theoretical estimate of compressive strength, evidencing the major role of these structural parameters for the modeled aggregates.

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Ejecta cloud from the AIDA space project kinetic impact on the secondary of a binary asteroid: II. Fates and evolutionary dependencies

Cited by 30 publications

References 34 publications

Dynamical Evolution of Simulated Particles Ejected From Asteroid Bennu

Dynamical Evolution of Simulated Particles Ejected From Asteroid Bennu

Seismic waves in the asteroid environment

Scaling behavior of cohesive self-gravitating aggregates

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