Impact excitation of a seismic pulse and vibrational normal modes on asteroid Bennu and associated slumping of regolith

Quillen, Alice C.; Zhao, Yi; Chen, Yuanyuan; Sánchez, Paul; Nelson, Randal C.; Schwartz, S. R.

doi:10.1016/j.icarus.2018.09.032

Cited by 21 publications

(32 citation statements)

References 110 publications

(220 reference statements)

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“…Furthermore, Quillen et al. (2019) propose a scaling of seismic acceleration to estimate the contribution of seismic reverberation. We aim to formulate a new seismic scaling by taking into account the effect of regolith yield strength.…”

Section: Implication For Asteroid Resurfacing By Seismic Shakingmentioning

confidence: 99%

Simulation of Seismic Wave Propagation on Asteroid Ryugu Induced by The Impact Experiment of The Hayabusa2 Mission: Limited Mass Transport by Low Yield Strength of Porous Regolith

et al. 2021

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Multiple space exploration missions have recently revealed that asteroids have complex and variable surfaces. Geomorphological features are clues for mass transport processes occurring on small bodies. For example, the NEAR Shoemaker mission discovered a loose regolith layer on asteroid Eros. There are direct evidences of downslope motions, such as flat-floored sediments ponds in craters, a deficit of small craters, and large blocks surrounded by debris aprons (e.g., Thomas et al., 2002; Veverka et al., 2001). Miyamoto et al. (2007) report from images taken by Hayabusa that the surface regolith on Itokawa is segregated. However, transporting processes of asteroid regolith in both lateral and vertical directions remain ambiguous.

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Section: Implication For Asteroid Resurfacing By Seismic Shakingmentioning

confidence: 99%

Simulation of Seismic Wave Propagation on Asteroid Ryugu Induced by The Impact Experiment of The Hayabusa2 Mission: Limited Mass Transport by Low Yield Strength of Porous Regolith

et al. 2021

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“…the body and from external masses, and the elastic and damping spring forces acting only between sufficiently close particle pairs with previously identified springs connecting them. When a large number of particles is used to resolve the spinning body, the mass-spring model behaves like an isotropic continuum elastic solid (Kot et al, 2015;Kot and Nagahashi, 2016), including its ability to exhibit normal mode oscillations and transmit seismic waves (Quillen et al, 2019b). The Kelvin-Voigt model arises because spring forces are exerted in parallel with damping.…”

Section: Simulationsmentioning

confidence: 99%

“…Sensitivity to numbers of particles simulated, spring network or lattice and particle generation technique is discussed by Quillen et al (2016b). Normal mode frequencies and seismic wave propagation speeds were checked for a near-spherical shape model by Quillen et al (2019b). We have also used this code to study spinorbit resonance capture and crossing in multiple body systems (Quillen et al, 2017).…”

Section: Simulationsmentioning

confidence: 99%

Near/far side asymmetry in the tidally heated Moon

Quillen

Martini

Nakajima

2019

Icarus

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Using viscoelastic mass spring model simulations to track heat distribution inside a tidally perturbed body, we measure the near/far side asymmetry of heating in the crust of a spin synchronous Moon in eccentric orbit about the Earth. With the young Moon within 8 Earth radii of the Earth, we find that tidal heating per unit area in a lunar crustal shell is asymmetric due to the octupole order moment in the Earth's tidal field and is 10 to 20% higher on its near side than on its far side. Tidal heating reduces the crustal basal heat flux and the rate of magma ocean crystallization. Assuming that the local crustal growth rate depends on the local basal heat flux and the distribution of tidal heating in latitude and longitude, a heat conductivity model illustrates that a moderately asymmetric and growing lunar crust could maintain its near/far side thickness asymmetry but only while the Moon is near the Earth.

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“…This evidence leads us to the assumption that Didymos A may have a loose regolith layer on the surface, i.e. local small-scale avalanches may occur episodically at the unstable regions, which could be caused by various triggering processes, such as surface failure due to thermal fatigue, and ground shaking because of local structural creep (Quillen et al 2016(Quillen et al , 2018. In effect, these local-scale avalanches may lead to a slight surface mass redistribution, or to mass shedding with much more complex influence on the dynamics of the binary system.…”

Section: Parameter Symbol Valuementioning

confidence: 99%

The expansion of debris flow shed from the primary of 65803 Didymos

Michel

Hirabayashi

et al. 2018

Monthly Notices of the Royal Astronomical Society

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This paper investigates the plausible mass shedding from the surface of Didymos A, the primary of Near-Earth binary asteroid 65803 Didymos, and the subsequent orbital evolution of the shedding debris. Shedding conditions are derived semi-analytically. The unstable surface area on Didymos A is determined by combining the analyses and numeric results of SSDEM simulations. We show the observation-based model gives a highly unstable surface for Didymos A. In particular, most of the equatorial ridge is unattachable for cohesionless regolith, and an active region emerges along the ridge, in which extensive avalanches that cause surface mass shedding seem likely to happen. We track the ballistic motion of shedding debris from the unstable area. Month-long simulations show the diverse evolutions of sample particles with different sizes, due to the varying magnitude of solar radiation pressure. Statistics on the dynamical fates of shedding debris give clues on the current development of this binary system. Depending on the observation-based reference model, we find a vast majority of the shedding mass is finally transferred to Didymos B and thus leads to a cumulative growth. The cumulated mass may cause a spiralling-in motion of Didymos B, and the spiralling-in speed depends on the frequency and magnitude of mass shedding. A topography dependence of the mass shedding/transfer is also noticed that the cumulated mass mostly originates from highly elevated regions of the ridge areas. Long term it suggests that the shedding processes prefer to erode the bulges first and force the equatorial ridge to evolve into good roundness.

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Impact excitation of a seismic pulse and vibrational normal modes on asteroid Bennu and associated slumping of regolith

Cited by 21 publications

References 110 publications

Simulation of Seismic Wave Propagation on Asteroid Ryugu Induced by The Impact Experiment of The Hayabusa2 Mission: Limited Mass Transport by Low Yield Strength of Porous Regolith

Simulation of Seismic Wave Propagation on Asteroid Ryugu Induced by The Impact Experiment of The Hayabusa2 Mission: Limited Mass Transport by Low Yield Strength of Porous Regolith

Near/far side asymmetry in the tidally heated Moon

The expansion of debris flow shed from the primary of 65803 Didymos

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