Dust Phenomena Relating to Airless Bodies

Szalay, J. R.; Poppe, A. R.; Agarwal, Jessica; Britt, D. T.; Belskaya, I. N.; Horányi, M.; Nakamura, Tomoki; Sachse, M.; Spahn, F.

doi:10.1007/s11214-018-0527-0

Cited by 25 publications

(20 citation statements)

References 309 publications

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“…One explanation may be grain segregation due to granular convection such as the Brazil nut effect [Watanabe et al, 2020]. Another explanation may be that small particles move on top surface layers more favorably than large boulders and are depleted [Szalay et al, 2018]. If this is the case, top surface layers can be considered to be mechanically weak and have evolved rapidly.…”

Section: Insights Into Reshaping and Top Shapes' Interiors From Surfamentioning

confidence: 99%

Spin-driven evolution of asteroids' top-shapes at fast and slow spins seen from (101955) Bennu and (162173) Ryugu

Hirabayashi

Nakano

Tatsumi

et al. 2020

Icarus

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Proximity observations by OSIRIS-REx and Hayabusa2 provided clues on the shape evolution processes of the target asteroids, (101955) Bennu and (162173) Ryugu. Their oblate shapes with equatorial ridges, or the so-called top shapes, may have evolved due to their rotational conditions at present and in the past. Different shape evolution scenarios were previously proposed; Bennu's top shape may have been driven by surface processing, while Ryugu's may have been developed due to large deformation. These two scenarios seem to be inconsistent. Here, we revisit the structural analyses in earlier works and fill a gap to connect these explanations. We also apply a semi-analytical technique for computing the cohesive strength distribution in a uniformly rotating triaxial ellipsoid to characterize the global failure of top-shaped bodies. Assuming that the structure is uniform, our semi-analytical approach describes the spatial variations in failed regions at different spin periods; surface regions are the most sensitive at longer spin periods, while interiors fail structurally at shorter spin periods. This finding suggests that the shape evolution of a top shape may vary due to rotation and internal structure, which can explain the different evolution scenarios of Bennu's and Ryugu's top shapes. We interpret our results as the indications of top shapes' various evolution processes. Highlights • We reanalyzed results from FEM analyses for asteroids Bennu and Ryugu, the targets of OSIRIS-REx and Hayabusa2, respectively. • We also applied a semi-analytical approach to quantify how the failure modes of top shapes vary with spin. • Top shapes may evolve by two deformation modes: surface processing at low spin and internal failure at high spin.

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Section: Insights Into Reshaping and Top Shapes' Interiors From Surfamentioning

confidence: 99%

Spin-driven evolution of asteroids' top-shapes at fast and slow spins seen from (101955) Bennu and (162173) Ryugu

Hirabayashi

Nakano

Tatsumi

et al. 2020

Icarus

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“…Understanding the impact velocity distribution and probability will aid in understanding the impact environment of these bodies and the expected rate of dust/debris production. These impacts may very well be responsible for formation of dust rings and satellites around planets (Harris 1984;Charnoz et al 2009Charnoz et al , 2018, dusty exospheres around small bodies (e.g., Szalay et al 2018), serve as source and replenishment of the interplanetary dust flux (e.g. Kuchner & Stark 2010;Vitense et al 2012;Poppe 2016) or lead to planetary surface cratering (e.g.…”

Section: Introductionmentioning

confidence: 99%

OSSOS. XXI. Collision Probabilities in the Edgeworth–Kuiper Belt

Abedin

Kavelaars

Greenstreet

et al. 2021

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Here, we present results on the intrinsic collision probabilities, P I , and range of collision speeds, V I , as a function of the heliocentric distance, r, in the trans-Neptunian region. The collision speed is one of the parameters, that serves as a proxy to a collisional outcome e.g., complete disruption and scattering of fragments, or formation of crater, where both processes are directly related to the impact energy. We utilize an improved and de-biased model of the trans-Neptunian object (TNO) region from the "Outer Solar System Origins Survey" (OSSOS). It provides a well-defined orbital distribution model of TNOs, based on multiple opposition observations of more than 1000 bodies. In this work we compute collisional probabilities for the OSSOS models of the main classical, resonant, detached+outer and scattering TNO populations. The intrinsic collision probabilities and collision speeds are computed using theÖpik's approach, as revised and modified by Wetherill for non-circular and inclined orbits. The calculations are carried out for each of the dynamical TNO groups, allowing for inter-population collisions as well as collisions within each TNO population, resulting in 28 combinations in total. Our results indicate that collisions in the trans-Neptunian region are possible over a wide range in (r, V I ) phase space. Although collisions are calculated to happen within r ∼ 20−200 AU and V I ∼ 0.1 km/s to as high as V I ∼ 9 km/s, most of the collisions are likely to happen at low relative velocities V I < 1 km/s and are dominated by the main classical belt.

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“…So far, many modeling efforts (Piquette & Horányi, 2017;Poppe & Horányi, 2010;Poppe et al, 2012;Stubbs et al, 2006) and laboratory experiments (Schwan et al, 2017;Wang et al, 2009Wang et al, , 2010Wang et al, , 2016 have been made to study the dust electrostatic process, whereas the mechanism capable of generating sufficiently large electric field or dust grain charges to levitate micron-sized particles has not been clearly identified (Hartzell & Scheeres, 2011;Szalay et al, 2018). Kimura et al (2014) proposed that the formation of the water molecules and silanols on the surface of the dielectric grains by the solar wind impacts is inevitable.…”

Section: Introductionmentioning

confidence: 99%

“…This explanation has been potentially supported by other observations (Grün et al, 2011;McCoy, 1976;Severny et al, 1975), and the dust was even reported to loft electrostatically to tens of kilometers height (McCoy, 1976;McCoy & Criswell, 1974;Zook & McCoy, 1991). Although it has been found that the Moon is surrounded by a tenuous, permanently present, and asymmetric dust cloud generated by the continual bombardment of meteoroids to the lunar surface (Horányi et al, 2015), the dust density observed at orbit is much smaller than that near the lunar surface where the dust electrostatic levitation plays an important role in the dust transport process (Szalay et al, 2018;Xie et al, 2016).…”

Section: Introductionmentioning

confidence: 99%

Weak Dust Activity Near a Geologically Young Surface Revealed by Chang'E‐3 Mission

Yan

Zhang

Xie

et al. 2019

Geophysical Research Letters

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In spite of great scientific and engineering interests in lunar exploration, natural dust activity near the Moon surface remains unclear. According to distinct reflectance features of lunar rocks and regolith observed by Chang'E‐3 mission, long‐term dust activity near a young surface is quantified with a new method. We found that a dust deposition upper line on rocks is about 28 cm above the ground. Below this line, the quantity of dust deposits becomes smaller as the altitude ascends, whereas above the line, no visible or only negligible amount of dust is distributed on the rocks. This dust distribution pattern could be explained by dust electrostatic levitation process. The results indicate distinctively weak long‐term dust activity near the young surface and suggest possible selection of geologically young regions as landing sites or lunar bases to minimize the effect of dust grains.

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Dust Phenomena Relating to Airless Bodies

Cited by 25 publications

References 309 publications

Spin-driven evolution of asteroids' top-shapes at fast and slow spins seen from (101955) Bennu and (162173) Ryugu

Spin-driven evolution of asteroids' top-shapes at fast and slow spins seen from (101955) Bennu and (162173) Ryugu

OSSOS. XXI. Collision Probabilities in the Edgeworth–Kuiper Belt

Weak Dust Activity Near a Geologically Young Surface Revealed by Chang'E‐3 Mission

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