Disruption patterns of rotating self-gravitating aggregates: A survey on angle of friction and tensile strength

Sánchez, Paul; Scheeres, Daniel J.

doi:10.1016/j.icarus.2016.01.016

Cited by 65 publications

(79 citation statements)

References 54 publications

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“…Rolling friction (Ai et al, 2011;Sánchez and Scheeres, 2016) has also been implemented in order to mimic the behaviour of aggregates formed by non-spherical grains. Particles are subjected to a torque that opposes the relative rotation of any two particles in contact.…”

Section: Numerical Modeling Detailsmentioning

confidence: 99%

Cohesive regolith on fast rotating asteroids

Sánchez

Scheeres

2020

Icarus

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The migration of cohesive regolith on the surface of an otherwise monolithic or strong asteroid is studied using theoretical and simulation models. The theory and simulations show that under an increasing spin rate (such as due to the YORP effect), the regolith covering is preferentially lost across certain regions of the body. For regolith with little or no cohesive strength, failure occurs by landsliding from the mid latitudes of the body at high enough spin rates.As the cohesive strength of the regolith increases, failure occurs by fission of grains (or coherent chunks of grains) across a greater extent of latitudes and eventually will first occur at the equator. As the spin rate is further increased, failure regions migrate from the first failure point to higher and lower latitudes. Eventually failure will encompass the equatorial region, however there always remains a region of high latitudes (around the poles) that will not undergo failure for arbitrarily high spin rates (unless disturbed by some other phenomenon). With these results a scaling law is derived that can be used to determine whether observed asteroids could retain surface regolith grains of a given size. The implications of this for the interpretation of spectral observations of small asteroids and boulder migration on large asteroids are discussed.

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Section: Numerical Modeling Detailsmentioning

confidence: 99%

Cohesive regolith on fast rotating asteroids

Sánchez

Scheeres

2020

Icarus

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“…Particles that are ejected near the equatorial plane can supposedly re-accumulate and form moonlet(s) . A more abrupt fission event could also produce a binary system (Tardivel et al 2018) or could be at the origin of the observed asteroid pairs (Pravec et al 2010;Sánchez and Scheeres 2016;Zhang et al 2018). Only the structurally strongest asteroids will reach the 2.4 h spin barrier.…”

Section: Spin Rate Size and Shapementioning

confidence: 99%

“…For the smaller asteroids (below ≈ 100 − 200 m), this spin barrier does not seem to exist (Pravec and Harris 2000). Additionally, this spin barrier might more accurately be described as a deformation or a fission barrier, as asteroids reaching it would have to deform or go through a fission process as their structure would fail at such high spin rates (Jewitt et al 2013(Jewitt et al , 2014Sánchez and Scheeres 2016;. From here, we can take one step further and study what happens to tri-axial ellipsoids when subjected to high spin rates.…”

Section: Deformation and Disruptionmentioning

confidence: 99%

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Small Solar System Bodies as granular media

Hestroffer

Sánchez

Staron

et al. 2019

Astron Astrophys Rev

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“…To solve this problem Sánchez and Scheeres [18] carried out a survey on angle of friction and tensile strength for ellipsoidal and spherical selfgravitating aggregates which were quasi-statically spun up to disruption. Fig.…”

Section: Disruption Patternsmentioning

confidence: 99%

Looking into the evolution of granular asteroids in the Solar System

et al. 2017

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Abstract. By now it has been accepted that most of the small asteroids in the Solar System are granular aggregates kept together by gravitational and possibly, cohesive forces. These aggregates can form, deform and disrupt over millennia subjected to different internal and external factors that would ultimately determine how they evolve over time. Parameters such as porosity, cohesive and tensile strength, angles of friction, particle size distributions, stress states, heterogeneity and yield criteria among others, determine how these granular systems will react when subjected to different, changing, external factors. These external factors include solar photon momentum, gravitational tides, micro-and macro-impacts and are believed to have produced and shaped the current asteroid population. In our research we use a combination of Soil Mechanics theory, Soft-Sphere Discrete Element Method (SSDEM) Simulations and Orbital Mechanics in order to understand how simulated, homogeneous and heterogeneous, ellipsoidal and spherical gravitational aggregates, a crude but useful representation of an asteroid, evolve when rotated to the point of disruption. Then, we compare our results to the shapes of observed asteroids as well as to the disruption patterns of a few active asteroids. Our results lead us to believe that the different shapes of observed asteroids as well as their unique disruption patterns could give us clues about their internal structure, strength and geophysical properties in general. Granular Asteroids and YORPIn the last decade, the study of asteroids as granular aggregates has gained importance. Even though it was originally assumed that the smallest of asteroids were monolithic rocks with a bare surface, the pictures obtained by NASA Galileo, Near-Showmaker (or just NEAR) and JAXA Hayabusa space missions revealed a substantial layer of unconsolidated rocky material and dust (regolith) covering the surface of (951) imply that not only asteroid surfaces are covered by regolith, but that their internal structure is not monolithic. This is what we define as a granular asteroid, a naturally occurring self-gravitating granular system.Of the many events that can disrupt a granular, nonmonolithic asteroid, here we will focus only on the disruption that could be caused by rotation. The angular velocity of this rotation, in the context of NEOs, can be accelerated by the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect which results from an interplay between solar radiation pressure and the shape of an asteroid [5,6]. Very succinctly, when the photons that come from the Sun ime-mail: diego.sanchez-lana@colorado.edu e-mail: dscheeres@colorado.edu e-mail: thirabayashi@purdue.edu e-mail: simon.tardivel@colorado.edu pact on the surface of an asteroid, they will be reflected, absorbed and re-emitted from it anisotropically due to its irregular shape. This will produce a net torque that affects the angular velocity of the asteroid. Over millennia, this change in the angular velocity will produce the deformation or ...

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Disruption patterns of rotating self-gravitating aggregates: A survey on angle of friction and tensile strength

Cited by 65 publications

References 54 publications

Cohesive regolith on fast rotating asteroids

Cohesive regolith on fast rotating asteroids

Small Solar System Bodies as granular media

Looking into the evolution of granular asteroids in the Solar System

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