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Coupled Spin and Shape Evolution of Small Rubble-Pile Asteroids: Self-Limitation of the YORP Effect | | Desireé Cotto-Figueroa
; Thomas S. Statler
; Derek C. Richardson
; Paolo Tanga
; | | Date: |
5 Nov 2014 | | Abstract: | We present the first self-consistent simulations of the coupled spin and
shape evolutions of small gravitational aggregates under the influence of the
YORP effect. Because of YORP sensitivity to detailed surface topography, even
small centrifugally driven reconfigurations of an aggregate can alter the YORP
torque dramatically, resulting in spin evolution that is, in most cases,
qualitatively different from the rigid-body prediction. A third of objects
simulated follow a simple evolution that can be described as a modified YORP
cycle. Two-thirds exhibit one or more of three distinct behaviors -stochastic
YORP, self-governed YORP, and stagnating YORP-which together result in YORP
self-limitation. Self-limitation confines the rotation rates of evolving
aggregates to far narrower ranges than would be expected in the classical YORP
cycle, and greatly prolonging the times over which objects can preserve their
sense of rotation. The asteroids are initially randomly packed, disordered
aggregates of identical spheres that collectively have a low internal angle of
friction. They are highly deformable and lie near, but not on, the
Maclaurin/Jacobi sequence for fluid spheroids/ellipsoids. Their evolution in
shape is characterized by rearrangement of the entire body, including the deep
interior, not predominantly by movement of surface material. They do not evolve
to axisymmetric top shapes with equatorial ridges. When they lose mass, they
generally do so in small amounts from the ends of a prolate-triaxial body, and
always after crossing the Jacobi ellipsoid sequence. YORP self-limitation may
inhibit the formation of top-shapes, binaries, or both, by restricting the
amount of angular momentum that can be imparted to a deformable body.
Stochastic YORP, in particular, will affect the evolution of collisional
families whose orbits drift apart under the influence of Yarkovsky forces, in
observable ways. | | Source: | arXiv, 1411.1114 | | Services: | Forum | Review | PDF | Favorites | |
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