Other
Scientific paper
Sep 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.5608j&link_type=abstract
American Astronomical Society, DPS meeting #41, #56.08
Other
Scientific paper
We derive a realistic model for the evolution of tidally perturbed binary asteroids to examine systems immediately after a spin-up fission event. The spin rate of an asteroid can be increased by the YORP effect--thermal re-radiation from an asymmetric body, which induces torques that can rotationally accelerate a body. If the asteroid is modeled as a "rubble pile", a collection of gravitationally bound boulders with a distribution of size scales and no tensile strength between them, increasing the spin rate leads to an eventual fission of components, determined by the largest separation between the mass centers of the asteroid. We note that these post-fission binaries are always unstable and initially evolve chaotically. We model the shapes of these bodies as tri-axial ellipsoids with a gravitational potential expanded up to second order. Our model applies instantaneous tidal torques to both members of the binary system to determine energy dissipation that could provide enough loss to settle the system into a stable orbit.
We find that most systems experience a period of chaotic evolution with rapid energy dissipation followed by a classical quasi-steady state tidal evolution. The mass ratio of the system plays a dominant role in determining the final state after the chaotic evolution. Systems can be divided into distinct evolutionary tracks that determine the outcome of their chaotic behavior in terms of timescale and total dissipated energy during the rapid phase. Secondary bodies of low mass ratio systems may proceed through their own spin-fission events. Systems with higher mass ratios approach a fully synchronous state after this fast energy dissipation period. After these systems emerge from their chaotic behavior they evolve according to the much slower classical theory, where other non-gravitational effects could play a more significant role. We would like to acknowledge NASA's PG&G Program.
Jacobson Seth A.
Scheeres Daniel J.
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