A long-term stable equilibrium for synchronous binaries including tides and the byorp effect

Details A long-term stable equilibrium for synchronous binaries including tides and the byorp effect A long-term stable equilibrium for synchronous binaries including tides and the byorp effect

Apr 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011dda....42.0102j&link_type=abstract

American Astronomical Society, DDA meeting #42, #1.02; Bulletin of the American Astronomical Society, Vol. 43, 2011

Physics

Geophysics

Scientific paper

We present theoretical evidence for the existence of a long-term stable equilibrium solution for synchronous binary asteroids accounting for mutual body tides, the binary YORP (BYORP) effect and dynamics. Synchronous binary asteroid systems consist of a rapidly spinning primary and a tidally-locked secondary, analogous to the Earth-Moon system. Tidal evolution of these systems leads to growth in the semi-major axis. Evolution from the BYORP effect can lead to both contraction and growth of the semi-major axis. There are two scenarios for joint evolution of a synchronous binary when both effects are considered: expansive and opposing evolution. During joint expansive evolution, both effects grow the semi-major axis. The system will either grow to the Hill sphere and disrupt if tidally dominated, or the mutual orbit will be de-stabilized due to runaway eccentricity growth if BYORP dominated. During joint opposing evolution, tidal and BYORP evolution act to evolve the system to a stable equilibrium. The location of this equilibrium to first order depends on just the tidal parameters, specific tidal dissipation number Q and the tidal Love number k, as well as the BYORP shape coefficient. If the observed population of small (0.1 - 10 km diameter), synchronous binaries are assumed to be in this static configuration, then our analysis shows that a monolithic geophysical model is not satisfactory, whereas the ``rubble pile'' model proposed by Goldreich & Sari (2009) is sufficient to prevent runaway eccentricity growth. The existence of this equilibrium and a secondary shape model built from observations enables direct study of asteroid geophysics through tidal theory. The existence of this equilibrium would be confirmed by a lack of migration in observational tests for the BYORP effect.
Goldreich, P. & R. Sari, ApJ, 691:54-60 (2009)

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