Binary asteroid orbit expansion due to continued YORP spin-up of the primary and primary surface particle motion

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2008.12.021 Byline: Eugene G. Fahnestock (a), Daniel J. Scheeres (b) Keywords: Asteroids; Asteroids; dynamics; Satellites of asteroids; Asteroids; surfaces; Regoliths Abstract: We examine the hypothesis that within close binary asteroid systems with super-synchronously rotating, roughly spheroidal primary (Alpha) and synchronous elongated secondary (Beta), continued YORP angular acceleration of the primary causes it to spin at rates where loose material near its equator is lofted from the surface. Subsequent interaction of the material with the binary components causes that material to lose angular momentum and re-impact Alpha. In this process angular momentum is transferred to the orbit, causing the orbit to expand. We confirm this hypothesis through precise dynamic and approximate statistical simulation. For this we use the well-characterized 1999 KW4 system model, as KW4 typifies the class of binaries of interest. Our results visibly demonstrate the transfer of angular momentum and the hypothesized orbit evolution mechanism. In particular, we observe regulation of Alpha spin rate at the rate for which material lofting begins on the same side of Alpha as Beta, but not yet on the opposite side. We observe nearly constant Alpha angular momentum while the orbit angular momentum grows steadily. The linear fit to that growth is consistent with the YORP torque angular acceleration applied. Lofting occurs in fast transient episodes separated by long periods of slow spin-up under that acceleration. The average amount of material aloft and rate of mass lofting are interesting metrics for the system's lofting activity level contained in our results, but are not physically descriptive at any particular instant, given episodic lofting. We translate the orbit angular momentum growth to average semi-major axis change rate with a simple formula, whose integration also leads to time scales for the system evolution several times faster than standard tidal evolution (such as present orbit size doubling time of 2.5[+ or -]0.7 Myr for KW4). The observationally-supported end state of the system's evolution is likely separation into two asteroids on closely-related heliocentric orbits. Possible shedding of sufficiently more material from the still YORP-torqued primary may form a new secondary and repeat the overall system evolution. Author Affiliation: (a) Department of Aerospace Engineering, University of Michigan, 2008 FXB Building, 1320 Beal Avenue, Ann Arbor, MI 48109, United States (b) Department of Aerospace Engineering Sciences/Colorado Center for Astrodynamics Research, University of Colorado, Engineering Center, ECOT 611, 429 UCB, Boulder, CO 80309, United States Article History: Received 9 April 2008; Revised 13 December 2008; Accepted 15 December 2008