Steady-state Population Of The Nea Binaries And Yorp Spinup Models

Details Steady-state Population Of The Nea Binaries And Yorp Spinup Models Steady-state Population Of The Nea Binaries And Yorp Spinup Models

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5308w&link_type=abstract

American Astronomical Society, DPS meeting #38, #53.08; Bulletin of the American Astronomical Society, Vol. 38, p.582

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We present results of a steady-state simulation of the near-Earth asteroid (NEA) binary population. This study combines the previous work on tidal disruption of gravitational aggregates [Walsh & Richardson 2006, Icarus 180, 201--206] with a Monte Carlo simulation of NEA planetary encounters. Evolutionary effects such as tidally induced binary circularization and widening, as well as binary disruption caused by close planetary encounters, are included. The results show that using the best known distributions of progenitor (small Main Belt asteroid) shape and spin, and current estimates of NEA lifetimes and encounter probabilities, that tidal disruption accounts for approximately 1-5% of NEAs being binaries. Since the observed population is around 15% binaries, there is potentially one or more other important binary formation mechanisms at work. Our work also suggests that even a large pre-existing Main Belt binary population cannot explain the discrepancy. Finally, we present preliminary results of the slow spinup of gravitational aggregates designed to model the effects of a thermal spinup mechanism (YORP) acting on small asteroids. This work quantifies how body shape and spin changes differ from fluid equilibrium limits (Jacobi ellipsoids) and determines the efficiency of binary formation via YORP. This material is based upon work supported by the National Science Foundation under Grant No. AST0307549.

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